<?xml version="1.0" encoding="UTF-8"?>
<!DOCTYPE article PUBLIC "-//NLM//DTD Journal Publishing DTD v2.3 20070202//EN" "journalpublishing.dtd">
<article article-type="research-article" dtd-version="2.3" xml:lang="EN" xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink">
<front>
<journal-meta>
<journal-id journal-id-type="publisher-id">Front. Astron. Space Sci.</journal-id>
<journal-title>Frontiers in Astronomy and Space Sciences</journal-title>
<abbrev-journal-title abbrev-type="pubmed">Front. Astron. Space Sci.</abbrev-journal-title>
<issn pub-type="epub">2296-987X</issn>
<publisher>
<publisher-name>Frontiers Media S.A.</publisher-name>
</publisher>
</journal-meta>
<article-meta>
<article-id pub-id-type="publisher-id">1071743</article-id>
<article-id pub-id-type="doi">10.3389/fspas.2023.1071743</article-id>
<article-categories>
<subj-group subj-group-type="heading">
<subject>Astronomy and Space Sciences</subject>
<subj-group>
<subject>Original Research</subject>
</subj-group>
</subj-group>
</article-categories>
<title-group>
<article-title>Gravitational orbits in the expanding Universe revisited</article-title>
<alt-title alt-title-type="left-running-head">Vavry&#x10d;uk</alt-title>
<alt-title alt-title-type="right-running-head">
<ext-link ext-link-type="uri" xlink:href="https://doi.org/10.3389/fspas.2023.1071743">10.3389/fspas.2023.1071743</ext-link>
</alt-title>
</title-group>
<contrib-group>
<contrib contrib-type="author" corresp="yes">
<name>
<surname>Vavry&#x10d;uk</surname>
<given-names>V&#xe1;clav</given-names>
</name>
<xref ref-type="corresp" rid="c001">&#x2a;</xref>
<uri xlink:href="https://loop.frontiersin.org/people/1089536/overview"/>
</contrib>
</contrib-group>
<aff>
<institution>Institute of Geophysics, Czech Academy of Sciences</institution>, <addr-line>Prague</addr-line>, <country>Czechia</country>
</aff>
<author-notes>
<fn fn-type="edited-by">
<p>
<bold>Edited by:</bold> <ext-link ext-link-type="uri" xlink:href="https://loop.frontiersin.org/people/430445/overview">Alvaro De La Cruz-Dombriz</ext-link>, University of Cape Town, South Africa</p>
</fn>
<fn fn-type="edited-by">
<p>
<bold>Reviewed by:</bold> <ext-link ext-link-type="uri" xlink:href="https://loop.frontiersin.org/people/159134/overview">Christian Corda</ext-link>, B. M. Birla Science Centre, India</p>
<p>
<ext-link ext-link-type="uri" xlink:href="https://loop.frontiersin.org/people/2100202/overview">Demosthenes Kazanas</ext-link>, Goddard Space Flight Center (NASA), United States</p>
</fn>
<corresp id="c001">&#x2a;Correspondence: V&#xe1;clav Vavry&#x10d;uk, <email>vv@ig.cas.cz</email>
</corresp>
<fn fn-type="other">
<p>This article was submitted to Cosmology, a section of the journal Frontiers in Astronomy and Space Sciences</p>
</fn>
</author-notes>
<pub-date pub-type="epub">
<day>06</day>
<month>02</month>
<year>2023</year>
</pub-date>
<pub-date pub-type="collection">
<year>2023</year>
</pub-date>
<volume>10</volume>
<elocation-id>1071743</elocation-id>
<history>
<date date-type="received">
<day>16</day>
<month>10</month>
<year>2022</year>
</date>
<date date-type="accepted">
<day>11</day>
<month>01</month>
<year>2023</year>
</date>
</history>
<permissions>
<copyright-statement>Copyright &#xa9; 2023 Vavry&#x10d;uk.</copyright-statement>
<copyright-year>2023</copyright-year>
<copyright-holder>Vavry&#x10d;uk</copyright-holder>
<license xlink:href="http://creativecommons.org/licenses/by/4.0/">
<p>This is an open-access article distributed under the terms of the Creative Commons Attribution License (CC BY). The use, distribution or reproduction in other forums is permitted, provided the original author(s) and the copyright owner(s) are credited and that the original publication in this journal is cited, in accordance with accepted academic practice. No use, distribution or reproduction is permitted which does not comply with these terms.</p>
</license>
</permissions>
<abstract>
<p>Modified Newtonian equations for gravitational orbits in the expanding Universe indicate that local gravitationally bounded systems like galaxies and planetary systems are unaffected by the expansion of the Universe. This result is derived for the space expansion described by the standard FLRW metric. In this paper, the modified Newtonian equations are derived for the space expansion described by the conformal cosmology (CC) metric. In this metric, the comoving and proper times are different similarly as the comoving and proper distances. As shown by Vavry&#x10d;uk (Front. Phys. 2022), this metric is advantageous, because it properly predicts the cosmic time dilation, and fits the Type Ia supernova luminosity observations with no need to introduce dark energy. Surprisingly, the solution of the equations for gravitational orbits based on the CC metric behaves quite differently than that based on the FLRW metric. In contrast to the common opinion that local systems resist the space expansion, they expand according to the Hubble flow in the CC metric. The evolution of the local systems with cosmic time is exemplified on numerical modelling of spiral galaxies. The size of the spiral galaxies grows consistently with observations and a typical spiral pattern is well reproduced. The theory predicts flat rotation curves without an assumption of dark matter surrounding the galaxy. The theory resolves challenges to the &#x39b;CDM model such as the problem of faint satellite galaxies, baryonic Tully-Fisher relation or the radial acceleration relation. Furthermore, puzzles in the solar system are successfully explained such as the Faint young Sun paradox or the Moon&#x2019;s and Titan&#x2019;s orbit anomalies.</p>
</abstract>
<kwd-group>
<kwd>cosmological redshift</kwd>
<kwd>cosmic time dilation</kwd>
<kwd>conformal metric</kwd>
<kwd>dark energy</kwd>
<kwd>rotation curves</kwd>
<kwd>dark matter</kwd>
<kwd>winding problem</kwd>
<kwd>galaxy expansion</kwd>
</kwd-group>
</article-meta>
</front>
<body>
<sec id="s1">
<title>1 Introduction</title>
<p>Observations of the cosmological redshift interpreted by <xref ref-type="bibr" rid="B95">Lema&#xee;tre (1927)</xref> and <xref ref-type="bibr" rid="B67">Hubble (1929)</xref> as an effect of the expansion of the Universe started a new era of cosmology and opened space for applying theory of General Relativity (GR) to cosmological problems. Subsequently, the Friedmann equations&#xa0;(<xref ref-type="bibr" rid="B58">Friedmann, 1922</xref>) became the basic equations describing the expanding history of the Universe. Immediately, cosmology was faced with the following fundamental questions: How does the global expansion of the Universe affect local gravitational systems? How do local gravitational fields interact with the expansion and where is a size threshold between systems affected by and resisting the global expansion? Do galaxies and galaxy clusters expand or not? How does the global expansion affect our solar system? These theoretical problems paid attention of many cosmologists, because they have essential consequences for understanding the evolution of the Universe and for interpreting cosmological observations (<xref ref-type="bibr" rid="B115">McVittie, 1933</xref>; <xref ref-type="bibr" rid="B49">Einstein and Straus, 1945</xref>; <xref ref-type="bibr" rid="B40">Dicke and Peebles, 1964</xref>; <xref ref-type="bibr" rid="B129">Noerdlinger and Petrosian, 1971</xref>; <xref ref-type="bibr" rid="B27">Carrera and Giulini, 2010</xref>; <xref ref-type="bibr" rid="B125">Nandra&#xa0;et&#xa0;al., 2012</xref>).</p>
<p>The simplest problem is to study the Newtonian equations of motion for two-point particles placed in the expanding space and mutually attracted by the gravitational force. If the local gravitational field is weak and velocities of particles are non-relativistic, the problem can be solved by perturbations (<xref ref-type="bibr" rid="B115">McVittie, 1933</xref>; <xref ref-type="bibr" rid="B129">Noerdlinger and Petrosian, 1971</xref>; <xref ref-type="bibr" rid="B16">Bolen&#xa0;et&#xa0;al., 2001</xref>; <xref ref-type="bibr" rid="B54">Faraoni and Jacques, 2007</xref>). In this case, we assume that the metric of the space expansion is perturbed by a weak gravitational field. Assuming that the space expansion is described by the Friedmann-Lemaitre-Robertson-Walker (FLRW) metric, the metric tensor <italic>g</italic>
<sub>
<italic>&#x3bc;&#x3bd;</italic>
</sub> of a gravitational field produced by a point mass <italic>M</italic> situated in the expanding space reads (<xref ref-type="bibr" rid="B129">Noerdlinger and Petrosian, 1971</xref>, their Eq. 11).<disp-formula id="e1">
<mml:math id="m1">
<mml:mtable class="aligned">
<mml:mtr>
<mml:mtd columnalign="right">
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>s</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mtd>
<mml:mtd columnalign="left">
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2b;</mml:mo>
<mml:mn>2</mml:mn>
<mml:mi>&#x3b1;</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>t</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:mn>2</mml:mn>
<mml:mi>&#x3b1;</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>k</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
<mml:mo>,</mml:mo>
</mml:mtd>
</mml:mtr>
<mml:mtr>
<mml:mtd columnalign="right">
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mtd>
<mml:mtd columnalign="left">
<mml:mo>&#x3d;</mml:mo>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>&#x3b8;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi mathvariant="normal">sin</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2061;</mml:mo>
<mml:mi>&#x3b8;</mml:mi>
<mml:mspace width="0.17em"/>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>,</mml:mo>
</mml:mtd>
</mml:mtr>
</mml:mtable>
</mml:math>
<label>(1)</label>
</disp-formula>where <italic>t</italic> is time, <italic>c</italic> is the speed of light, <italic>a</italic>(<italic>t</italic>) is the scale factor, <italic>k</italic> is the Gaussian curvature of the space, <italic>r</italic> is the comoving distance, and <italic>&#x3b8;</italic> and <italic>&#x3d5;</italic> are the spherical angles. Parameter<disp-formula id="e2">
<mml:math id="m2">
<mml:mi>&#x3b1;</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>G</mml:mi>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>r</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>,</mml:mo>
<mml:mspace width="0.17em"/>
<mml:mo stretchy="false">&#x7c;</mml:mo>
<mml:mi>&#x3b1;</mml:mi>
<mml:mo stretchy="false">&#x7c;</mml:mo>
<mml:mo>&#x226a;</mml:mo>
<mml:mn>1</mml:mn>
<mml:mo>,</mml:mo>
</mml:math>
<label>(2)</label>
</disp-formula>is the Newtonian gravitational potential normalized to <italic>c</italic>
<sup>2</sup>, and <italic>G</italic> is the gravitational constant. Assuming a massive non-relativistic particle (<italic>v</italic> &#x226a; <italic>c</italic>) orbiting in the gravitational field and using the geodesic equation, we finally obtain the following equation for the proper radius <italic>R</italic> of the orbit (<xref ref-type="bibr" rid="B27">Carrera and Giulini, 2010</xref>, their Eq. 12a, b).<disp-formula id="e3">
<mml:math id="m3">
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>G</mml:mi>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>L</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>3</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>R</mml:mi>
<mml:mo>,</mml:mo>
</mml:math>
<label>(3)</label>
</disp-formula>
<disp-formula id="e4">
<mml:math id="m4">
<mml:mi>L</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mi mathvariant="normal">c</mml:mi>
<mml:mi mathvariant="normal">o</mml:mi>
<mml:mi mathvariant="normal">n</mml:mi>
<mml:mi mathvariant="normal">s</mml:mi>
<mml:mi mathvariant="normal">t</mml:mi>
<mml:mo>,</mml:mo>
</mml:math>
<label>(4)</label>
</disp-formula>where <italic>L</italic> &#x3d; <italic>RV</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> is the proper angular momentum, and <italic>V</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> is the proper tangential velocity. For a more detailed derivation, see <xref ref-type="app" rid="app1">Appendix&#xa0;A</xref>.</p>
<p>Eqs.&#xa0;<xref ref-type="disp-formula" rid="e3">3</xref>, <xref ref-type="disp-formula" rid="e4">4</xref> are called the modified (or improved) Newtonian equations and they differ from the standard Newtonian equations describing the Kepler orbits by term <inline-formula id="inf1">
<mml:math id="m5">
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>R</mml:mi>
</mml:math>
</inline-formula> in Eq.&#xa0;<xref ref-type="disp-formula" rid="e3">3</xref> related to the space expansion. The analysis of the modified Newtonian equations applied to the galaxy dynamics shows that the expansion term <inline-formula id="inf2">
<mml:math id="m6">
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>R</mml:mi>
</mml:math>
</inline-formula> affects the orbits within galaxies negligibly (<xref ref-type="bibr" rid="B54">Faraoni and Jacques, 2007</xref>). This result led to the conclusion that galaxies and all smaller gravitational systems are not affected by the space expansion and behave as in the static Universe (<xref ref-type="bibr" rid="B40">Dicke and Peebles, 1964</xref>; <xref ref-type="bibr" rid="B129">Noerdlinger and Petrosian, 1971</xref>; <xref ref-type="bibr" rid="B29">Cooperstock&#xa0;et&#xa0;al., 1998</xref>; <xref ref-type="bibr" rid="B54">Faraoni and Jacques, 2007</xref>; <xref ref-type="bibr" rid="B72">Iorio, 2013</xref>).</p>
<p>The key in deriving the modified Newtonian equations is the assumption that the space expansion is described by the FLRW metric. However, this metric is not the only metric, which can describe the evolution of the isotropic homogeneous Universe. A potentially applicable metric is also the conformal cosmology (CC) metric (<xref ref-type="bibr" rid="B52">Endean, 1994</xref>; <xref ref-type="bibr" rid="B51">Endean, 1997</xref>; <xref ref-type="bibr" rid="B68">Ibison, 2007</xref>; <xref ref-type="bibr" rid="B74">Kastrup, 2008</xref>; <xref ref-type="bibr" rid="B32">Dabrowski&#xa0;et&#xa0;al., 2009</xref>; <xref ref-type="bibr" rid="B64">Gr&#xf8;n and Johannesen, 2011</xref>; <xref ref-type="bibr" rid="B177">Visser, 2015</xref>; <xref ref-type="bibr" rid="B65">Harada&#xa0;et&#xa0;al., 2018</xref>). This metric has the scale factor <italic>a</italic>(<italic>t</italic>) not only at the space components but also at the time component of the metric tensor <italic>g</italic>
<sub>
<italic>&#x3bc;&#x3bd;</italic>
</sub>. Hence, the metric is characterized not only by the space expansion but also by the time dilation during the cosmic evolution. The CC metric has exceptional properties being intensively studied in GR and its modifications such as the Conformal Gravity theory (<xref ref-type="bibr" rid="B104">Mannheim, 1990</xref>; <xref ref-type="bibr" rid="B103">Mannheim, 2006</xref>; <xref ref-type="bibr" rid="B106">Mannheim, 2012</xref>). Interestingly, the CC metric is Lorentz invariant and leaves the Maxwell&#x2019;s equations unchanged from their form in the Minkowski spacetime (<xref ref-type="bibr" rid="B69">Infeld and Schild, 1945</xref>; <xref ref-type="bibr" rid="B70">Infeld and Schild, 1946</xref>; <xref ref-type="bibr" rid="B68">Ibison, 2007</xref>).</p>
<p>Importantly, <xref ref-type="bibr" rid="B175">Vavry&#x10d;uk (2022a)</xref> shows that the CC metric should be preferable against the FLRW metric, because the FLRW metric is actually inconsistent with observations of the cosmological redshift and cosmic time dilation. He claims that the CC metric is necessary for a proper description of the expansion of the Universe, because: 1) The time-time component of the metric tensor <italic>g</italic>
<sub>00</sub> must vary with cosmic time similarly as the space-space components, and 2) the comoving and proper times must be different in analogy to the comoving and proper distances. Consequently, time should not be invariant as in the FLRW metric, but its rate must vary during the evolution of the Universe. Without changing the time rate, the frequency of photons propagating in the Universe cannot be changed during the expansion and the photons cannot be redshifted.</p>
<p>The varying time rate during the evolution of the Universe is also supported by observations of Type Ia supernovae (SNe Ia). Since the SNe Ia display rather uniform light curves, they can serve as the standard candles as well as the standard local clocks. The spectral evolution of the light curves and stretching of time in the observer frame was disclosed by many authors (<xref ref-type="bibr" rid="B91">Leibundgut&#xa0;et&#xa0;al., 1996</xref>; <xref ref-type="bibr" rid="B60">Goldhaber&#xa0;et&#xa0;al., 1997</xref>; <xref ref-type="bibr" rid="B138">Phillips&#xa0;et&#xa0;al., 1999</xref>; <xref ref-type="bibr" rid="B61">Goldhaber&#xa0;et&#xa0;al., 2001</xref>). The stretching of light curves at high redshift is firmly acknowledged and corrections for time dilation are now routinely applied to the SNe Ia data (<xref ref-type="bibr" rid="B90">Leibundgut, 2001</xref>; <xref ref-type="bibr" rid="B62">Goobar and Leibundgut, 2011</xref>). The light curve stretching is commonly interpreted as the effect of the cosmic time dilation even though the standard FLRW metric does not allow it.</p>
<p>In addition, the CC model fits the SNe Ia luminosity observations with no need to introduce dark energy and an accelerated expansion of the Universe (<xref ref-type="bibr" rid="B8">Behnke&#xa0;et&#xa0;al., 2002</xref>; <xref ref-type="bibr" rid="B175">Vavry&#x10d;uk, 2022a</xref>). A possibility that the varying time rate might solve the dark energy problem is reported also by <xref ref-type="bibr" rid="B177">Visser (2015)</xref>. Considering the varying time rate during the cosmic evolution has also other important consequences. For example, the cosmological and gravitational redshifts are calculated from the metric tensor by the same formula. This emphasizes a common physical origin of both redshifts. The gravitational redshift reflects the time distortion due to the presence of the local gravitational field, while the cosmological redshift is due to changes of the global gravitational field of the Universe.</p>
<p>Obviously, we can ask a question, whether does a local gravitational field in the CC metric behave differently from that in the FLRW metric or not. Hence, the aim of this paper is to study local gravitational systems in the expanding space described by the CC metric. The gravitational field is assumed to be a perturbation of the global gravitational field of the Universe and velocities of particles are non-relativistic. The improved Newtonian equations are derived using the geodesic equation. It is shown that the local gravitational systems behave quite differently in the CC metric than in the FLRW metric. In contrast to the common opinion that local systems resist the space expansion, the results show that all local systems expand according to the Hubble flow in the CC metric. The evolution of the local systems is exemplified on numerical modelling of spiral galaxies. The presented theory predicts flat rotation curves and the observed morphology of spirals. Also, other observations supporting the presented theory are discussed.</p>
</sec>
<sec id="s2">
<title>2 Theory</title>
<sec id="s2-1">
<title>2.1 Expanding Universe described by the CC metric</title>
<p>Let us assume an expanding Universe described by the CC metric in the following form (<xref ref-type="bibr" rid="B64">Gr&#xf8;n and Johannesen, 2011</xref>; <xref ref-type="bibr" rid="B175">Vavry&#x10d;uk, 2022a</xref>):<disp-formula id="e5">
<mml:math id="m7">
<mml:mtable class="aligned">
<mml:mtr>
<mml:mtd columnalign="right">
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>s</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mtd>
<mml:mtd columnalign="left">
<mml:mo>&#x3d;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>t</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>k</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
<mml:mo>,</mml:mo>
</mml:mtd>
</mml:mtr>
<mml:mtr>
<mml:mtd columnalign="right">
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mtd>
<mml:mtd columnalign="left">
<mml:mo>&#x3d;</mml:mo>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>&#x3b8;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi mathvariant="normal">sin</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2061;</mml:mo>
<mml:mi>&#x3b8;</mml:mi>
<mml:mspace width="0.17em"/>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>,</mml:mo>
</mml:mtd>
</mml:mtr>
</mml:mtable>
</mml:math>
<label>(5)</label>
</disp-formula>where <italic>a</italic>(<italic>t</italic>) is the scale factor defining the cosmic expansion, <italic>t</italic> is the comoving (contravariant) time, <italic>c</italic> is the speed of light, <italic>k</italic> is the Gaussian curvature of the space, <italic>r</italic> is the comoving (contravariant) distance, and <italic>&#x3b8;</italic> and <italic>&#x3d5;</italic> are the spherical angles.</p>
<p>To avoid confusions, we have to discuss the CC metric described by Eq.&#xa0;<xref ref-type="disp-formula" rid="e5">5</xref> in more detail. This form of the metric is often used in cosmology but in a modified notation and in a different physical context. Time <italic>t</italic> is called the &#x201c;conformal time&#x201d; and it is usually denoted as <italic>&#x3b7;</italic>. However, the physical meanings of the comoving time <italic>t</italic> and the conformal time <italic>&#x3b7;</italic> are essentially different. Here, we consider time <italic>t</italic> in Eq.&#xa0;<xref ref-type="disp-formula" rid="e5">5</xref> as the physical comoving cosmic time. Consequently, the time-time component of the metric tensor <italic>g</italic>
<sub>00</sub> is time dependent. The rate of time varies and Eq.&#xa0;<xref ref-type="disp-formula" rid="e5">5</xref> encompasses the space expansion as well as the time dilation during the evolution of the Universe. By contrast, the conformal time <italic>&#x3b7;</italic> is commonly assumed to be a rescaled proper time with no physical meaning and no effects on the metric. The <italic>g</italic>
<sub>00</sub> component is still time independent as for the FLRW metric. In this way, the metric with the conformal time <italic>&#x3b7;</italic> describes the space expansion with a uniform rate of time and no time dilation during the evolution of the Universe.</p>
<p>When introducing the FLRW metric, it is often argued that <italic>g</italic>
<sub>00</sub> can be assumed to be time invariant, because we have a freedom to rescale time to keep <italic>g</italic>
<sub>00</sub> constant (<xref ref-type="bibr" rid="B179">Weinberg, 1972</xref>). From this point of view, the FLRW and CC metrics would be equivalent (<xref ref-type="bibr" rid="B177">Visser, 2015</xref>). However, this is not correct, because we cannot rescale arbitrarily a cosmological coordinate system without physical consequences. A trivial example is a relation between the space metrics for a static and expanding Universe. Both metrics can be transformed each into the other. However, this does not mean that the model of the static and expanding Universe are physically equivalent. Similarly, the CC metric and the FLRW metric are not physically equivalent, because the FLRW metric is characterized by a uniform rate of time, but the CC metric is characterized by a varying rate of time during the evolution of the Universe.</p>
</sec>
<sec id="s2-2">
<title>2.2 Comoving and proper speeds in the CC metric</title>
<p>Using Eq.&#xa0;<xref ref-type="disp-formula" rid="e5">5</xref>, the equation of the null geodesics, which describes propagation of photons, <italic>ds</italic>
<sup>2</sup> &#x3d; 0, reads<disp-formula id="e6">
<mml:math id="m8">
<mml:mtable class="gathered">
<mml:mtr>
<mml:mtd>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>t</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>l</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>0</mml:mn>
<mml:mo>,</mml:mo>
</mml:mtd>
</mml:mtr>
<mml:mtr>
<mml:mtd>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>l</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>k</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>.</mml:mo>
</mml:mtd>
</mml:mtr>
</mml:mtable>
</mml:math>
<label>(6)</label>
</disp-formula>
</p>
<p>Consequently, we get for the comoving velocity <italic>v</italic> and the proper velocity <italic>V</italic> of photons (<xref ref-type="bibr" rid="B175">Vavry&#x10d;uk, 2022a</xref>, his Eq. A6)<disp-formula id="e7">
<mml:math id="m9">
<mml:mi>v</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>l</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x3d;</mml:mo>
<mml:mi>c</mml:mi>
<mml:mo>,</mml:mo>
<mml:mspace width="0.17em"/>
<mml:mspace width="0.17em"/>
<mml:mi>V</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mi>a</mml:mi>
<mml:mi>c</mml:mi>
<mml:mo>.</mml:mo>
</mml:math>
<label>(7)</label>
</disp-formula>The propagation velocity of massive particles is described by the geodesic equation<disp-formula id="e8">
<mml:math id="m10">
<mml:mfrac>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>d</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:msup>
<mml:mrow>
<mml:mi>x</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3bc;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>s</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:msubsup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x393;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b1;</mml:mi>
<mml:mi>&#x3b2;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3bc;</mml:mi>
</mml:mrow>
</mml:msubsup>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>x</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b1;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>s</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>x</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b2;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>s</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>0</mml:mn>
<mml:mo>.</mml:mo>
</mml:math>
<label>(8)</label>
</disp-formula>Substituting the distance element <italic>ds</italic> by the time element <italic>dt</italic>, we obtain<disp-formula id="e9">
<mml:math id="m11">
<mml:mfrac>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>d</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:msup>
<mml:mrow>
<mml:mi>x</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3bc;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>t</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:msubsup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x393;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b1;</mml:mi>
<mml:mi>&#x3b2;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3bc;</mml:mi>
</mml:mrow>
</mml:msubsup>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>x</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b1;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>x</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b2;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:msubsup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x393;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b1;</mml:mi>
<mml:mi>&#x3b2;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msubsup>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>x</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b1;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>x</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b2;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>x</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3bc;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mo>.</mml:mo>
</mml:math>
<label>(9)</label>
</disp-formula>Considering the metric tensor <italic>g</italic>
<sub>
<italic>&#x3bc;&#x3bd;</italic>
</sub> needed for calculating the Christoffel symbols <inline-formula id="inf3">
<mml:math id="m12">
<mml:msubsup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x393;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b1;</mml:mi>
<mml:mi>&#x3b2;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3bc;</mml:mi>
</mml:mrow>
</mml:msubsup>
</mml:math>
</inline-formula> in Eq.&#xa0;<xref ref-type="disp-formula" rid="e9">9</xref> defined by Eq.&#xa0;<xref ref-type="disp-formula" rid="e5">5</xref>, we get<disp-formula id="e10">
<mml:math id="m13">
<mml:mi>a</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x2b;</mml:mo>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>v</mml:mi>
<mml:mo>&#x2212;</mml:mo>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>3</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>0</mml:mn>
<mml:mo>,</mml:mo>
</mml:math>
<label>(10)</label>
</disp-formula>hence<disp-formula id="e11">
<mml:math id="m14">
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>v</mml:mi>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>/</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mo>.</mml:mo>
</mml:math>
<label>(11)</label>
</disp-formula>Consequently, for a massive non-relativistic particle (<italic>v</italic> &#x226a; <italic>c</italic>) we write<disp-formula id="e12">
<mml:math id="m15">
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
</mml:math>
<label>(12)</label>
</disp-formula>and the comoving velocity <italic>v</italic> and the proper velocity <italic>V</italic> read<disp-formula id="e13">
<mml:math id="m16">
<mml:mi>v</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msub>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mn>1</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>,</mml:mo>
<mml:mspace width="0.17em"/>
<mml:mspace width="0.17em"/>
<mml:mi>V</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mi>a</mml:mi>
<mml:mi>v</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi>V</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msub>
<mml:mo>,</mml:mo>
</mml:math>
<label>(13)</label>
</disp-formula>where subscript &#x201c;0&#x201d; refers to quantities at present.</p>
<p>Hence, the proper velocity of photons is not constant as in the FLRW metric, but it increases in the CC metric with the expansion as <italic>a</italic>(<italic>t</italic>)<italic>c</italic>, where <italic>c</italic> is the speed of light for <italic>a</italic> &#x3d; 1. By contrast, the proper velocity of massive non-relativistic particles is not affected by the Universe expansion. This is in contradiction with behaviour of non-relativistic massive particles in the FLRW metric, where the comoving velocity <italic>v</italic> depends on <italic>a</italic> as <italic>a</italic>
<sup>&#x2212;2</sup> and the proper velocity <italic>V</italic> as <italic>a</italic>
<sup>&#x2212;1</sup>.</p>
<p>Note that the varying speed of light in Eq.&#xa0;<xref ref-type="disp-formula" rid="e7">7</xref> for the CC metric is an inevitable consequence of the time dependence of <italic>g</italic>
<sub>00</sub>. The varying speed of light seems apparently against the basic principles of theory of the Special and General Relativity, but according to <xref ref-type="bibr" rid="B48">Einstein (1920)</xref>: &#x201c;The law of the constancy of the velocity of light <italic>in vacuo</italic>, which constitutes one of the fundamental assumptions in the special theory of relativity and to which we have already frequently referred, cannot claim any unlimited validity&#x201d;...&#x201c;its results hold only so long as we are able to disregards the influences of gravitational fields on the phenomena (e.g., of light)&#x201d;. Since we do not study the speed of light in free-falling inertial systems but in non-inertial systems, the acceleration due to gravity is not cancelled with the gravitational field. Hence, the varying (coordinate-dependent) speed of light in the CC metric is fully consistent with GR being analogous, for example, to the varying (coordinate-dependent) speed of light known in the famous Schwarzschild solution (<xref ref-type="bibr" rid="B179">Weinberg, 1972</xref>).</p>
</sec>
<sec id="s2-3">
<title>2.3 Conformal Friedmann equations</title>
<p>Assuming the FLRW metric described by Eq.&#xa0;<xref ref-type="disp-formula" rid="eA_1">A-1</xref>, the Friedmann equation for the perfect isotropic fluid reads (<xref ref-type="bibr" rid="B136">Peacock, 1999</xref>; <xref ref-type="bibr" rid="B147">Ryden, 2016</xref>)<disp-formula id="e14">
<mml:math id="m17">
<mml:msup>
<mml:mrow>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mfrac>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mo>&#x2032;</mml:mo>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mn>8</mml:mn>
<mml:mi>&#x3c0;</mml:mi>
<mml:mi>G</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>3</mml:mn>
</mml:mrow>
</mml:mfrac>
<mml:mi>&#x3c1;</mml:mi>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>k</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>,</mml:mo>
</mml:math>
<label>(14)</label>
</disp-formula>where <italic>a</italic>&#x2032; &#x3d; <italic>da</italic>/<italic>dT</italic> is the derivative of the scale factor <italic>a</italic>(<italic>t</italic>) with respect to the proper time <italic>T</italic>, <italic>G</italic> is the gravitational constant, <italic>&#x3c1;</italic> is the mean mass density, and <italic>k</italic> is the spatial curvature of the Universe at present.</p>
<p>In order to express Eq.&#xa0;<xref ref-type="disp-formula" rid="e14">14</xref> in the CC metric, we have to substitute the proper time <italic>T</italic> by the comoving time <italic>t</italic> and time derivative <italic>a</italic>&#x2032; &#x3d; <italic>da</italic>/<italic>dT</italic> by <inline-formula id="inf4">
<mml:math id="m18">
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x3d;</mml:mo>
<mml:mi>d</mml:mi>
<mml:mi>a</mml:mi>
<mml:mo>/</mml:mo>
<mml:mi>d</mml:mi>
<mml:mi>t</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mi>a</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mo>&#x2032;</mml:mo>
</mml:mrow>
</mml:msup>
</mml:math>
</inline-formula>. Hence, the conformal Friedmann equation reads<disp-formula id="e15">
<mml:math id="m19">
<mml:msup>
<mml:mrow>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mn>8</mml:mn>
<mml:mi>&#x3c0;</mml:mi>
<mml:mi>G</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>3</mml:mn>
</mml:mrow>
</mml:mfrac>
<mml:mi>&#x3c1;</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>k</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>,</mml:mo>
</mml:math>
<label>(15)</label>
</disp-formula>where <inline-formula id="inf5">
<mml:math id="m20">
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
</mml:math>
</inline-formula> denotes the derivative with respect to the comoving time <italic>t</italic>. Considering the matter-dominated Universe, we get<disp-formula id="e16">
<mml:math id="m21">
<mml:mfrac>
<mml:mrow>
<mml:mn>8</mml:mn>
<mml:mi>&#x3c0;</mml:mi>
<mml:mi>G</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>3</mml:mn>
</mml:mrow>
</mml:mfrac>
<mml:mi>&#x3c1;</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:msubsup>
<mml:mrow>
<mml:mi>H</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msubsup>
<mml:mspace width="0.17em"/>
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>m</mml:mi>
</mml:mrow>
</mml:msub>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mn>3</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>.</mml:mo>
</mml:math>
<label>(16)</label>
</disp-formula>Eq.&#xa0;<xref ref-type="disp-formula" rid="e15">15</xref> is rewritten as (<xref ref-type="bibr" rid="B175">Vavry&#x10d;uk, 2022a</xref>)<disp-formula id="e17">
<mml:math id="m22">
<mml:msup>
<mml:mrow>
<mml:mi>H</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:msubsup>
<mml:mrow>
<mml:mi>H</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msubsup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>m</mml:mi>
</mml:mrow>
</mml:msub>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mn>1</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>k</mml:mi>
</mml:mrow>
</mml:msub>
</mml:mrow>
</mml:mfenced>
</mml:math>
<label>(17)</label>
</disp-formula>with the condition<disp-formula id="e18">
<mml:math id="m23">
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>m</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mo>&#x2b;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>k</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>1</mml:mn>
<mml:mo>,</mml:mo>
</mml:math>
<label>(18)</label>
</disp-formula>where <inline-formula id="inf6">
<mml:math id="m24">
<mml:mi>H</mml:mi>
<mml:mrow>
<mml:mo stretchy="false">(</mml:mo>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo stretchy="false">)</mml:mo>
</mml:mrow>
<mml:mo>&#x3d;</mml:mo>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>/</mml:mo>
<mml:mi>a</mml:mi>
</mml:math>
</inline-formula> is the Hubble parameter, <italic>H</italic>
<sub>0</sub> is the Hubble constant, &#x3a9;<sub>
<italic>m</italic>
</sub> is the normalized matter density, and &#x3a9;<sub>
<italic>k</italic>
</sub> is the normalized space curvature. As shown in <xref ref-type="bibr" rid="B175">Vavry&#x10d;uk (2022a)</xref>, Eq.&#xa0;<xref ref-type="disp-formula" rid="e17">17</xref> describes the Type Ia supernova (SNe Ia) dimming well with no need to introduce dark energy, which is necessary in the standard &#x39b;CDM model in order to fit the SNe Ia data.</p>
<p>Considering <italic>a</italic> &#x3d; 1/(1 &#x2b; <italic>z</italic>), the comoving time <italic>t</italic> is expressed from Eq.&#xa0;<xref ref-type="disp-formula" rid="e17">17</xref> as a function of redshift as follows<disp-formula id="e19">
<mml:math id="m25">
<mml:mi>d</mml:mi>
<mml:mi>t</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mn>1</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:msub>
<mml:mrow>
<mml:mi>H</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msub>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2b;</mml:mo>
<mml:mi>z</mml:mi>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
</mml:mfrac>
<mml:msup>
<mml:mrow>
<mml:mfenced open="[" close="]">
<mml:mrow>
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>m</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2b;</mml:mo>
<mml:mi>z</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x2b;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>k</mml:mi>
</mml:mrow>
</mml:msub>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
<mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mn>1</mml:mn>
<mml:mo>/</mml:mo>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>d</mml:mi>
<mml:mi>z</mml:mi>
<mml:mo>,</mml:mo>
</mml:math>
<label>(19)</label>
</disp-formula>and the proper time <italic>T</italic> related to comoving <italic>t</italic> as <italic>dT</italic> &#x3d; <italic>a</italic>(<italic>t</italic>) <italic>dt</italic> reads<disp-formula id="e20">
<mml:math id="m26">
<mml:mi>d</mml:mi>
<mml:mi>T</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mn>1</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:msub>
<mml:mrow>
<mml:mi>H</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msub>
<mml:msup>
<mml:mrow>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2b;</mml:mo>
<mml:mi>z</mml:mi>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:msup>
<mml:mrow>
<mml:mfenced open="[" close="]">
<mml:mrow>
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>m</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2b;</mml:mo>
<mml:mi>z</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x2b;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>k</mml:mi>
</mml:mrow>
</mml:msub>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
<mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mn>1</mml:mn>
<mml:mo>/</mml:mo>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>d</mml:mi>
<mml:mi>z</mml:mi>
<mml:mo>.</mml:mo>
</mml:math>
<label>(20)</label>
</disp-formula>These relations are needed for relating observations of redshift to cosmic time.</p>
</sec>
<sec id="s2-4">
<title>2.4 Gravitational orbits in the expanding Universe</title>
<p>Next, we study the influence of the expanding Universe on the local gravity field produced by a point mass. The gravity field is assumed to produce a small perturbation of the metric tensor <italic>g</italic>
<sub>
<italic>&#x3bc;&#x3bd;</italic>
</sub> describing the expanding space. So far, this problem has been studied under the assumption that the space expansion is defined by the standard FLRW metric (<xref ref-type="bibr" rid="B27">Carrera and Giulini, 2010</xref>), see <xref ref-type="app" rid="app1">Appendix&#xa0;A</xref>. Here, we derive equations for the gravitational orbits for the space expansion defined by the CC metric.</p>
<p>The homogeneous and isotropic expanding space characterized by the CC metric will be disturbed by a spherically symmetric gravitational field produced by a point mass <italic>M</italic> situated in the origin of coordinates. Since we limit ourselves to the weak gravitational effects of the point mass only, Eq.&#xa0;<xref ref-type="disp-formula" rid="e5">5</xref> is modified as follows<disp-formula id="e21">
<mml:math id="m27">
<mml:mtable class="aligned">
<mml:mtr>
<mml:mtd columnalign="right">
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>s</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mfenced open="[" close="]">
<mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2b;</mml:mo>
<mml:mn>2</mml:mn>
<mml:mi>&#x3b1;</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>t</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:mn>2</mml:mn>
<mml:mi>&#x3b1;</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>k</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
<mml:mo>,</mml:mo>
</mml:mtd>
</mml:mtr>
</mml:mtable>
</mml:math>
<label>(21)</label>
</disp-formula>where<disp-formula id="e22">
<mml:math id="m28">
<mml:mi>&#x3b1;</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>G</mml:mi>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>r</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>,</mml:mo>
<mml:mspace width="0.17em"/>
<mml:mo stretchy="false">&#x7c;</mml:mo>
<mml:mi>&#x3b1;</mml:mi>
<mml:mo stretchy="false">&#x7c;</mml:mo>
<mml:mo>&#x226a;</mml:mo>
<mml:mn>1</mml:mn>
</mml:math>
<label>(22)</label>
</disp-formula>is the Newtonian gravitational potential normalized to <italic>c</italic>
<sup>2</sup>, <italic>r</italic> is the comoving distance of an orbiting particle from the point mass <italic>M</italic>, and <italic>G</italic> is the gravitational constant.</p>
<p>Let us assume a massive non-relativistic particle (<italic>v</italic> &#x226a; <italic>c</italic>) orbiting in the gravitational field in the plane defined by <italic>&#x3b8;</italic> &#x3d; 0. The metric tensor <italic>g</italic>
<sub>
<italic>&#x3bc;&#x3bd;</italic>
</sub> is defined by Eq.&#xa0;<xref ref-type="disp-formula" rid="e21">21</xref>. Calculating the Christoffel symbols <inline-formula id="inf7">
<mml:math id="m29">
<mml:msubsup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x393;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b1;</mml:mi>
<mml:mi>&#x3b2;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3bc;</mml:mi>
</mml:mrow>
</mml:msubsup>
</mml:math>
</inline-formula> in Eq.&#xa0;<xref ref-type="disp-formula" rid="e9">9</xref>, we get<disp-formula id="e23">
<mml:math id="m30">
<mml:mtable class="gathered">
<mml:mtr>
<mml:mtd>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>r</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>&#x3b1;</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>&#x3b1;</mml:mi>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>2</mml:mn>
<mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>r</mml:mi>
<mml:mo>&#x2212;</mml:mo>
<mml:mn>3</mml:mn>
<mml:mfrac>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
</mml:mfrac>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mn>1</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>0</mml:mn>
<mml:mo>,</mml:mo>
</mml:mtd>
</mml:mtr>
</mml:mtable>
</mml:math>
<label>(23)</label>
</disp-formula>
<disp-formula id="e24">
<mml:math id="m31">
<mml:mtable class="gathered">
<mml:mtr>
<mml:mtd>
<mml:mi>r</mml:mi>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x2b;</mml:mo>
<mml:mn>2</mml:mn>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x2b;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>r</mml:mi>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x2b;</mml:mo>
<mml:mn>2</mml:mn>
<mml:mi>&#x3b1;</mml:mi>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mn>1</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>0</mml:mn>
<mml:mo>,</mml:mo>
</mml:mtd>
</mml:mtr>
</mml:mtable>
</mml:math>
<label>(24)</label>
</disp-formula>where dots over quantities mean derivatives with respect to the comoving time <italic>t</italic>. Since &#x7c;<italic>&#x3b1;</italic>&#x7c;&#x226a; 1 and <italic>c</italic>
<sup>2</sup> &#x226b; 1, terms multiplied by <italic>&#x3b1;</italic> or by 1/<italic>c</italic>
<sup>2</sup> in Eqs.&#xa0;<xref ref-type="disp-formula" rid="e23">23</xref>, <xref ref-type="disp-formula" rid="e24">24</xref> can be neglected and we get the following approximate equations<disp-formula id="e25">
<mml:math id="m32">
<mml:mfrac>
<mml:mrow>
<mml:mn>1</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>a</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>G</mml:mi>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x3d;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi>f</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>g</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mo>&#x2b;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi>f</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mo>,</mml:mo>
</mml:math>
<label>(25)</label>
</disp-formula>
<disp-formula id="e26">
<mml:math id="m33">
<mml:mfrac>
<mml:mrow>
<mml:mn>1</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>t</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>a</mml:mi>
<mml:mi>r</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>0</mml:mn>
<mml:mo>,</mml:mo>
</mml:math>
<label>(26)</label>
</disp-formula>where <inline-formula id="inf8">
<mml:math id="m34">
<mml:msup>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
</mml:math>
</inline-formula> is the radial comoving velocity, <inline-formula id="inf9">
<mml:math id="m35">
<mml:msup>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mi>r</mml:mi>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
</mml:math>
</inline-formula> is the tangential comoving velocity, and <italic>f</italic>
<sub>
<italic>g</italic>
</sub> and <italic>f</italic>
<sub>
<italic>c</italic>
</sub> are the radial gravitational and centrifugal forces in the comoving coordinate system. If we assume that the orbit of the particle is stationary, the radial and centrifugal forces are balanced (<italic>f</italic>
<sub>
<italic>g</italic>
</sub> &#x3d; &#x2212;<italic>f</italic>
<sub>
<italic>c</italic>
</sub>) and the RHS of Eq.&#xa0;<xref ref-type="disp-formula" rid="e25">25</xref> equals zero. Consequently, we get<disp-formula id="e27">
<mml:math id="m36">
<mml:mi>a</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>V</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mi mathvariant="normal">c</mml:mi>
<mml:mi mathvariant="normal">o</mml:mi>
<mml:mi mathvariant="normal">n</mml:mi>
<mml:mi mathvariant="normal">s</mml:mi>
<mml:mi mathvariant="normal">t</mml:mi>
<mml:mo>,</mml:mo>
</mml:math>
<label>(27)</label>
</disp-formula>
<disp-formula id="e28">
<mml:math id="m37">
<mml:mi>a</mml:mi>
<mml:mi>r</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>v</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mi>r</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>V</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mi mathvariant="normal">c</mml:mi>
<mml:mi mathvariant="normal">o</mml:mi>
<mml:mi mathvariant="normal">n</mml:mi>
<mml:mi mathvariant="normal">s</mml:mi>
<mml:mi mathvariant="normal">t</mml:mi>
<mml:mo>,</mml:mo>
</mml:math>
<label>(28)</label>
</disp-formula>where <italic>V</italic>
<sup>
<italic>r</italic>
</sup> and <italic>V</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> are the radial and tangential components of the proper velocity <italic>V</italic>. For a circular orbit in the comoving coordinates, Eqs.&#xa0;<xref ref-type="disp-formula" rid="e27">27</xref>, <xref ref-type="disp-formula" rid="e28">28</xref> are further simplified as<disp-formula id="e29">
<mml:math id="m38">
<mml:msup>
<mml:mrow>
<mml:mi>V</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>0</mml:mn>
<mml:mo>,</mml:mo>
<mml:mspace width="0.17em"/>
<mml:mspace width="0.17em"/>
<mml:msup>
<mml:mrow>
<mml:mi>V</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mi mathvariant="normal">c</mml:mi>
<mml:mi mathvariant="normal">o</mml:mi>
<mml:mi mathvariant="normal">n</mml:mi>
<mml:mi mathvariant="normal">s</mml:mi>
<mml:mi mathvariant="normal">t</mml:mi>
<mml:mo>,</mml:mo>
</mml:math>
<label>(29)</label>
</disp-formula>
<disp-formula id="e30">
<mml:math id="m39">
<mml:mi>r</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mi mathvariant="normal">c</mml:mi>
<mml:mi mathvariant="normal">o</mml:mi>
<mml:mi mathvariant="normal">n</mml:mi>
<mml:mi mathvariant="normal">s</mml:mi>
<mml:mi mathvariant="normal">t</mml:mi>
<mml:mo>,</mml:mo>
<mml:mspace width="0.17em"/>
<mml:mi>R</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mi>a</mml:mi>
<mml:msub>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msub>
<mml:mo>,</mml:mo>
</mml:math>
<label>(30)</label>
</disp-formula>where subscript &#x201c;0&#x201d; refers to the quantity at present.</p>
</sec>
<sec id="s2-5">
<title>2.5 Physical consequences for the evolution of local systems</title>
<p>Eq.&#xa0;<xref ref-type="disp-formula" rid="e30">30</xref> is surprising and in contradiction to the common opinion that the expansion of the Universe is without any appreciable effect on local gravitational systems (<xref ref-type="bibr" rid="B27">Carrera and Giulini, 2010</xref>). This opinion is based on equations for gravitational orbits in an expanding space described by the FLRW metric (see <xref ref-type="app" rid="app1">Appendix&#xa0;A</xref>). The equations were derived by many authors (<xref ref-type="bibr" rid="B40">Dicke and Peebles, 1964</xref>; <xref ref-type="bibr" rid="B133">Pachner, 1964</xref>; <xref ref-type="bibr" rid="B24">Callan&#xa0;et&#xa0;al., 1965</xref>; <xref ref-type="bibr" rid="B29">Cooperstock&#xa0;et&#xa0;al., 1998</xref>; <xref ref-type="bibr" rid="B54">Faraoni and Jacques, 2007</xref>; <xref ref-type="bibr" rid="B155">Sereno and Jetzer, 2007</xref>; <xref ref-type="bibr" rid="B27">Carrera and Giulini, 2010</xref>) and they differ from the standard Newtonian equations for orbits in the static Universe only slightly. The only difference is that the equation for the radial acceleration of an orbiting body in the gravitational field imbedded in the space with the FLRW metric contains a term <inline-formula id="inf10">
<mml:math id="m40">
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>R</mml:mi>
</mml:math>
</inline-formula>, which is related to the space expansion (see <xref ref-type="app" rid="app1">Appendix&#xa0;A</xref>, Eq. A-7). It can be shown that this term might be appreciable in dynamics of large-scale structures as galaxy clusters, but the orbits within galaxies are affected negligibly. Consequently, all gravitationally bound systems with size of galaxies or smaller should be unaffected by the space expansion.</p>
<p>By contrast, considering the CC metric for the expanding Universe, the evolution of the local gravitational systems is essentially different from that obtained for the FLRW metric. In particular, the CC metric predicts:<list list-type="simple">
<list-item>
<p>1 An increase of the proper orbital radius <italic>R</italic>
<sub>orb</sub> with the expansion irrespective of the size of the local system and an increase of the proper orbital period <italic>T</italic>
<sub>orb</sub> with the expansion. Consequently, the size of galaxies (and all other local gravitational systems) must growth in the expanding Universe. The rate of growth is (1 &#x2b; <italic>z</italic>)<sup>&#x2212;1</sup>. The orbit is stationary in comoving coordinates but non-stationary in proper coordinates.</p>
</list-item>
<list-item>
<p>2 A constant proper rotation velocity <italic>V</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> of particles along the orbits irrespective of the orbital radius during the space expansion. Hence, the stationary circular orbits in the comoving coordinate system become spirals in the proper coordinate system. Stars and gas within spirals have flat rotation curves. Since the flat rotation curves are a consequence of the expansion of the Universe, no dark matter is needed to explain dynamics of galaxies.</p>
</list-item>
</list>
</p>
</sec>
</sec>
<sec id="s3">
<title>3 Numerical modelling of the galaxy dynamics</title>
<p>In this section, we will examine the evolution of local gravitationally bounded systems in the expanding Universe by numerical modelling. The modelling is simple and reflects only basic features of the galaxy evolution. It is focused on studying the formation of spirals and their evolution in time. The gravitational field is axially symmetric and interactions between stars and gas inside spirals are neglected. The aim is just to demonstrate the potential of the derived Eqs&#xa0;<xref ref-type="disp-formula" rid="e29">29</xref>, <xref ref-type="disp-formula" rid="e30">30</xref> of gravitational orbits in the CC metric for the full realistic modelling of the galaxy evolution in future studies.</p>
<sec id="s3-1">
<title>3.1 Parameters for modelling</title>
<p>For modelling, we need to specify the expanding history of the Universe described by the Hubble parameter <italic>H</italic>(<italic>z</italic>). Since we do not use the FLRW metric, we cannot adopt the &#x39b;CDM model. Instead, the CC metric described by Eq.&#xa0;<xref ref-type="disp-formula" rid="e17">17</xref> must be used. According to <xref ref-type="bibr" rid="B175">Vavry&#x10d;uk (2022a)</xref>, we use parameters &#x3a9;<sub>
<italic>m</italic>
</sub> &#x3d; 1.2, &#x3a9;<sub>&#x39b;</sub> &#x3d; 0 (no dark energy), and &#x3a9;<sub>
<italic>k</italic>
</sub> &#x3d; &#x2212;0.2 (closed Universe). The Hubble constant is <italic>H</italic>
<sub>0</sub> &#x3d; 69.8&#xa0;km&#xa0;s<sup>&#x2212;1</sup>&#xa0;Mpc<sup>&#x2212;1</sup>, obtained by <xref ref-type="bibr" rid="B57">Freedman&#xa0;et&#xa0;al. (2019)</xref> from observations of the SNe Ia data with a red giant calibration. Obviously, Eqs.&#xa0;<xref ref-type="disp-formula" rid="e17">17</xref>, <xref ref-type="disp-formula" rid="e19">19</xref> predict a quite different evolution of the Hubble parameter and a time-redshift relation than the &#x39b;CDM model. For example, redshift <italic>z</italic> &#x3d; 4 corresponds to the cosmic time of 12&#xa0;Gyr for the &#x39b;CDM model but 8.2&#xa0;Gyr for the CC model (see <xref ref-type="fig" rid="F1">Figure&#xa0;1</xref>).</p>
<fig id="F1" position="float">
<label>FIGURE 1</label>
<caption>
<p>The Hubble parameter <bold>(A)</bold> and the proper cosmic lookback time <bold>(B)</bold> as a function of redshift. The cosmological model is described by Eq.&#xa0;<xref ref-type="disp-formula" rid="e17">17</xref> for the CC metric (blue line) with &#x3a9;<sub>
<italic>m</italic>
</sub> &#x3d; 1.2, and &#x3a9;<sub>
<italic>k</italic>
</sub> &#x3d; &#x2212;0.2 (<xref ref-type="bibr" rid="B175">Vavry&#x10d;uk, 2022a</xref>). The red line shows the standard &#x39b;CDM model. The Hubble constant is <italic>H</italic>
<sub>0</sub> &#x3d; 69.8&#xa0;km&#xa0;s<sup>&#x2212;1</sup>&#xa0;Mpc<sup>&#x2212;1</sup>, obtained by <xref ref-type="bibr" rid="B57">Freedman&#xa0;et&#xa0;al. (2019)</xref> from observations of the SNe Ia data with a red giant calibration. Note that panel <bold>(B)</bold> does not imply that the age of the Universe is less than about 9 Gyr in the CC model. For redshifts <italic>z</italic> &#x3e; 15, the cosmic evolution becomes more complicated due to light-matter interactions, and Eq.&#xa0;<xref ref-type="disp-formula" rid="e17">17</xref> must be modified, see <xref ref-type="bibr" rid="B174">Vavry&#x10d;uk (2022b)</xref>.</p>
</caption>
<graphic xlink:href="fspas-10-1071743-g001.tif"/>
</fig>
<p>The galaxy is assumed to be formed by a bulge and disk with the following exponential density profiles (<xref ref-type="bibr" rid="B113">McGaugh, 2016</xref>)<disp-formula id="e31">
<mml:math id="m41">
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a3;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>b</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a3;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>b</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:msub>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>b</mml:mi>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msub>
</mml:mrow>
</mml:mfenced>
<mml:msup>
<mml:mrow>
<mml:mi>e</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>r</mml:mi>
<mml:mo>&#x2212;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>b</mml:mi>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msub>
</mml:mrow>
</mml:mfenced>
<mml:mo>/</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>b</mml:mi>
</mml:mrow>
</mml:msub>
</mml:mrow>
</mml:msup>
<mml:mo>,</mml:mo>
</mml:math>
<label>(31)</label>
</disp-formula>
<disp-formula id="e32">
<mml:math id="m42">
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a3;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a3;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:msub>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msub>
</mml:mrow>
</mml:mfenced>
<mml:msup>
<mml:mrow>
<mml:mi>e</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>r</mml:mi>
<mml:mo>&#x2212;</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msub>
</mml:mrow>
</mml:mfenced>
<mml:mo>/</mml:mo>
<mml:msub>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
</mml:mrow>
</mml:msub>
</mml:mrow>
</mml:msup>
<mml:mo>,</mml:mo>
</mml:math>
<label>(32)</label>
</disp-formula>where &#x3a3;<sub>
<italic>b</italic>
</sub>(<italic>R</italic>) and &#x3a3;<sub>
<italic>d</italic>
</sub>(<italic>R</italic>) are the surface densities of the bulge and disk, respectively. The required parameters are for the bulge &#x3a3;<sub>
<italic>b</italic>
</sub>(<italic>R</italic>
<sub>
<italic>b</italic>0</sub>) &#x3d; 3.6&#xa0;M<sub>&#x2299;</sub>&#xa0;pc<sup>&#x2212;2</sup>, <italic>R</italic>
<sub>
<italic>b</italic>0</sub> &#x3d; 2.5&#xa0;kpc, <italic>R</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 0.3&#xa0;kpc, and for the disk &#x3a3;<sub>
<italic>d</italic>
</sub>(<italic>R</italic>
<sub>
<italic>d</italic>0</sub>) &#x3d; 99.2&#xa0;M<sub>&#x2299;</sub>&#xa0;pc<sup>&#x2212;2</sup>, <italic>R</italic>
<sub>
<italic>d</italic>0</sub> &#x3d; 8.0&#xa0;kpc, <italic>R</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 2.8&#xa0;kpc. The total masses of the bulge and disk are <italic>M</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>9</sup>&#xa0;M<sub>&#x2299;</sub> and <italic>M</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>10</sup>&#xa0;M<sub>&#x2299;</sub>, respectively. The bulge is usually modelled as a prolate, triaxial bar (<xref ref-type="bibr" rid="B14">Binney&#xa0;et&#xa0;al., 1997</xref>; <xref ref-type="bibr" rid="B15">Bissantz and Gerhard, 2002</xref>), but we do not focus on modelling a 3D geometry of the bulge and its evolution, so the simplified approximation described by Eq.&#xa0;<xref ref-type="disp-formula" rid="e31">31</xref> is satisfactory.</p>
</sec>
<sec id="s3-2">
<title>3.2 Bulge-bar region and spirals</title>
<p>The density profiles and the Newtonian rotation curves predicted for the used parameters are shown in <xref ref-type="fig" rid="F2">Figure&#xa0;2</xref>. The total rotation curve (<xref ref-type="fig" rid="F2">Figure&#xa0;2B</xref>, black line) is separated into two domains. The separation (critical) distance <italic>R</italic>
<sub>
<italic>c</italic>
</sub> is about 4&#xa0;kpc (<xref ref-type="fig" rid="F2">Figure&#xa0;2B</xref>, dashed vertical line) and corresponds to the maximum rotation velocity associated with the disk density profile (<xref ref-type="fig" rid="F2">Figure&#xa0;2B</xref>, red line). For shorter distances (bulge-bar domain), the behaviour of the rotation curve is complex being affected by both the bulge and disk. For larger distances (spiral domain), the initial rotation curve is monotonously decreasing affected mostly by the total mass in the bulge-bar area. Obviously, the critical distance <italic>R</italic>
<sub>
<italic>c</italic>
</sub> may vary for different galaxies being dependent on their mass and density profiles. As discussed below, the rotation curve evolves in time and the final rotation curve becomes flat in the spiral domain (<xref ref-type="fig" rid="F2">Figure&#xa0;2B</xref>, green line).</p>
<fig id="F2" position="float">
<label>FIGURE 2</label>
<caption>
<p>The density profile <bold>(A)</bold> and the initial and final rotation velocity curves <bold>(B)</bold> for a simulated galaxy. The surface densities of the bulge (blue line in <bold>(A)</bold>) and disk (red line in <bold>(A)</bold>) are calculated by Eqs&#xa0;<xref ref-type="disp-formula" rid="e31">31</xref>, <xref ref-type="disp-formula" rid="e32">32</xref> with &#x3a3;<sub>
<italic>b</italic>
</sub>(<italic>R</italic>
<sub>
<italic>b</italic>0</sub>) &#x3d; 3.6&#xa0;M<sub>&#x2299;</sub>pc<sup>&#x2212;2</sup>, <italic>R</italic>
<sub>
<italic>b</italic>0</sub> &#x3d; 2.5&#xa0;kpc, <italic>R</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 0.3&#xa0;kpc for the bulge, and with &#x3a3;<sub>
<italic>d</italic>
</sub>&#xa0;(<italic>R</italic>
<sub>
<italic>d</italic>0</sub>) &#x3d; 99.2&#xa0;M<sub>&#x2299;</sub>&#xa0;pc<sup>&#x2212;2</sup>, <italic>R</italic>
<sub>
<italic>d</italic>0</sub> &#x3d; 8.0&#xa0;kpc, <italic>R</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 2.8&#xa0;kpc for the disk. The total masses of the bulge and disk are <italic>M</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>9</sup>&#xa0;M<sub>&#x2299;</sub> and <italic>M</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>10</sup>&#xa0;M<sub>&#x2299;</sub>, respectively. The total initial rotation velocity (black line in <bold>(B)</bold>) is shown together with the contribution of the bulge (blue line in <bold>(B)</bold>) and disk (red line in <bold>(B)</bold>). The vertical dashed line in <bold>(B)</bold> defines the boundary <italic>R</italic>
<sub>
<italic>c</italic>
</sub> &#x3d; 4&#xa0;kpc between the bulge-bar regime and the trailing-spiral regime. The green line in <bold>(B)</bold> shows the final rotation curve caused by the space expansion (the stellar mass and gas with <italic>R</italic> &#x3e; <italic>R</italic>
<sub>
<italic>c</italic>
</sub> are continuously moving out of the galaxy centre, but they keep their rotation velocity).</p>
</caption>
<graphic xlink:href="fspas-10-1071743-g002.tif"/>
</fig>
<p>
<xref ref-type="fig" rid="F3">Figure&#xa0;3</xref> shows the bulge-bar and spiral regions for the spiral galaxy UGC 6093 together with a scheme suggesting a possible origin of spirals and their temporal evolution. The bulge-bar region is characterized by a high concentration of stars and gas. Consequently, gravitational forces maintain the shape of the galaxy inside this region, irrespective of its rotation. Since the bar is continuously increasing due to the space expansion, its ends cross the region boundary and outflow from the bulge-bar region into the spiral region. In this region, the radial gravitational forces become dominant and stars and gas move as bodies in a spherically symmetric gravitational field. Their motion will be described by Eqs.&#xa0;<xref ref-type="disp-formula" rid="e29">29</xref>, <xref ref-type="disp-formula" rid="e30">30</xref>: the rotation velocity will be constant with time but the orbital radius will increase. Consequently, the rotating bar will outstrip the material in the spiral region, which will form a pattern of trailing spirals. The material will display flat rotation curves in all spirals, and the size of galaxies will increase with time.</p>
<fig id="F3" position="float">
<label>FIGURE 3</label>
<caption>
<p>The spiral galaxy UGC 6093 observed by ESA/Hubble <bold>(A)</bold> and the scheme of the spiral galaxy <bold>(B)</bold>. The bulge and bar of the galaxy in plot <bold>(B)</bold> is marked by the purple colour. The purple arrows in <bold>(B)</bold> show the rotation direction of the bar. The black arrows in <bold>(B)</bold> show the direction of the outflow from the bulge-bar domain into the spiral domain. The white dashed circle in <bold>(A)</bold> and the solid black circle in <bold>(B)</bold> mark the boundary between the bulge-bar and spiral domains.</p>
</caption>
<graphic xlink:href="fspas-10-1071743-g003.tif"/>
</fig>
</sec>
<sec id="s3-3">
<title>3.3 Scenarios of the galaxy evolution</title>
<p>The form of spirals depends on several factors: 1) The radius of the bulge-bar area, 2) the age of the galaxy, 3) the mass of the galaxy, density profile and its rotation velocity, and 4) the expansion history of the Universe. Therefore, we assume several alternative scenarios in the numerical modelling, where we vary some of these parameters. The radius of the bulge-bar area <italic>R</italic>
<sub>
<italic>c</italic>
</sub> will be considered 3, 4, and 5&#xa0;kpc. The age of a galaxy will be 8.0, 8.5, and 8.8&#xa0;Gyr. This age will correspond to the redshift <italic>z</italic> of 3.2, 5.6, and 11.2. The masses of the bulge and disk of a galaxy are <italic>M</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>9</sup>&#xa0;M<sub>&#x2299;</sub> and <italic>M</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>10</sup>&#xa0;M<sub>&#x2299;</sub>, but we will also model a galaxy with a half of this mass and with a twice higher mass.</p>
<p>In order to simulate a more realistic galaxy evolution, we assume random conditions for the bulge-bar outflow. The critical distance <italic>R</italic>
<sub>
<italic>c</italic>
</sub> is not defined by a single value, but it varies according to the Gaussian distribution with the standard deviation of 0.05&#xa0;kpc. Similarly, the bulge-bar outflow does not cross the domain boundary at two single points defined at the two ends of the bar by angles <italic>&#x3d5;</italic> &#x3d; 0&#xb0; and 180&#xb0;. Instead, angle <italic>&#x3d5;</italic> obeys the Gaussian distribution centred at 0&#xb0; and 180&#xb0; with the standard deviation of 20&#xb0;.</p>
</sec>
<sec id="s3-4">
<title>3.4 Results</title>
<p>In modelling, we calculate orbits of stars and gas flowed out from the bulge-bar domain into the spiral domain and the evolution of the orbits in time. Geometry of orbits is defined by Eqs.&#xa0;<xref ref-type="disp-formula" rid="e29">29</xref>, <xref ref-type="disp-formula" rid="e30">30</xref>, in which we specify the rotation velocity at the boundary between the bulge-bar and spiral regions and the expansion history defined by the Hubble parameter <italic>H</italic>(<italic>z</italic>). <xref ref-type="fig" rid="F4">Figure&#xa0;4</xref> shows the evolution of a galaxy with age of 8.8&#xa0;Gyr. The galaxy started to evolve at redshift <italic>z</italic> of 11.2. The galaxy was formed just by the bulge and bar with no spirals at the beginning of the simulation. At this time, the radius of the galaxy was 4&#xa0;kpc being the same as the radius of the bulge-bar area. The material, which outflowed from the bulge-bar domain due to the space expansion, formed typical trailed spirals during the galaxy evolution (<xref ref-type="fig" rid="F4">Figure&#xa0;4B</xref>). Hence, the radius of the galaxy increased from 4&#xa0;kpc to 49&#xa0;kpc during its life (<xref ref-type="fig" rid="F4">Figure&#xa0;4A</xref>). The rotation velocity of the material in the spirals is uniform and attains a value of 217.7&#xa0;km/s. The classical problem in the galaxy dynamics called the &#x201c;winding paradox&#x201d; of spirals (<xref ref-type="bibr" rid="B55">Ferreras, 2019</xref>) cannot appear, because the radius of spirals is continuously increased and spiral arms are moving away from the bulge-bar region.</p>
<fig id="F4" position="float">
<label>FIGURE 4</label>
<caption>
<p>The proper radius of a galaxy as a function of redshift <bold>(A)</bold>, and the spiral arms formed during the galaxy evolution <bold>(B)</bold>. The density of the material in the spiral arms in <bold>(B)</bold> is colour coded. The age of the galaxy is 8.8&#xa0;Gyr and the maximum redshift is <italic>z</italic> &#x3d; 11.2. The solid black circle in <bold>(B)</bold> marks the boundary between the bulge-bar and spiral domains with radius <italic>R</italic>
<sub>
<italic>c</italic>
</sub> &#x3d; 4&#xa0;kpc. The black dashed line in <bold>(B)</bold> denotes the central orbit with unperturbed parameters <italic>R</italic>
<sub>
<italic>c</italic>
</sub> and <italic>&#x3d5;</italic>. The other orbits forming the spirals are characterized by perturbed parameters <italic>R</italic>
<sub>
<italic>c</italic>
</sub> and <italic>&#x3d5;</italic>, see the text. The red bulge and bar inside the black circle in <bold>(B)</bold> illustrate schematically the orientation of the bar.</p>
</caption>
<graphic xlink:href="fspas-10-1071743-g004.tif"/>
</fig>
<p>
<xref ref-type="fig" rid="F5">Figure&#xa0;5</xref> demonstrates a dependence of the spiral pattern on the size of the bulge-bar area. The age of the galaxy is again 8.8 Gyr and the evolution started at redshift <italic>z</italic> of 11.2. For a smaller radius of the bulge-bar area (<xref ref-type="fig" rid="F5">Figure&#xa0;5A</xref>, <italic>R</italic>
<sub>
<italic>c</italic>
</sub> &#x3d; 3&#xa0;kpc), the rotation velocity is slightly higher being 218.3&#xa0;km/s. As a result, the orbital period is smaller and the recession of the spirals from the central part of the galaxy is not so pronounced. By contrast, for a larger radius of the bulge-bar area (<xref ref-type="fig" rid="F5">Figure&#xa0;5C</xref>, <italic>R</italic>
<sub>
<italic>c</italic>
</sub> &#x3d; 5&#xa0;kpc), the rotation velocity is slightly lower being 215.2&#xa0;km/s. The orbital period is higher and the recession of the spirals from the central part of the galaxy is more distinct.</p>
<fig id="F5" position="float">
<label>FIGURE 5</label>
<caption>
<p>Geometry of spirals: dependence on the initial size of the bulge-bar region. The age of the galaxy is 8.8&#xa0;Gyr and the maximum redshift is <italic>z</italic> &#x3d; 11.2. The upper/lower plots show orbits with unperturbed/perturbed parameters <italic>R</italic>
<sub>
<italic>c</italic>
</sub> and <italic>&#x3d5;</italic>. The critical radius <italic>R</italic>
<sub>
<italic>c</italic>
</sub> and the rotation velocity <italic>V</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> are 3&#xa0;kpc and 218.3&#xa0;km/s in <bold>(A, B)</bold>, 4&#xa0;kpc and 217.7&#xa0;km/s in <bold>(C, D)</bold>, and 5&#xa0;kpc and 215.2&#xa0;km/s in <bold>(E, F)</bold>. The masses of the bulge and disk are <italic>M</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>9</sup>&#xa0;M<sub>&#x2299;</sub> and <italic>M</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>10</sup>&#xa0;M<sub>&#x2299;</sub>, respectively.</p>
</caption>
<graphic xlink:href="fspas-10-1071743-g005.tif"/>
</fig>
<p>
<xref ref-type="fig" rid="F6">Figure&#xa0;6</xref> shows how is the spiral pattern affected by the age of the galaxy. The figure shows three galaxies with the age of 8.0, 8.5, and 8.8&#xa0;Gyr. The corresponding redshifts are 3.2, 5.6, and 11.2. The radius of the bulge-bar area is <italic>R</italic>
<sub>
<italic>c</italic>
</sub> &#x3d; 4&#xa0;kpc and the rotation velocity is 217.7&#xa0;km/s for all three galaxies. As expected, the younger the galaxy, the less evolved the spiral pattern. Consequently, the final radius of the galaxy increased from 4&#xa0;kpc to 17, 26, and 49&#xa0;kpc, respectively.</p>
<fig id="F6" position="float">
<label>FIGURE 6</label>
<caption>
<p>Geometry of spirals: dependence on the galaxy age. The critical radius <italic>R</italic>
<sub>
<italic>c</italic>
</sub> and the rotation velocity <italic>V</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> are 4&#xa0;kpc and 217.7&#xa0;km/s. The upper/lower plots show orbits with unperturbed/perturbed parameters <italic>R</italic>
<sub>
<italic>c</italic>
</sub> and <italic>&#x3d5;</italic>. The galaxy age and the maximum redshift are 8.0&#xa0;Gyr and <italic>z</italic> &#x3d; 3.20 in <bold>(A, B)</bold>, 8.5&#xa0;Gyr and <italic>z</italic> &#x3d; 5.65 in <bold>(C, D)</bold>, and 8.8&#xa0;Gyr and <italic>z</italic> &#x3d; 11.18 in <bold>(E, F)</bold>. The masses of the bulge and disk are <italic>M</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>9</sup>&#xa0;M<sub>&#x2299;</sub> and <italic>M</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>10</sup>&#xa0;M<sub>&#x2299;</sub>, respectively.</p>
</caption>
<graphic xlink:href="fspas-10-1071743-g006.tif"/>
</fig>
<p>Finally, <xref ref-type="fig" rid="F7">Figure&#xa0;7</xref> presents how is the spiral pattern affected by the mass of a galaxy. <xref ref-type="fig" rid="F7">Figure&#xa0;7B</xref> shows a galaxy with masses of the bulge and disk of a galaxy are <italic>M</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>9</sup>&#xa0;M<sub>&#x2299;</sub> and <italic>M</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>10</sup>&#xa0;M<sub>&#x2299;</sub> (rotation velocity at <italic>R</italic>
<sub>
<italic>c</italic>
</sub> &#x3d; 4&#xa0;kpc is 217.7&#xa0;km/s). These values were used in all previous simulations (<xref ref-type="fig" rid="F4">Figures&#xa0;4</xref>&#x2013;<xref ref-type="fig" rid="F6">6</xref>). <xref ref-type="fig" rid="F7">Figure&#xa0;7A</xref> shows a galaxy, which has a twice higher mass. The corresponding rotation velocity at <italic>R</italic>
<sub>
<italic>c</italic>
</sub> &#x3d; 4&#xa0;kpc is 307.9&#xa0;km/s. By contrast, <xref ref-type="fig" rid="F7">Figure&#xa0;7C</xref> shows a galaxy, which has a twice lower mass. The corresponding rotation velocity at <italic>R</italic>
<sub>
<italic>c</italic>
</sub> &#x3d; 4&#xa0;kpc is 153.9&#xa0;km/s only. The age of the three galaxies is 8.8&#xa0;Gyr and their evolution started at redshift <italic>z</italic> &#x3d; 11.2. Since the galaxies have the same age, their size increases in the same way: from 4&#xa0;kpc to 49&#xa0;kpc. Still the spiral pattern is remarkably different for all three galaxies. The massive galaxy rotates fast and the spirals are receding slowly from the galaxy centre (<xref ref-type="fig" rid="F7">Figure&#xa0;7A</xref>). The galaxy with the smallest mass rotates slowly and the recession of spirals from the galaxy centre is high (<xref ref-type="fig" rid="F7">Figure&#xa0;7C</xref>).</p>
<fig id="F7" position="float">
<label>FIGURE 7</label>
<caption>
<p>Geometry of spirals: dependence on the galaxy mass. The critical radius <italic>R</italic>
<sub>
<italic>c</italic>
</sub>, the galaxy age and the maximum redshift are 4&#xa0;kpc, 8.8&#xa0;Gyr and <italic>z</italic> &#x3d; 11.18. The upper/lower plots show orbits with unperturbed/perturbed parameters <italic>R</italic>
<sub>
<italic>c</italic>
</sub> and <italic>&#x3d5;</italic>. The masses of the bulge and disk are <italic>M</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 17 &#xd7; 10<sup>9</sup>&#xa0;M<sub>&#x2299;</sub> and <italic>M</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 17 &#xd7; 10<sup>10</sup>&#xa0;M<sub>&#x2299;</sub> in <bold>(A, B)</bold>, <italic>M</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>9</sup>&#xa0;M<sub>&#x2299;</sub> and <italic>M</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 8.5 &#xd7; 10<sup>10</sup>&#xa0;M<sub>&#x2299;</sub> in <bold>(C, D)</bold>, and <italic>M</italic>
<sub>
<italic>b</italic>
</sub> &#x3d; 4.25 &#xd7; 10<sup>9</sup>&#xa0;M<sub>&#x2299;</sub> and <italic>M</italic>
<sub>
<italic>d</italic>
</sub> &#x3d; 4.25 &#xd7; 10<sup>10</sup>&#xa0;M<sub>&#x2299;</sub> in <bold>(E, F)</bold>. The rotation velocity <italic>V</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> is 307.9&#xa0;km/s in <bold>(A, B)</bold>, 217.7&#xa0;km/s in <bold>(C, D)</bold>, and 153.9&#xa0;km/s in <bold>(E, F)</bold>.</p>
</caption>
<graphic xlink:href="fspas-10-1071743-g007.tif"/>
</fig>
</sec>
</sec>
<sec id="s4">
<title>4 Supporting observational evidence</title>
<p>The presented results are supported by many observations difficult to explain under the standard cosmological model. This applies to galaxy dynamics, morphology of spiral galaxies as well as dynamics of the solar system. In the next, we review several puzzles in modern cosmology resolved by the proposed theory.</p>
<sec id="s4-1">
<title>4.1 Galaxy expansion</title>
<p>As shown in the previous sections, the size of galaxies should increase with redshift as (1 &#x2b; <italic>z</italic>)<sup>&#x2212;1</sup> with no change of the galaxy mass. Based on observations, it is accepted that the size of galaxies evolves rapidly during the cosmic time (<xref ref-type="bibr" rid="B172">van&#xa0;Dokkum&#xa0;et&#xa0;al., 2008</xref>; <xref ref-type="bibr" rid="B173">van&#xa0;Dokkum&#xa0;et&#xa0;al., 2010</xref>; <xref ref-type="bibr" rid="B183">Williams&#xa0;et&#xa0;al., 2010</xref>), see <xref ref-type="fig" rid="F8">Figure&#xa0;8</xref>. Using observations from the Hubble Space Telescope (HST), galaxy sizes defined by the effective radius, <italic>R</italic>
<sub>
<italic>e</italic>
</sub>, have been extensively measured with the Advanced Camera for Surveys (ACS) and the Wide Field Camera 3/IR channel on board HST for massive galaxies at <italic>z</italic> &#x3c; 3 (<xref ref-type="bibr" rid="B171">van&#xa0;der&#xa0;Wel&#xa0;et&#xa0;al., 2014</xref>) and <italic>z</italic> &#x2265; 3&#x2013;4 Lyman break galaxies (LBGs) selected in the dropout technique (<xref ref-type="bibr" rid="B168">Trujillo&#xa0;et&#xa0;al., 2006</xref>; <xref ref-type="bibr" rid="B33">Dahlen&#xa0;et&#xa0;al., 2007</xref>; <xref ref-type="bibr" rid="B114">McLure&#xa0;et&#xa0;al., 2013</xref>). The average size is reported to evolve according to <italic>R</italic>
<sub>
<italic>e</italic>
</sub> &#x223c; (1 &#x2b; <italic>z</italic>)<sup>&#x2212;<italic>B</italic>
</sup>, with <italic>B</italic> ranging most frequently between 0.8 and 1.2 (<xref ref-type="bibr" rid="B18">Bouwens&#xa0;et&#xa0;al., 2004</xref>; <xref ref-type="bibr" rid="B132">Oesch&#xa0;et&#xa0;al., 2010</xref>; <xref ref-type="bibr" rid="B66">Holwerda&#xa0;et&#xa0;al., 2015</xref>). For example, <xref ref-type="bibr" rid="B156">Shibuya&#xa0;et&#xa0;al. (2015)</xref> studied the redshift evolution of the galaxy effective radius <italic>R</italic>
<sub>
<italic>e</italic>
</sub> obtained from the HST samples of &#x223c;190,000 galaxies at <italic>z</italic> &#x3d; 0&#x2013;10, consisted of 176,152 photo-<italic>z</italic> galaxies at <italic>z</italic> &#x3d; 0&#x2013;6 from the 3D-HST &#x2b; CANDELS catalogue and 10,454 Lyman break galaxies (LBGs) at <italic>z</italic> &#x3d; 4&#x2013;10 identified in the CANDELS, HUDF 09/12, and HFF parallel fields. They found that <italic>R</italic>
<sub>
<italic>e</italic>
</sub> values at a given luminosity decrease toward high <italic>z</italic>, as <italic>R</italic>
<sub>
<italic>e</italic>
</sub> &#x223c; (1 &#x2b; <italic>z</italic>)<sup>&#x2212;<italic>B</italic>
</sup>, with <italic>B</italic> &#x3d; 1.10 &#xb1; 0.06 for median, see <xref ref-type="fig" rid="F8">Figure&#xa0;8A</xref>.</p>
<fig id="F8" position="float">
<label>FIGURE 8</label>
<caption>
<p>Galaxy size evolution with redshift. <bold>(A)</bold> Median of the effective galaxy radius <italic>R</italic> as a function of redshift for galaxies in the bin of <inline-formula id="inf11">
<mml:math id="m43">
<mml:msub>
<mml:mrow>
<mml:mi>L</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>U</mml:mi>
<mml:mi>V</mml:mi>
</mml:mrow>
</mml:msub>
<mml:mo>&#x3d;</mml:mo>
<mml:mrow>
<mml:mo stretchy="false">(</mml:mo>
<mml:mrow>
<mml:mn>0.3</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:mn>1</mml:mn>
</mml:mrow>
<mml:mo stretchy="false">)</mml:mo>
</mml:mrow>
<mml:mspace width="0.17em"/>
<mml:msubsup>
<mml:mrow>
<mml:mi>L</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>z</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>3</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mo>&#x2a;</mml:mo>
</mml:mrow>
</mml:msubsup>
</mml:math>
</inline-formula>. The red and cyan filled circles indicate radius <italic>R</italic> for star-forming galaxies measured in the optical (4,500&#x2013;8,000&#xa0;&#xc5;) and UV (1,500&#x2013;3,000&#xa0;&#xc5;) wavelength ranges, respectively. The blue filled circles indicate radius <italic>R</italic> for the Lyman break galaxies measured in the UV wavelength range. For details, see <xref ref-type="bibr" rid="B156">Shibuya&#xa0;et&#xa0;al. (2015</xref>, their Figure&#xa0;8). <bold>(B)</bold> Median Petrosian radius of galaxies as a function of redshift for the mass-limited sample in the range of 10<sup>9</sup>&#xa0;M<sub>&#x2299;</sub> &#x2264; <italic>M</italic>&#x2a; &#x2264; 10<sup>10.5</sup>&#xa0;M<sub>&#x2299;</sub>. The ratio of the surface brightness at radius <italic>R</italic> to the mean surface brightness of a galaxy is <italic>&#x3b7;</italic> &#x3d; 0.2. For details, see <xref ref-type="bibr" rid="B182">Whitney&#xa0;et&#xa0;al. (2019</xref>, their Figure&#xa0;8). The dashed lines in <bold>(A, B)</bold> show the size evolution predicted by the presented theory.</p>
</caption>
<graphic xlink:href="fspas-10-1071743-g008.tif"/>
</fig>
<p>Since it is believed that the size of galaxies cannot be affected by the expansion of the Universe, the observed expansion of galaxies is explained by other mechanisms. The most popular theory suggests the growth of galaxies being produced by galaxy mergers (<xref ref-type="bibr" rid="B124">Naab&#xa0;et&#xa0;al., 2009</xref>; <xref ref-type="bibr" rid="B79">Kormendy and Ho, 2013</xref>; <xref ref-type="bibr" rid="B114">McLure&#xa0;et&#xa0;al., 2013</xref>; <xref ref-type="bibr" rid="B28">Conselice, 2014</xref>). An important role in merging of galaxies play dark matter haloes (<xref ref-type="bibr" rid="B75">Kauffmann&#xa0;et&#xa0;al., 1993</xref>; <xref ref-type="bibr" rid="B120">Mo&#xa0;et&#xa0;al., 1998</xref>). Two types of mergers are distinguished: a major merger where the stellar masses of the galaxies are comparable, and a minor merger where the stellar mass of one galaxy is much lower.</p>
<p>However, the idea of the galaxy expansion due to galaxy mergers is controversial for several reasons (<xref ref-type="bibr" rid="B96">Lerner, 2018</xref>). First, observations indicate that the major and minor merger rates are much lower to explain the galaxy expansion (<xref ref-type="bibr" rid="B165">Taylor&#xa0;et&#xa0;al., 2010</xref>; <xref ref-type="bibr" rid="B101">Man&#xa0;et&#xa0;al., 2012</xref>; <xref ref-type="bibr" rid="B102">Man&#xa0;et&#xa0;al., 2016</xref>). For example, <xref ref-type="bibr" rid="B123">Mundy&#xa0;et&#xa0;al. (2017)</xref> report approximately 0.5 major mergers at <italic>z</italic> &#x3c; 3.5 representing an increase in stellar mass of 20%&#x2013;30% only when considering constant stellar mass samples. As regards minor mergers, <xref ref-type="bibr" rid="B128">Newman&#xa0;et&#xa0;al. (2012)</xref> studied 935 galaxies selected with 0.4 &#x3c; <italic>z</italic> &#x3c; 2.5 and concluded that minor merging cannot account for a rapid growth of the size seen at higher redshifts. <xref ref-type="bibr" rid="B102">Man&#xa0;et&#xa0;al. (2016)</xref> studied massive galaxies using the UltraVISTA/COSMOS catalogue, complemented with the deeper, higher resolution 3DHST &#x2b; CANDELS catalogue and estimated &#x223c;1 major merger and &#x223c;0.7 minor merger on average for a massive (<italic>M</italic>
<sub>&#x2a;</sub> &#x2265; 10<sup>10.8</sup>&#xa0;M<sub>&#x2299;</sub>) galaxy during <italic>z</italic> &#x3d; 0.1&#x2013;2.5. The observed number of major and minor mergers can increase the size of a massive quiescent galaxy by a factor of two at most. Hence, additional mechanisms are needed to fully explain the galaxy evolution. Second, mergers cannot explain the growth of spiral galaxies, because mergers destroy disks as shown by <xref ref-type="bibr" rid="B17">Bournaud&#xa0;et&#xa0;al. (2007)</xref>. Third, the idea of mergers implies an increase of stellar mass in galaxies over cosmic time. However, observations show no or slight mass evolution in time (<xref ref-type="bibr" rid="B23">Bundy&#xa0;et&#xa0;al., 2017</xref>; <xref ref-type="bibr" rid="B76">Kawinwanichakij&#xa0;et&#xa0;al., 2020</xref>).</p>
</sec>
<sec id="s4-2">
<title>4.2 Galaxy rotation curves</title>
<p>Another basic characteristics predicted by the presented theory are flat rotation curves of spiral galaxies. In Newton theory, a velocity of stars in a rotating galaxy is controlled by gravitational and centrifugal forces only. Assuming the Newton&#x2019;s gravitation law, a balance between the forces implies a decay of the orbital speed <italic>V</italic>(<italic>R</italic>) of a star with its distance <italic>R</italic> from the galaxy centre<disp-formula id="e33">
<mml:math id="m44">
<mml:msup>
<mml:mrow>
<mml:mi>V</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>G</mml:mi>
<mml:mi>M</mml:mi>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mo>,</mml:mo>
</mml:math>
<label>(33)</label>
</disp-formula>where <italic>M</italic>(<italic>R</italic>) is the mass of the galaxy as a function of <italic>R</italic>. Hence, the rotation curve <italic>V</italic>(<italic>R</italic>) decays as <italic>R</italic>
<sup>&#x2212;1/2</sup> provided the most of mass is concentrated in the galaxy centre. The same applies to the improved Newtonian equations in an expanding Universe described by the standard FLRW metric. Obviously, the flat rotation curves predicted by the improved Newtonian equations in the Universe with the CC metric point to fundamental differences between both the metrics. Importantly, the flat rotation curves of spiral galaxies are observationally confirmed.</p>
<sec id="s4-2-1">
<title>4.2.1 Observations of flat rotation curves</title>
<p>
<xref ref-type="bibr" rid="B146">Rubin and Ford (1970)</xref> discovered that the rotation curve of the Andromeda Galaxy has a sharp maximum of <italic>V</italic> &#x3d; 225&#xa0;km/s at <italic>R</italic> &#x3d; 400&#xa0;pc, a deep minimum at <italic>R</italic> &#x3d; 2&#xa0;kpc, and it is nearly flat at <italic>R</italic> &#x3e; 3&#xa0;kpc with the maximum velocity of 270 &#xb1; 10&#xa0;km/s. Such behaviour was later confirmed also for other spiral galaxies (<xref ref-type="bibr" rid="B145">Rubin&#xa0;et&#xa0;al., 1980</xref>; <xref ref-type="bibr" rid="B144">Rubin&#xa0;et&#xa0;al., 1985</xref>; <xref ref-type="bibr" rid="B170">van&#xa0;Albada&#xa0;et&#xa0;al., 1985</xref>; <xref ref-type="bibr" rid="B7">Begeman, 1989</xref>; <xref ref-type="bibr" rid="B150">Sanders, 1996</xref>; <xref ref-type="bibr" rid="B163">Swaters&#xa0;et&#xa0;al., 2000</xref>; <xref ref-type="bibr" rid="B161">Sofue and Rubin, 2001</xref>; <xref ref-type="bibr" rid="B37">de&#xa0;Blok and Bosma, 2002</xref>; <xref ref-type="bibr" rid="B36">de&#xa0;Blok&#xa0;et&#xa0;al., 2008</xref>; <xref ref-type="bibr" rid="B112">McGaugh, 2019</xref>; <xref ref-type="bibr" rid="B166">Tiley&#xa0;et&#xa0;al., 2019</xref>), for an example, see the rotation curve of the NGC 6503 Galaxy in <xref ref-type="fig" rid="F9">Figure&#xa0;9</xref>. The measurements of rotation curves are mostly based on (<xref ref-type="bibr" rid="B159">Sofue, 2017</xref>): observations of emission lines at optical wavelengths such as H<italic>&#x3b1;</italic> and [N<sub>II</sub>] lines, particularly, in H<sub>II</sub> regions in galactic disks; at infrared wavelengths revealing kinematics of dusty disks and nuclear regions of spiral galaxies with significant dust extinction; and at 21-cm H<sub>I</sub> line powerful to study kinematics of entire spiral galaxy.</p>
<fig id="F9" position="float">
<label>FIGURE 9</label>
<caption>
<p>Rotation curve for the NGC 6503 Galaxy. The spiral domain covering distances greater than 4&#xa0;kpc is indicated. In this domain, receding of spirals from the galaxy centre causes the flatness of the rotation curve. For data, see <xref ref-type="bibr" rid="B6">Begeman (1987)</xref> and <xref ref-type="bibr" rid="B93">Lelli&#xa0;et&#xa0;al. (2016a)</xref>.</p>
</caption>
<graphic xlink:href="fspas-10-1071743-g009.tif"/>
</fig>
<p>The rotation curves of spiral galaxies display a significant similarity irrespective of their morphology (<xref ref-type="bibr" rid="B137">Persic&#xa0;et&#xa0;al., 1996</xref>; <xref ref-type="bibr" rid="B160">Sofue, 2016</xref>; <xref ref-type="bibr" rid="B159">Sofue, 2017</xref>). The differences are mainly connected to the mass and size of the galaxies. More massive and larger galaxies (Sa and Sb) have high rotation velocity close to the nucleus, while smaller galaxies (Sc) show slower rotation in the centre. The earlier-type (Sa and Sb) galaxies display a flat or slowly declining velocity at the outermost part of the rotation curve, while the rotation velocity of the later-type (Sc) galaxies monotonically increases. Similarly, dwarf and LSB galaxies display monotonically increasing rotation velocity until their galaxy edges (<xref ref-type="bibr" rid="B163">Swaters&#xa0;et&#xa0;al., 2000</xref>; <xref ref-type="bibr" rid="B38">de&#xa0;Blok&#xa0;et&#xa0;al., 2001</xref>; <xref ref-type="bibr" rid="B164">Swaters&#xa0;et&#xa0;al., 2003</xref>). In addition, <xref ref-type="bibr" rid="B169">Tully and Fisher (1977)</xref> revealed an empirical statistical relation between the galaxy luminosity and the maximum rotation velocity at a few galactic disk radii. The Tully-Fisher relation is commonly used for estimating the luminosity of distant galaxies (<xref ref-type="bibr" rid="B73">Jacoby&#xa0;et&#xa0;al., 1992</xref>; <xref ref-type="bibr" rid="B109">Mathewson&#xa0;et&#xa0;al., 1992</xref>; <xref ref-type="bibr" rid="B139">Phillips, 1993</xref>) and for measuring the Hubble constant (<xref ref-type="bibr" rid="B122">Mould&#xa0;et&#xa0;al., 2000</xref>; <xref ref-type="bibr" rid="B56">Freedman&#xa0;et&#xa0;al., 2001</xref>).</p>
</sec>
<sec id="s4-2-2">
<title>4.2.2 Dark matter</title>
<p>To explain the discrepancy between predicted and observed rotation curves, several theories have been proposed. The most straightforward way is to assume the presence of dark matter (DM) with distribution calculated as (<xref ref-type="bibr" rid="B152">Schneider, 2015</xref>, his Eq.&#xa0;3.17)<disp-formula id="e34">
<mml:math id="m45">
<mml:msub>
<mml:mrow>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mtext>dark</mml:mtext>
</mml:mrow>
</mml:msub>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>G</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:msubsup>
<mml:mrow>
<mml:mi>V</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mtext>obs</mml:mtext>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msubsup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x2212;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>V</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
</mml:mfenced>
<mml:mo>,</mml:mo>
</mml:math>
<label>(34)</label>
</disp-formula>where <italic>V</italic>
<sub>obs</sub>(<italic>R</italic>) is the observed rotation velocity and <italic>V</italic>(<italic>R</italic>) is calculated according to Eq.&#xa0;<xref ref-type="disp-formula" rid="e33">33</xref>. The idea of dark matter origins from Zwicky (<xref ref-type="bibr" rid="B187">Zwicky, 1937</xref>; <xref ref-type="bibr" rid="B188">Zwicky, 2009</xref>) who postulated &#x201c;missing mass&#x201d; to account for the orbital velocities of galaxies in clusters. Originally, the DM was assumed to be baryonic formed by gas, dust and microscopic and macroscopic solid bodies including black-holes. Later on, the baryonic origin of DM was questioned and rejected. Since the analysis of galaxy rotation curves revealed that the mass of DM (<xref ref-type="bibr" rid="B170">van&#xa0;Albada&#xa0;et&#xa0;al., 1985</xref>; <xref ref-type="bibr" rid="B44">Dubinski and Carlberg, 1991</xref>; <xref ref-type="bibr" rid="B127">Navarro&#xa0;et&#xa0;al., 1996</xref>; <xref ref-type="bibr" rid="B137">Persic&#xa0;et&#xa0;al., 1996</xref>; <xref ref-type="bibr" rid="B126">Navarro&#xa0;et&#xa0;al., 1997</xref>) is much higher than estimates of dust and gas in galaxies (<xref ref-type="bibr" rid="B25">Calzetti&#xa0;et&#xa0;al., 2000</xref>; <xref ref-type="bibr" rid="B47">Dunne&#xa0;et&#xa0;al., 2000</xref>; <xref ref-type="bibr" rid="B43">Draine and Li, 2007</xref>; <xref ref-type="bibr" rid="B31">da&#xa0;Cunha&#xa0;et&#xa0;al., 2008</xref>; <xref ref-type="bibr" rid="B151">Sandstrom&#xa0;et&#xa0;al., 2013</xref>), DM was considered to be mostly of non-baryonic nature (<xref ref-type="bibr" rid="B181">White and Rees, 1978</xref>; <xref ref-type="bibr" rid="B35">Davis&#xa0;et&#xa0;al., 1985</xref>; <xref ref-type="bibr" rid="B180">White&#xa0;et&#xa0;al., 1987</xref>; <xref ref-type="bibr" rid="B100">Maddox&#xa0;et&#xa0;al., 1990</xref>; <xref ref-type="bibr" rid="B121">Moore&#xa0;et&#xa0;al., 1999</xref>; <xref ref-type="bibr" rid="B10">Bergstr&#xf6;m, 2000</xref>; <xref ref-type="bibr" rid="B11">Bertone and Hooper, 2018</xref>). To reconcile the theoretical and observed rotation curves, the DM is significant at large distances and forms a DM halo with the total mass exceeding the stellar galaxy mass by about one order or more (<xref ref-type="bibr" rid="B170">van&#xa0;Albada&#xa0;et&#xa0;al., 1985</xref>; <xref ref-type="bibr" rid="B44">Dubinski and Carlberg, 1991</xref>; <xref ref-type="bibr" rid="B127">Navarro&#xa0;et&#xa0;al., 1996</xref>; <xref ref-type="bibr" rid="B137">Persic&#xa0;et&#xa0;al., 1996</xref>).</p>
</sec>
<sec id="s4-2-3">
<title>4.2.3 Conformal Gravity and MOND theory</title>
<p>The non-baryonic DM concept is not, however, unanimously accepted. The non-baryonic DM is questioned, in particular, for its exotic and mysterious nature and for difficulties to be detected by other methods independent of gravity. Also, significant discrepancies with predictions of the &#x39b;CDM model on small scale are reported by many authors (<xref ref-type="bibr" rid="B87">Kroupa, 2015</xref>; <xref ref-type="bibr" rid="B39">Del&#xa0;Popolo and Le&#xa0;Delliou, 2017</xref>). Therefore, several alternative theories have been proposed to explain the flat rotation curves (<xref ref-type="bibr" rid="B103">Mannheim, 2006</xref>). The most famous alternative theories are the Conformal Gravity and Modified Newtonian Dynamics theory (<xref ref-type="bibr" rid="B103">Mannheim, 2006</xref>).</p>
<p>The Conformal Gravity (CG) attempts to solve both the problems of dark energy and dark matter. Similarly as the CC approach presented in this paper, the CG theory emphasizes the importance of conformal transformations for solving gravity problems (<xref ref-type="bibr" rid="B103">Mannheim, 2006</xref>). However, both the approaches are essentially different: the CC metric is applied to the standard GR equations, while the CG theory is based on modifying the GR equations, in order the equations to be conformally invariant. The CG equations are based on minimizing the Weyl action with the use of the Weyl conformal tensor rather than on the Einstein-Hilbert action (<xref ref-type="bibr" rid="B104">Mannheim, 1990</xref>; <xref ref-type="bibr" rid="B103">Mannheim, 2006</xref>; <xref ref-type="bibr" rid="B106">Mannheim, 2012</xref>). The CG theory avoids dark energy as well as fits rotation curves without use of dark matter. Unlike the Newtonian gravity, the CG is global theory, where both the local galactic and the exterior gravitational fields are considered. The rotation velocity is affected by a linear potential caused by the Hubble flow and by a quadratic potential caused by inhomogeneities (<xref ref-type="bibr" rid="B108">Mannheim and O&#x2019;Brien, 2011</xref>; <xref ref-type="bibr" rid="B105">Mannheim, 2019</xref>). As reported by <xref ref-type="bibr" rid="B105">Mannheim (2019)</xref>, the CG theory has successfully fitted rotation curves of 207 galaxies including dwarf galaxies, see also <xref ref-type="bibr" rid="B107">Mannheim and O&#x2019;Brien (2012)</xref> and <xref ref-type="bibr" rid="B131">O&#x2019;Brien and Mannheim (2012)</xref>.</p>
<p>The Modified Newtonian Dynamics (MOND) theory was presented by <xref ref-type="bibr" rid="B117">Milgrom (1983a)</xref>, <xref ref-type="bibr" rid="B116">Milgrom (1983b)</xref>, <xref ref-type="bibr" rid="B9">Bekenstein (2004)</xref>, <xref ref-type="bibr" rid="B118">Milgrom (2010)</xref>, and <xref ref-type="bibr" rid="B119">Milgrom (2012)</xref>, who proposed to modify the Newton gravity law for very low accelerations. Below <italic>a</italic>
<sub>0</sub> &#x223c; <italic>cH</italic>
<sub>0</sub>/6, the standard Newton gravity acceleration <italic>g</italic>
<sub>
<italic>N</italic>
</sub> is substituted by <inline-formula id="inf12">
<mml:math id="m46">
<mml:msqrt>
<mml:mrow>
<mml:msub>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
</mml:msub>
<mml:msub>
<mml:mrow>
<mml:mi>g</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>N</mml:mi>
</mml:mrow>
</mml:msub>
</mml:mrow>
</mml:msqrt>
</mml:math>
</inline-formula>. This causes that the Newton&#x2019;s law keeps valid for planetary and other small-scale systems but it does not apply to galaxies and galaxy clusters. As a consequence, rotation curves fit well observations (<xref ref-type="bibr" rid="B5">Begeman&#xa0;et&#xa0;al., 1991</xref>). Except for the flat rotation curves, the MOND theory is successful in accounting for some other phenomena listed below, which are difficult to explain using the DM hypothesis (<xref ref-type="bibr" rid="B149">Sanders and McGaugh, 2002</xref>; <xref ref-type="bibr" rid="B20">Bugg, 2015</xref>).</p>
<sec id="s4-2-3-1">
<title>4.2.3.1 Faint satellite galaxies</title>
<p>The existence of the non-baryonic DM is questioned by a detailed study of properties of faint satellite galaxies of the Milky Way (MW), see <xref ref-type="bibr" rid="B86">Kroupa&#xa0;et&#xa0;al. (2010)</xref>, which are distributed on a planar structure. Similar alignments were observed also in isolated dwarf galaxies in the local group (<xref ref-type="bibr" rid="B134">Pawlowski and Kroupa, 2013</xref>; <xref ref-type="bibr" rid="B135">Pawlowski and McGaugh, 2014</xref>) as well as in more distant galaxies (<xref ref-type="bibr" rid="B59">Galianni&#xa0;et&#xa0;al., 2010</xref>; <xref ref-type="bibr" rid="B45">Duc&#xa0;et&#xa0;al., 2014</xref>). This is a challenge for cosmological simulations, because the DM sub-haloes are assumed to be isotropically distributed.</p>
</sec>
<sec id="s4-2-3-2">
<title>4.2.3.2 Dual Dwarf Galaxy Theorem</title>
<p>The standard &#x39b;CDM model predicts two types of dwarf galaxies: Primordial DM dominated dwarf galaxies (Type A), and tidal and ram-pressure dwarf galaxies (Type B). While Type A dwarfs should surround the host galaxy spherically, the B dwarfs should be typically correlated in phase space. However, only dwarf galaxies of Type B are observed. This falsifies the Dual Dwarf Galaxy Theorem and the presence of DM haloes (<xref ref-type="bibr" rid="B88">Kroupa, 2012</xref>).</p>
</sec>
<sec id="s4-2-3-3">
<title>4.2.3.3 Baryonic Tully-Fisher relation</title>
<p>Observation of the baryonic Tully-Fisher (BTF) relation, which is a power-law relation between the rotation velocity of a galaxy and its baryonic mass <italic>M</italic>
<sub>S&#x2b;G</sub>, calculated as the sum of stellar mass <italic>M</italic>
<sub>S</sub> and gas mass <italic>M</italic>
<sub>G</sub> (<xref ref-type="bibr" rid="B176">Verheijen, 2001</xref>; <xref ref-type="bibr" rid="B130">Noordermeer and Verheijen, 2007</xref>; <xref ref-type="bibr" rid="B185">Zaritsky&#xa0;et&#xa0;al., 2014</xref>). This empirical relation is valid over several orders of magnitude and with an extremely small scatter. In the &#x39b;CDM model, the rotation velocity should be primarily related to the total virial mass, represented mostly by the dark matter halo, <italic>M</italic> &#x223c; <italic>V</italic>
<sup>3</sup>, but not to <italic>M</italic>
<sub>S&#x2b;G</sub>. Since the dark matter halo is largely independent of baryonic processes, it is difficult to explain the observed extremely low scatter of the BTF relation (<xref ref-type="bibr" rid="B94">Lelli&#xa0;et&#xa0;al., 2016b</xref>; <xref ref-type="bibr" rid="B111">McGaugh&#xa0;et&#xa0;al., 2018</xref>; <xref ref-type="bibr" rid="B92">Lelli&#xa0;et&#xa0;al., 2019</xref>). If the most mass of a galaxy is formed by the baryonic dark matter located in the galaxy disk but not in the halo, the close relation between the stellar, gas and dust masses is expected.</p>
</sec>
<sec id="s4-2-3-4">
<title>4.2.3.4 Radial acceleration relation</title>
<p>A further close connection between mass of stars and gas <italic>M</italic>
<sub>S&#x2b;G</sub> and the total mass <italic>M</italic> of galaxies, was revealed by <xref ref-type="bibr" rid="B110">McGaugh&#xa0;et&#xa0;al. (2016)</xref>, when they studied a relation between the acceleration <italic>g</italic>
<sub>S&#x2b;G</sub> due to mass <italic>M</italic>
<sub>S&#x2b;G</sub> and the observed acceleration <italic>g</italic>
<sub>obs</sub> due to total mass <italic>M</italic>. The observed relation is fully empirical and points to a strong coupling between the mass of the dark matter and mass of stars and gas. Similarly as for the BTF relation, the observed coupling between <italic>g</italic>
<sub>S&#x2b;G</sub> and <italic>g</italic>
<sub>obs</sub> is difficult to explain in the &#x39b;CDM model.</p>
</sec>
<sec id="s4-2-3-5">
<title>4.2.3.5 Deficiency of Conformal Gravity and MOND theory</title>
<p>Although, the MOND theory matches some observations quite successfully, the theory was originally designed rather empirically to fit observations with no profound physical consistency. For example, some deep reasoning, why value of <italic>a</italic>
<sub>0</sub> is within an order of magnitude of <italic>cH</italic>
<sub>0</sub>, is missing.</p>
<p>A common deficiency of MOND and CG seems violation of the GR equations. By contrast, theory presented in this paper explains satisfactorily the flat rotation curves and the above mentioned phenomena with no need to violate the GR theory. Nevertheless, we have to admit that the definitive resolution, whether GR or its modifications such as MOND (<xref ref-type="bibr" rid="B117">Milgrom, 1983a</xref>; <xref ref-type="bibr" rid="B9">Bekenstein, 2004</xref>; <xref ref-type="bibr" rid="B118">Milgrom, 2010</xref>; <xref ref-type="bibr" rid="B119">Milgrom, 2012</xref>) or Conformal Gravity (<xref ref-type="bibr" rid="B103">Mannheim, 2006</xref>; <xref ref-type="bibr" rid="B108">Mannheim and O&#x2019;Brien, 2011</xref>; <xref ref-type="bibr" rid="B107">Mannheim and O&#x2019;Brien, 2012</xref>; <xref ref-type="bibr" rid="B105">Mannheim, 2019</xref>) describe the gravitational field more appropriately, will need other future tests, e.g., based on detection of gravitational waves (<xref ref-type="bibr" rid="B30">Corda, 2009</xref>).</p>
</sec>
</sec>
</sec>
<sec id="s4-3">
<title>4.3 Morphology of spiral galaxies</title>
<p>Several theories have been proposed to explain the origin and evolution of structure of spiral galaxies and to predict basic properties of spiral arms (<xref ref-type="bibr" rid="B167">Toomre, 1977</xref>; <xref ref-type="bibr" rid="B42">Dobbs and Baba, 2014</xref>; <xref ref-type="bibr" rid="B158">Shu, 2016</xref>). <xref ref-type="bibr" rid="B99">Lindblad (1962)</xref> was the first, who assumed that the spiral structure arose from interaction between the orbits and gravitational forces of the stars of the disk, and suggested to explain the spiral arms as density waves. This idea was further elaborated by <xref ref-type="bibr" rid="B97">Lin and Shu (1964)</xref> and <xref ref-type="bibr" rid="B98">Lin and Shu (1966)</xref> in their hypothesis of the quasi-stationary density waves, in which the spirals are formed by standing waves in the disk. They assume that the spiral pattern rotates in a particular angular frequency different from the rotation velocity of stars, which depends on the star distance from the galaxy centre. The formation of the global spiral pattern is considered as an instability of the stellar disk caused by the self-gravity. The density-wave theory was further developed and extended (<xref ref-type="bibr" rid="B157">Shu, 1970</xref>; <xref ref-type="bibr" rid="B143">Roberts&#xa0;et&#xa0;al., 1975</xref>; <xref ref-type="bibr" rid="B153">Sellwood and Carlberg, 1984</xref>; <xref ref-type="bibr" rid="B50">Elmegreen&#xa0;et&#xa0;al., 1999</xref>; <xref ref-type="bibr" rid="B154">Sellwood, 2011</xref>) and it is now the main tool for studying the gravitational stability of disk galaxies. The results are not decisive, but <italic>N</italic>-body simulations suggest that the spiral arms are transient and recurrent rather than quasi-stationary (<xref ref-type="bibr" rid="B2">Baba&#xa0;et&#xa0;al., 2009</xref>; <xref ref-type="bibr" rid="B3">Baba&#xa0;et&#xa0;al., 2013</xref>).</p>
<p>The density-wave theory faces, however, with several open questions and limitations. First, the theory is based on the classical Newtonian gravity, which neglects the space expansion. Second, predictions of the theory are uncertain. Still it is not clearly resolved, whether the spiral arms must be dynamic or whether the quasi-static arms are a feasible solution. Third, the observationally documented growth of the spiral galaxies with cosmic time is completely ignored and unexplained in this theory.</p>
<p>All the mentioned difficulties with modelling of spiral arms arise from the fact that the theory starts with rejecting an idea of spirals formed by stars and gas that remain fixed in the spirals. The reason is the so-called winding problem, when objects moving with the same orbital speed in the disk cause a differential rotation of material in galaxies (<xref ref-type="bibr" rid="B55">Ferreras, 2019</xref>). Since the length of orbits is shorter near the galaxy centre, the inner part of spirals winds up tighter than its outer part. Hence, a typical spiral pattern disappears after a few rotations. This idea is, however, simplistic and incorrect, because the GR effects in the galaxy evolution are ignored. If the space expansion and time dilation are considered, the galaxy size is growing and galaxy rotation speed varies with time. The spiral pattern is not destroyed, because it is continuously expanding. Consequently, the winding problem does not occur as demonstrated by numerical modelling in <xref ref-type="sec" rid="s3">Section&#xa0;3</xref>.</p>
</sec>
<sec id="s4-4">
<title>4.4 Solar system</title>
<p>Observations confirm that the global expansion affects also the solar system. Here we mention some of prominent examples (<xref ref-type="bibr" rid="B1">Anderson&#xa0;et&#xa0;al., 1998</xref>; <xref ref-type="bibr" rid="B81">Krizek, 2012</xref>; <xref ref-type="bibr" rid="B71">Iorio, 2015</xref>; <xref ref-type="bibr" rid="B83">Krizek&#xa0;et&#xa0;al., 2015</xref>; <xref ref-type="bibr" rid="B85">Krizek and Somer, 2015</xref>).</p>
<sec id="s4-4-1">
<title>4.4.1 Faint young Sun paradox</title>
<p>According to the Standard solar model (<xref ref-type="bibr" rid="B4">Bahcall&#xa0;et&#xa0;al., 2001</xref>), the radius and luminosity of the Sun significantly evolved during the cosmic time. As the Sun is a star on the main sequence of the HR diagram, the solar radius was 4&#xa0;Gyr ago about 89% of the solar radius at present and the luminosity was about 73.8% of the present luminosity (<xref ref-type="bibr" rid="B4">Bahcall&#xa0;et&#xa0;al., 2001</xref>, their tables&#xa0;1 and 2). For a constant distance between the Sun and the Earth during this time span, such changes would have dramatic consequences for life conditions on the Earth (<xref ref-type="bibr" rid="B140">Ribas&#xa0;et&#xa0;al., 2010</xref>). The solar constant, i.e., the flux density at the Earth&#x2019;s mean orbital distance, is <italic>I</italic> &#x3d; 1.36&#xa0;kWm<sup>&#x2212;2</sup> at present (<xref ref-type="bibr" rid="B78">Kopp and Lean, 2011</xref>), but 4&#xa0;Gyr ago it was <italic>I</italic>
<sub>0</sub> &#x3d; 1.00&#xa0;kWm<sup>&#x2212;2</sup> only. Calculating the equilibrium temperature as<disp-formula id="e35">
<mml:math id="m47">
<mml:msup>
<mml:mrow>
<mml:mi>T</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mtext>eq</mml:mtext>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mfrac>
<mml:mrow>
<mml:mi>I</mml:mi>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>A</mml:mi>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
<mml:mrow>
<mml:mn>4</mml:mn>
<mml:mi>&#x3c3;</mml:mi>
</mml:mrow>
</mml:mfrac>
</mml:mrow>
</mml:mfenced>
</mml:mrow>
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>/</mml:mo>
<mml:mn>4</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>,</mml:mo>
</mml:math>
<label>(35)</label>
</disp-formula>where <italic>A</italic> &#x3d; 0.3 is the Earth&#x2019;s albedo (<xref ref-type="bibr" rid="B63">Goode&#xa0;et&#xa0;al., 2001</xref>) and <italic>&#x3c3;</italic> is the Stefan-Boltzmann constant, we get <italic>T</italic>
<sup>eq</sup> &#x3d; 254.5&#xa0;K and <inline-formula id="inf13">
<mml:math id="m48">
<mml:msubsup>
<mml:mrow>
<mml:mi>T</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mtext>eq</mml:mtext>
</mml:mrow>
</mml:msubsup>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>236.0</mml:mn>
<mml:mspace width="0.17em"/>
<mml:mi mathvariant="normal">K</mml:mi>
</mml:math>
</inline-formula> for the present time and for the past, respectively. Assuming the same level of the greenhouse effect (&#x2b;32.5&#xb0;C), the global average Earth&#x2019;s temperature would be &#x2212;4.7&#xb0;C in the past instead of 13.9&#xb0;C observed at present (<ext-link ext-link-type="uri" xlink:href="https://www.climate.gov/news-features/understanding-climate/climate-change-global-temperature">https://www.climate.gov/news-features/understanding-climate/climate-change-global-temperature</ext-link>). In fact, because of the ice albedo, the temperature would be even lower in the era of 4&#xa0;Gyr ago. For the Earth&#x2019;s albedo of 0.5, we get <inline-formula id="inf14">
<mml:math id="m49">
<mml:msubsup>
<mml:mrow>
<mml:mi>T</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>0</mml:mn>
</mml:mrow>
<mml:mrow>
<mml:mtext>eq</mml:mtext>
</mml:mrow>
</mml:msubsup>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>249.4</mml:mn>
<mml:mspace width="0.17em"/>
<mml:mi mathvariant="normal">K</mml:mi>
</mml:math>
</inline-formula> and the global average Earth&#x2019;s temperature would be &#x2212;23.8&#xb0;C. By contrast, no glaciation is indicated from geological observations in the first 2.7&#xa0;Gyr of the Earth&#x2019;s evolution (<xref ref-type="bibr" rid="B12">Bertotti&#xa0;et&#xa0;al., 2003</xref>) and water-related sediments have been found 3.8&#xa0;Gyr ago (<xref ref-type="bibr" rid="B184">Windley, 1984</xref>). This severe discrepancy is known as the Faint young Sun paradox.</p>
<p>The paradox is resolved, if the expansion of the solar system is taken into account (<xref ref-type="bibr" rid="B81">K&#x159;&#xed;&#x17e;ek, 2012</xref>; <xref ref-type="bibr" rid="B85">K&#x159;&#xed;&#x17e;ek and Somer, 2015</xref>). The age of 4&#xa0;Gyr corresponds to redshift <italic>z</italic> &#x3d; 0.46 (see <xref ref-type="fig" rid="F1">Figure&#xa0;1B</xref>) and the orbital radius of the Earth was (1 &#x2b; <italic>z</italic>) times shorter than at the present time. The flux corrected for a shorter orbital radius is easily calculated as 1.00 &#xd7; (1 &#x2b; <italic>z</italic>)<sup>2</sup> &#x3d; 2.13&#xa0;kWm<sup>&#x2212;2</sup> and the corresponding Earth&#x2019;s temperature is 44.5&#xb0;C, provided we assume the same greenhouse effect as at present (&#x2b;32.5&#xb0;C). Hence, the temperature conditions on the Earth were convenient for life over the whole Earth&#x2019;s history. Note that higher temperatures of oceans (70&#xb0;C) in the Precambrian era (3.5&#xa0;Gyr ago) are independently indicated by observations of silicon and oxygen isotope data (<xref ref-type="bibr" rid="B77">Knauth, 2005</xref>; <xref ref-type="bibr" rid="B142">Robert and Chaussidon, 2006</xref>). The recession velocity of the Earth from the Sun comparable to the Hubble flow is indicated also from growth patterns on fossil corals observed for the time span of the last 500&#xa0;Myr (<xref ref-type="bibr" rid="B186">Zhang&#xa0;et&#xa0;al., 2010</xref>).</p>
</sec>
<sec id="s4-4-2">
<title>4.4.2 Lunar orbit anomaly</title>
<p>The Moon&#x2019;s orbital distance is slowly increasing and the Earth&#x2019;s rotation rate is decreasing due to tidal forces transferring angular momentum from the Earth to the Moon. In order to investigate the Earth-Moon system, the Lunar Laser Ranging Experiment (LLR) from Apollo 11, 14, 15 and Lunokhod missions was performed to measure accurately the recession velocity of the Moon. The missions report the Moon&#x2019;s semimajor axis <italic>d</italic> &#x3d; 384, 402&#xa0;km, which increases at rate (<xref ref-type="bibr" rid="B41">Dickey&#xa0;et&#xa0;al., 1994</xref>) of (3.82 &#xb1; 0.08)&#xa0;cm/yr. This value is anomalously high and inconsistent with an expected lunar recession velocity due to tidal forces, which should be lower by 30&#x2013;45% (<xref ref-type="bibr" rid="B82">K&#x159;&#xed;&#x17e;ek, 2009</xref>; <xref ref-type="bibr" rid="B141">Riofrio, 2012</xref>; <xref ref-type="bibr" rid="B84">K&#x159;&#xed;&#x17e;ek and Somer, 2022</xref>). The observed lunar recession velocity would correspond to increasing Earth&#x2019;s rotation period at a rate of &#x2b;2.3&#xa0;ms per century, but only a rate of &#x2b;1.8&#xa0;ms per century is observed (<xref ref-type="bibr" rid="B162">Stephenson&#xa0;et&#xa0;al., 2016</xref>). In addition, numerical modelling of the orbital evolution under such tidal dissipation would imply the age of the lunar orbit to be 1.5 &#xd7; 10<sup>9</sup>&#xa0;years, instead of 4 &#xd7; 10<sup>9</sup>&#xa0;years suggested by observations (<xref ref-type="bibr" rid="B13">Bills and Ray, 1999</xref>). This discrepancy is known as the Lunar orbit anomaly and so far its origin is unclear.</p>
<p>If the expansion of the solar system is considered, the recession velocity of the Moon due to the expansion is 2.74&#xa0;cm/yr assuming distance of the Moon <italic>d</italic> &#x3d; 384, 402&#xa0;km and the Hubble parameter <italic>H</italic>
<sub>0</sub> &#x3d; 69.8&#xa0;kms<sup>&#x2212;1</sup>Mpc<sup>&#x2212;1</sup> (<xref ref-type="bibr" rid="B57">Freedman&#xa0;et&#xa0;al., 2019</xref>). Hence, the lunar recession velocity due to tides is reduced to 1.08&#xa0;cm/yr that is more realistic. If the tides were fully responsible for the slowing Earth&#x2019;s rotation at rate of &#x2b;1.8&#xa0;ms per century, the lunar recession velocity would be <inline-formula id="inf15">
<mml:math id="m50">
<mml:mo>&#x223c;</mml:mo>
<mml:mn>2.25</mml:mn>
<mml:mspace width="0.17em"/>
<mml:mi mathvariant="normal">c</mml:mi>
<mml:mi mathvariant="normal">m</mml:mi>
<mml:mo>/</mml:mo>
<mml:mi mathvariant="normal">y</mml:mi>
<mml:mi mathvariant="normal">r</mml:mi>
</mml:math>
</inline-formula>. However, this is an upper limit only, because also other processes can slow down the Earth&#x2019;s rotation, such as impacts of massive meteorites, large earthquakes, huge volcanic eruptions, and energy dissipation in the Earth&#x2019;s mantle and the outer Earth&#x2019;s core due to convection.</p>
</sec>
<sec id="s4-4-3">
<title>4.4.3 Other observations</title>
<p>The Hubble flow in the solar system is indicated by many other observations (<xref ref-type="bibr" rid="B85">K&#x159;&#xed;&#x17e;ek and Somer, 2015</xref>). Mars had to be much closer to the Sun in the past; it is dusty and icy at the present, but detailed images of the Martian surface reveal that it was formed by rivers in the period of 3&#x2013;4&#xa0;Gyr ago (<xref ref-type="bibr" rid="B26">Carr, 1995</xref>; <xref ref-type="bibr" rid="B34">Davis&#xa0;et&#xa0;al., 2016</xref>; <xref ref-type="bibr" rid="B148">Salese&#xa0;et&#xa0;al., 2020</xref>). Measurements of the Titan&#x2019;s orbital expansion rate by the Cassini spacecraft during ten close encounters of the Moon between 2006 and 2016 revealed that Titan rapidly migrates away from Saturn (<xref ref-type="bibr" rid="B89">Lainey&#xa0;et&#xa0;al., 2020</xref>). The Titan-Saturn mean distance is <italic>d</italic> &#x3d; 1,221, 870&#xa0;km and the Titan&#x2019;s recession velocity is 11.3&#xa0;cm/yr. The corresponding recession velocity due to the Hubble flow is 8.7&#xa0;cm/yr. If this velocity is subtracted, the anomaly disappears and the resultant rate of 2.6&#xa0;cm/yr produced by tidal forces becomes realistic. Also, the expansion of the solar system can explain the formation of Neptune and Kuiper belt, the existence of fast satellites of Mars, Jupiter, Uranus and Neptune that are below the stationary orbit, or the large orbital momentum of the Moon (<xref ref-type="bibr" rid="B85">K&#x159;&#xed;&#x17e;ek and Somer, 2015</xref>).</p>
</sec>
</sec>
</sec>
<sec id="s5">
<title>5 Discussion and conclusion</title>
<p>The presented theory and numerical modelling satisfactorily explain several severe tensions between the standard &#x39b;CDM model and observations.<list list-type="simple">
<list-item>
<p>&#x2022; The improved Newtonian equations derived for the CC metric predict an increasing radius of gravitational orbits of local systems. The rate of growth with cosmic time is (1 &#x2b; <italic>z</italic>)<sup>&#x2212;1</sup>. This applies to all local systems including galaxy clusters, galaxies, and planetary systems. The gravitational orbits are stationary in the comoving coordinates but non-stationary in the proper coordinates.</p>
</list-item>
<list-item>
<p>&#x2022; The existence of spirals in disk galaxies is a direct consequence of the space expansion and time dilation. The spirals are formed by the stellar mass and gas that remain fixed in them. The stellar mass and gas are continuously outflowed from the bulge-bar region into the spiral region. The spirals are detached from the bulge-bar region due to the space expansion.</p>
</list-item>
<list-item>
<p>&#x2022; Since the orbital velocity of particles is conserved and the radius of orbits gradually increases during the space expansion, the spiral galaxies display flat rotation curves.</p>
</list-item>
</list>
</p>
<p>The constant rotation velocity, the space expansion and time dilation are the primary factors forming the morphology of spirals. The time dilation is particularly important, because a slower rate of time in the past significantly helped to separate spirals from the bulge-bar domain. As shown in the numerical modelling, the morphology of spirals depends on the expansion history of the Universe, on the galaxy mass, galaxy age and size of the bulge. Obviously, the presented modelling is rather simple and definitely far from being complete. A detailed parametric study based on observations of various types of galaxies is necessary for drawing more specific conclusions about the galaxy dynamics.</p>
<p>The previous theoretical attempts to correctly explain the galaxy dynamics were unsuccessful for the following reasons: 1) The simplest attempts ignored the space expansion and assumed galaxies in the static Universe. Consequently, the GR effects related to the expansion of the Universe were neglected and stars moved along stationary orbits not evolving in time. 2) Theories, which considered the space expansion using the GR theory, applied an incorrect cosmological model defined by the FLRW metric. This metric erroneously assumes that time is invariant of the space expansion. This assumption has fatal consequences for dynamics of local systems. An additional radial acceleration originating in the space expansion is included in the Newtonian equations for orbiting bodies, but the proper angular momentum <italic>L</italic> &#x3d; <italic>RV</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> keeps constant. The constant <italic>L</italic> causes that the effect of the Hubble flow on the orbiting bodies is eliminated and the radius of the orbits is effectively insensitive to the space expansion.</p>
<p>By contrast, the proper angular momentum <italic>L</italic> &#x3d; <italic>RV</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> in the Newtonian equations derived under the CC metric is not constant but it increases with redshift. Consequently, the orbits are not stationary any more, but their radius increases with cosmic time. Since the velocity of orbiting massive particles does not depend on the space expansion and the radius of orbits is continuously increasing, the rotation curves are essentially flat. Importantly, the rotation curves are flat without assuming non-baryonic dark matter haloes surrounding galaxies. No dark matter is needed for explaining all basic properties of the galactic dynamics. Applying the CC metric to interpretations of the SNe Ia dimming reveals that also dark energy is unnecessary for getting fit with observations (<xref ref-type="bibr" rid="B8">Behnke&#xa0;et&#xa0;al., 2002</xref>; <xref ref-type="bibr" rid="B175">Vavry&#x10d;uk, 2022a</xref>). Hence, dark energy and dark matter are false and superfluous concepts originating in a wrong description of the space expansion, when the time dilation is ignored during the evolution of the Universe. Once a correct metric is applied, the cosmological model is consistent with observations with no need to introduce new unphysical concepts. A controversy of dark matter and dark energy concepts is evidenced also by many other observations (<xref ref-type="bibr" rid="B88">Kroupa, 2012</xref>; <xref ref-type="bibr" rid="B178">Weinberg&#xa0;et&#xa0;al., 2013</xref>; <xref ref-type="bibr" rid="B87">Kroupa, 2015</xref>; <xref ref-type="bibr" rid="B19">Buchert&#xa0;et&#xa0;al., 2016</xref>; <xref ref-type="bibr" rid="B21">Bull&#xa0;et&#xa0;al., 2016</xref>; <xref ref-type="bibr" rid="B80">Koyama, 2016</xref>; <xref ref-type="bibr" rid="B22">Bullock and Boylan-Kolchin, 2017</xref>; <xref ref-type="bibr" rid="B53">Ezquiaga and Zumalac&#xe1;rregui, 2017</xref>).</p>
<p>In addition, the presented theory resolves several other puzzles and paradoxes in cosmology. It explains the origin of spirals in a completely different way than proposed by the density-wave hypothesis. The spirals are not an effect of standing waves in the disk as so far believed (<xref ref-type="bibr" rid="B167">Toomre, 1977</xref>; <xref ref-type="bibr" rid="B42">Dobbs and Baba, 2014</xref>; <xref ref-type="bibr" rid="B158">Shu, 2016</xref>). Instead, they are objects formed by material remained fixed in spirals. Still, the winding problem is avoided. The theory also removes tensions related to the observed galaxy growth explained by major and/or minor mergers of galaxies. Since the hypothesis of mergers (<xref ref-type="bibr" rid="B124">Naab&#xa0;et&#xa0;al., 2009</xref>; <xref ref-type="bibr" rid="B79">Kormendy and Ho, 2013</xref>; <xref ref-type="bibr" rid="B114">McLure&#xa0;et&#xa0;al., 2013</xref>; <xref ref-type="bibr" rid="B28">Conselice, 2014</xref>) is refuted by observations of no evolution of the galaxy mass (<xref ref-type="bibr" rid="B23">Bundy&#xa0;et&#xa0;al., 2017</xref>; <xref ref-type="bibr" rid="B76">Kawinwanichakij&#xa0;et&#xa0;al., 2020</xref>), the problem of a galaxy growth is so far unsolved. The presented theory also resolves challenges to the &#x39b;CDM model such as the problem of faint satellite galaxies, the baryonic Tully-Fisher relation or the radial acceleration relation. Furthermore, numerous puzzles in the solar system are successfully explained such as the Faint young Sun paradox, the lunar orbit anomaly, the presence of rivers on ancient Mars, the Titan recession velocity anomaly, formation of the Kuiper belt and others (<xref ref-type="bibr" rid="B46">Dumin, 2015</xref>; <xref ref-type="bibr" rid="B83">K&#x159;&#xed;&#x17e;ek&#xa0;et&#xa0;al., 2015</xref>; <xref ref-type="bibr" rid="B85">K&#x159;&#xed;&#x17e;ek and Somer, 2015</xref>).</p>
</sec>
</body>
<back>
<sec sec-type="data-availability" id="s6">
<title>Data availability statement</title>
<p>The original contributions presented in the study are included in the article/supplementary material, further inquiries can be directed to the corresponding author.</p>
</sec>
<sec id="s7">
<title>Author contributions</title>
<p>VV is responsible for the whole study presented in the paper.</p>
</sec>
<sec id="s8">
<title>Funding</title>
<p>The Institute of Geophysics of the Czech Academy of Sciences supported this research.</p>
</sec>
<sec sec-type="COI-statement" id="s9">
<title>Conflict of interest</title>
<p>The author declares that the research was conducted in the absence of any commercial or financial relationships that could be construed as a potential conflict of interest.</p>
</sec>
<sec sec-type="disclaimer" id="s10">
<title>Publisher&#x2019;s note</title>
<p>All claims expressed in this article are solely those of the authors and do not necessarily represent those of their affiliated organizations, or those of the publisher, the editors and the reviewers. Any product that may be evaluated in this article, or claim that may be made by its manufacturer, is not guaranteed or endorsed by the publisher.</p>
</sec>
<ref-list>
<title>References</title>
<ref id="B1">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Anderson</surname>
<given-names>J. D.</given-names>
</name>
<name>
<surname>Laing</surname>
<given-names>P. A.</given-names>
</name>
<name>
<surname>Lau</surname>
<given-names>E. L.</given-names>
</name>
<name>
<surname>Liu</surname>
<given-names>A. S.</given-names>
</name>
<name>
<surname>Nieto</surname>
<given-names>M. M.</given-names>
</name>
<name>
<surname>Turyshev</surname>
<given-names>S. G.</given-names>
</name>
</person-group> (<year>1998</year>). <article-title>Indication, from Pioneer 10/11, Galileo, and Ulysses data, of an apparent anomalous, weak, long-range acceleration</article-title>. <source>Phys. Rev. Lett.</source> <volume>81</volume>, <fpage>2858</fpage>&#x2013;<lpage>2861</lpage>. <pub-id pub-id-type="doi">10.1103/PhysRevLett.81.2858</pub-id>
</citation>
</ref>
<ref id="B2">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Baba</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Asaki</surname>
<given-names>Y.</given-names>
</name>
<name>
<surname>Makino</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Miyoshi</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Saitoh</surname>
<given-names>T. R.</given-names>
</name>
<name>
<surname>Wada</surname>
<given-names>K.</given-names>
</name>
</person-group> (<year>2009</year>). <article-title>The origin of large peculiar motions of star-forming regions and spiral structures of our galaxy</article-title>. <source>ApJ</source> <volume>706</volume>, <fpage>471</fpage>&#x2013;<lpage>481</lpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/706/1/471</pub-id>
</citation>
</ref>
<ref id="B3">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Baba</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Saitoh</surname>
<given-names>T. R.</given-names>
</name>
<name>
<surname>Wada</surname>
<given-names>K.</given-names>
</name>
</person-group> (<year>2013</year>). <article-title>Dynamics of non-steady spiral arms in disk galaxies</article-title>. <source>ApJ</source> <volume>763</volume>, <fpage>46</fpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/763/1/46</pub-id>
</citation>
</ref>
<ref id="B4">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bahcall</surname>
<given-names>J. N.</given-names>
</name>
<name>
<surname>Pinsonneault</surname>
<given-names>M. H.</given-names>
</name>
<name>
<surname>Basu</surname>
<given-names>S.</given-names>
</name>
</person-group> (<year>2001</year>). <article-title>Solar models: Current epoch and time dependences, neutrinos, and helioseismological properties</article-title>. <source>ApJ</source> <volume>555</volume>, <fpage>990</fpage>&#x2013;<lpage>1012</lpage>. <pub-id pub-id-type="doi">10.1086/321493</pub-id>
</citation>
</ref>
<ref id="B5">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Begeman</surname>
<given-names>K. G.</given-names>
</name>
<name>
<surname>Broeils</surname>
<given-names>A. H.</given-names>
</name>
<name>
<surname>Sanders</surname>
<given-names>R. H.</given-names>
</name>
</person-group> (<year>1991</year>). <article-title>Extended rotation curves of spiral galaxies: Dark haloes and modified dynamics</article-title>. <source>MNRAS</source> <volume>249</volume>, <fpage>523</fpage>&#x2013;<lpage>537</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/249.3.523</pub-id>
</citation>
</ref>
<ref id="B6">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Begeman</surname>
<given-names>K. G.</given-names>
</name>
</person-group> (<year>1987</year>). <source>HI rotation curves of spiral galaxies</source>. <comment>Ph.D. thesis</comment>. <publisher-loc>Groningen</publisher-loc>: <publisher-name>University of Groningen, Kapteyn Astronomical Institute</publisher-name>.</citation>
</ref>
<ref id="B7">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Begeman</surname>
<given-names>K. G.</given-names>
</name>
</person-group> (<year>1989</year>). <article-title>HI rotation curves of spiral galaxies. I. NGC 3198</article-title>. <source>Astron. Astrophys.</source> <volume>223</volume>, <fpage>47</fpage>&#x2013;<lpage>60</lpage>.</citation>
</ref>
<ref id="B8">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Behnke</surname>
<given-names>D.</given-names>
</name>
<name>
<surname>Blaschke</surname>
<given-names>D. B.</given-names>
</name>
<name>
<surname>Pervushin</surname>
<given-names>V. N.</given-names>
</name>
<name>
<surname>Proskurin</surname>
<given-names>D.</given-names>
</name>
</person-group> (<year>2002</year>). <article-title>Description of supernova data in conformal cosmology without cosmological constant</article-title>. <source>Phys. Lett. B</source> <volume>530</volume>, <fpage>20</fpage>&#x2013;<lpage>26</lpage>. <pub-id pub-id-type="doi">10.1016/S0370-2693(02)01341-2</pub-id>
</citation>
</ref>
<ref id="B9">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bekenstein</surname>
<given-names>J. D.</given-names>
</name>
</person-group> (<year>2004</year>). <article-title>Relativistic gravitation theory for the modified Newtonian dynamics paradigm</article-title>. <source>Phys. Rev. D.</source> <volume>70</volume>, <fpage>083509</fpage>. <pub-id pub-id-type="doi">10.1103/PhysRevD.70.083509</pub-id>
</citation>
</ref>
<ref id="B10">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bergstr&#xf6;m</surname>
<given-names>L.</given-names>
</name>
</person-group> (<year>2000</year>). <article-title>Non-baryonic dark matter: Observational evidence and detection methods</article-title>. <source>Rep. Prog. Phys.</source> <volume>63</volume>, <fpage>793</fpage>&#x2013;<lpage>841</lpage>. <pub-id pub-id-type="doi">10.1088/0034-4885/63/5/2r3</pub-id>
</citation>
</ref>
<ref id="B11">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bertone</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Hooper</surname>
<given-names>D.</given-names>
</name>
</person-group> (<year>2018</year>). <article-title>History of dark matter</article-title>. <source>Rev. Mod. Phys.</source> <volume>90</volume>, <fpage>045002</fpage>. <pub-id pub-id-type="doi">10.1103/RevModPhys.90.045002</pub-id>
</citation>
</ref>
<ref id="B12">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bertotti</surname>
<given-names>B.</given-names>
</name>
<name>
<surname>Farinella</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Vokrouhlick</surname>
<given-names>D.</given-names>
</name>
</person-group> (<year>2003</year>). <article-title>Physics of the solar system - dynamics and evolution, space physics, and spacetime structure</article-title>. <source>Astrophysics and Space Science Library</source>.<volume>293</volume>. <pub-id pub-id-type="doi">10.1007/978-94-010-0233-2</pub-id>
</citation>
</ref>
<ref id="B13">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bills</surname>
<given-names>B. G.</given-names>
</name>
<name>
<surname>Ray</surname>
<given-names>R. D.</given-names>
</name>
</person-group> (<year>1999</year>). <article-title>Lunar orbital evolution: A synthesis of recent results</article-title>. <source>Geophys. Res. Lett.</source> <volume>26</volume>, <fpage>3045</fpage>&#x2013;<lpage>3048</lpage>. <pub-id pub-id-type="doi">10.1029/1999GL008348</pub-id>
</citation>
</ref>
<ref id="B14">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Binney</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Gerhard</surname>
<given-names>O.</given-names>
</name>
<name>
<surname>Spergel</surname>
<given-names>D.</given-names>
</name>
</person-group> (<year>1997</year>). <article-title>The photometric structure of the inner Galaxy</article-title>. <source>MNRAS</source> <volume>288</volume>, <fpage>365</fpage>&#x2013;<lpage>374</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/288.2.365</pub-id>
</citation>
</ref>
<ref id="B15">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bissantz</surname>
<given-names>N.</given-names>
</name>
<name>
<surname>Gerhard</surname>
<given-names>O.</given-names>
</name>
</person-group> (<year>2002</year>). <article-title>Spiral arms, bar shape and bulge microlensing in the Milky Way</article-title>. <source>MNRAS</source> <volume>330</volume>, <fpage>591</fpage>&#x2013;<lpage>608</lpage>. <pub-id pub-id-type="doi">10.1046/j.1365-8711.2002.05116.x</pub-id>
</citation>
</ref>
<ref id="B16">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bolen</surname>
<given-names>B.</given-names>
</name>
<name>
<surname>Bombelli</surname>
<given-names>L.</given-names>
</name>
<name>
<surname>Puzio</surname>
<given-names>R.</given-names>
</name>
</person-group> (<year>2001</year>). <article-title>Expansion-induced contribution to the precession of binary orbits</article-title>. <source>Class. Quantum Gravity</source> <volume>18</volume>, <fpage>1173</fpage>&#x2013;<lpage>1178</lpage>. <pub-id pub-id-type="doi">10.1088/0264-9381/18/7/302</pub-id>
</citation>
</ref>
<ref id="B17">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bournaud</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>Jog</surname>
<given-names>C. J.</given-names>
</name>
<name>
<surname>Combes</surname>
<given-names>F.</given-names>
</name>
</person-group> (<year>2007</year>). <article-title>Multiple minor mergers: Formation of elliptical galaxies and constraints for the growth of spiral disks</article-title>. <source>Astron. Astrophys.</source> <volume>476</volume>, <fpage>1179</fpage>&#x2013;<lpage>1190</lpage>. <pub-id pub-id-type="doi">10.1051/0004-6361:20078010</pub-id>
</citation>
</ref>
<ref id="B18">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bouwens</surname>
<given-names>R. J.</given-names>
</name>
<name>
<surname>Illingworth</surname>
<given-names>G. D.</given-names>
</name>
<name>
<surname>Blakeslee</surname>
<given-names>J. P.</given-names>
</name>
<name>
<surname>Broadhurst</surname>
<given-names>T. J.</given-names>
</name>
<name>
<surname>Franx</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2004</year>). <article-title>Galaxy size evolution at high redshift and surface brightness selection effects: Constraints from the Hubble ultra deep field</article-title>. <source>ApJ</source> <volume>611</volume>, <fpage>L1</fpage>&#x2013;<lpage>L4</lpage>. <pub-id pub-id-type="doi">10.1086/423786</pub-id>
</citation>
</ref>
<ref id="B19">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Buchert</surname>
<given-names>T.</given-names>
</name>
<name>
<surname>Coley</surname>
<given-names>A. A.</given-names>
</name>
<name>
<surname>Kleinert</surname>
<given-names>H.</given-names>
</name>
<name>
<surname>Roukema</surname>
<given-names>B. F.</given-names>
</name>
<name>
<surname>Wiltshire</surname>
<given-names>D. L.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>Observational challenges for the standard FLRW model</article-title>. <source>Int. J. Mod. Phys. D</source> <volume>25</volume>, <fpage>1630007</fpage>&#x2013;<lpage>1630244</lpage>. <pub-id pub-id-type="doi">10.1142/S021827181630007X</pub-id>
</citation>
</ref>
<ref id="B20">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bugg</surname>
<given-names>D. V.</given-names>
</name>
</person-group> (<year>2015</year>). <article-title>Mond &#x2014; a review</article-title>. <source>Can. J. Phys.</source> <volume>93</volume>, <fpage>119</fpage>&#x2013;<lpage>125</lpage>. <pub-id pub-id-type="doi">10.1139/cjp-2014-0057</pub-id>
</citation>
</ref>
<ref id="B21">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bull</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Akrami</surname>
<given-names>Y.</given-names>
</name>
<name>
<surname>Adamek</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Baker</surname>
<given-names>T.</given-names>
</name>
<name>
<surname>Bellini</surname>
<given-names>E.</given-names>
</name>
<name>
<surname>Beltr&#xe1;n Jim&#xe9;nez</surname>
<given-names>J.</given-names>
</name>
<etal/>
</person-group> (<year>2016</year>). <article-title>Beyond &#x39b;CDM: Problems, solutions, and the road ahead</article-title>. <source>Phys. Dark Universe</source> <volume>12</volume>, <fpage>56</fpage>&#x2013;<lpage>99</lpage>. <pub-id pub-id-type="doi">10.1016/j.dark.2016.02.001</pub-id>
</citation>
</ref>
<ref id="B22">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bullock</surname>
<given-names>J. S.</given-names>
</name>
<name>
<surname>Boylan-Kolchin</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2017</year>). <article-title>Small-scale challenges to the &#x39b;CDM paradigm</article-title>. <source>Annu. Rev. Astronomy Astrophysics</source> <volume>55</volume>, <fpage>343</fpage>&#x2013;<lpage>387</lpage>. <pub-id pub-id-type="doi">10.1146/annurev-astro-091916-055313</pub-id>
</citation>
</ref>
<ref id="B23">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Bundy</surname>
<given-names>K.</given-names>
</name>
<name>
<surname>Leauthaud</surname>
<given-names>A.</given-names>
</name>
<name>
<surname>Saito</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>Maraston</surname>
<given-names>C.</given-names>
</name>
<name>
<surname>Wake</surname>
<given-names>D. A.</given-names>
</name>
<name>
<surname>Thomas</surname>
<given-names>D.</given-names>
</name>
</person-group> (<year>2017</year>). <article-title>The Stripe 82 Massive Galaxy Project. III. A lack of growth among massive galaxies</article-title>. <source>ApJ</source> <volume>851</volume>, <fpage>34</fpage>. <pub-id pub-id-type="doi">10.3847/1538-4357/aa9896</pub-id>
</citation>
</ref>
<ref id="B24">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Callan</surname>
<given-names>C.</given-names>
</name>
<name>
<surname>Dicke</surname>
<given-names>R. H.</given-names>
</name>
<name>
<surname>Peebles</surname>
<given-names>P. J. E.</given-names>
</name>
</person-group> (<year>1965</year>). <article-title>Cosmology and Newtonian mechanics</article-title>. <source>Am. J. Phys.</source> <volume>33</volume>, <fpage>105</fpage>&#x2013;<lpage>108</lpage>. <pub-id pub-id-type="doi">10.1119/1.1971256</pub-id>
</citation>
</ref>
<ref id="B25">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Calzetti</surname>
<given-names>D.</given-names>
</name>
<name>
<surname>Armus</surname>
<given-names>L.</given-names>
</name>
<name>
<surname>Bohlin</surname>
<given-names>R. C.</given-names>
</name>
<name>
<surname>Kinney</surname>
<given-names>A. L.</given-names>
</name>
<name>
<surname>Koornneef</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Storchi-Bergmann</surname>
<given-names>T.</given-names>
</name>
</person-group> (<year>2000</year>). <article-title>The dust content and opacity of actively star-forming galaxies</article-title>. <source>ApJ</source> <volume>533</volume>, <fpage>682</fpage>&#x2013;<lpage>695</lpage>. <pub-id pub-id-type="doi">10.1086/308692</pub-id>
</citation>
</ref>
<ref id="B26">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Carr</surname>
<given-names>M. H.</given-names>
</name>
</person-group> (<year>1995</year>). <article-title>The Martian drainage system and the origin of valley networks and fretted channels</article-title>. <source>J. Geophys. Res.</source> <volume>100</volume>, <fpage>7479</fpage>&#x2013;<lpage>7508</lpage>. <pub-id pub-id-type="doi">10.1029/95JE00260</pub-id>
</citation>
</ref>
<ref id="B27">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Carrera</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Giulini</surname>
<given-names>D.</given-names>
</name>
</person-group> (<year>2010</year>). <article-title>Influence of global cosmological expansion on local dynamics and kinematics</article-title>. <source>Rev. Mod. Phys.</source> <volume>82</volume>, <fpage>169</fpage>&#x2013;<lpage>208</lpage>. <pub-id pub-id-type="doi">10.1103/RevModPhys.82.169</pub-id>
</citation>
</ref>
<ref id="B28">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Conselice</surname>
<given-names>C. J.</given-names>
</name>
</person-group> (<year>2014</year>). <article-title>The evolution of galaxy structure over cosmic time</article-title>. <source>Annu. Rev. Astron. Astrophys.</source> <volume>52</volume>, <fpage>291</fpage>&#x2013;<lpage>337</lpage>. <pub-id pub-id-type="doi">10.1146/annurev-astro-081913-040037</pub-id>
</citation>
</ref>
<ref id="B29">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Cooperstock</surname>
<given-names>F. I.</given-names>
</name>
<name>
<surname>Faraoni</surname>
<given-names>V.</given-names>
</name>
<name>
<surname>Vollick</surname>
<given-names>D. N.</given-names>
</name>
</person-group> (<year>1998</year>). <article-title>The influence of the cosmological expansion on local systems</article-title>. <source>ApJ</source> <volume>503</volume>, <fpage>61</fpage>&#x2013;<lpage>66</lpage>. <pub-id pub-id-type="doi">10.1086/305956</pub-id>
</citation>
</ref>
<ref id="B30">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Corda</surname>
<given-names>C.</given-names>
</name>
</person-group> (<year>2009</year>). <article-title>Interferometric detection of gravitational waves: The definitive test for General Relativity</article-title>. <source>Int. J. Mod. Phys. D</source> <volume>18</volume>, <fpage>2275</fpage>&#x2013;<lpage>2282</lpage>. <pub-id pub-id-type="doi">10.1142/S0218271809015904</pub-id>
</citation>
</ref>
<ref id="B31">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>da Cunha</surname>
<given-names>E.</given-names>
</name>
<name>
<surname>Charlot</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>Elbaz</surname>
<given-names>D.</given-names>
</name>
</person-group> (<year>2008</year>). <article-title>A simple model to interpret the ultraviolet, optical and infrared emission from galaxies</article-title>. <source>MNRAS</source> <volume>388</volume>, <fpage>1595</fpage>&#x2013;<lpage>1617</lpage>. <pub-id pub-id-type="doi">10.1111/j.1365-2966.2008.13535.x</pub-id>
</citation>
</ref>
<ref id="B32">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Dabrowski</surname>
<given-names>M. P.</given-names>
</name>
<name>
<surname>Garecki</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Blaschke</surname>
<given-names>D. B.</given-names>
</name>
</person-group> (<year>2009</year>). <article-title>Conformal transformations and conformal invariance in gravitation</article-title>. <source>Ann. Phys.</source> <volume>521</volume>, <fpage>13</fpage>&#x2013;<lpage>32</lpage>. <pub-id pub-id-type="doi">10.1002/andp.20095210105</pub-id>
</citation>
</ref>
<ref id="B33">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Dahlen</surname>
<given-names>T.</given-names>
</name>
<name>
<surname>Mobasher</surname>
<given-names>B.</given-names>
</name>
<name>
<surname>Dickinson</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Ferguson</surname>
<given-names>H. C.</given-names>
</name>
<name>
<surname>Giavalisco</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Kretchmer</surname>
<given-names>C.</given-names>
</name>
<etal/>
</person-group> (<year>2007</year>). <article-title>Evolution of the luminosity function, star formation rate, morphology, and size of star-forming galaxies selected at rest-frame 1500 and 2800 &#xc5;</article-title>. <source>ApJ</source> <volume>654</volume>, <fpage>172</fpage>&#x2013;<lpage>185</lpage>. <pub-id pub-id-type="doi">10.1086/508854</pub-id>
</citation>
</ref>
<ref id="B34">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Davis</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Balme</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Grindrod</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Williams</surname>
<given-names>R.</given-names>
</name>
<name>
<surname>Gupta</surname>
<given-names>S.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>Extensive Noachian fluvial systems in Arabia Terra: Implications for early Martian climate</article-title>. <source>Geology</source> <volume>44</volume>, <fpage>847</fpage>&#x2013;<lpage>850</lpage>. <pub-id pub-id-type="doi">10.1130/G38247.1</pub-id>
</citation>
</ref>
<ref id="B35">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Davis</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Efstathiou</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Frenk</surname>
<given-names>C. S.</given-names>
</name>
<name>
<surname>White</surname>
<given-names>S. D. M.</given-names>
</name>
</person-group> (<year>1985</year>). <article-title>The evolution of large-scale structure in a universe dominated by cold dark matter</article-title>. <source>ApJ</source> <volume>292</volume>, <fpage>371</fpage>&#x2013;<lpage>394</lpage>. <pub-id pub-id-type="doi">10.1086/163168</pub-id>
</citation>
</ref>
<ref id="B36">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>de Blok</surname>
<given-names>W. J. G.</given-names>
</name>
<name>
<surname>Walter</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>Brinks</surname>
<given-names>E.</given-names>
</name>
<name>
<surname>Trachternach</surname>
<given-names>C.</given-names>
</name>
<name>
<surname>Oh</surname>
<given-names>S. H.</given-names>
</name>
<name>
<surname>Kennicutt</surname>
<given-names>J. R. C.</given-names>
</name>
</person-group> (<year>2008</year>). <article-title>High-resolution rotation curves and galaxy mass models from THINGS</article-title>. <source>AJ</source> <volume>136</volume>, <fpage>2648</fpage>&#x2013;<lpage>2719</lpage>. <pub-id pub-id-type="doi">10.1088/0004-6256/136/6/2648</pub-id>
</citation>
</ref>
<ref id="B37">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>de Blok</surname>
<given-names>W. J. G.</given-names>
</name>
<name>
<surname>Bosma</surname>
<given-names>A.</given-names>
</name>
</person-group> (<year>2002</year>). <article-title>High-resolution rotation curves of low surface brightness galaxies</article-title>. <source>Astron. Astrophys.</source> <volume>385</volume>, <fpage>816</fpage>&#x2013;<lpage>846</lpage>. <pub-id pub-id-type="doi">10.1051/0004-6361:20020080</pub-id>
</citation>
</ref>
<ref id="B38">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>de Blok</surname>
<given-names>W. J. G.</given-names>
</name>
<name>
<surname>McGaugh</surname>
<given-names>S. S.</given-names>
</name>
<name>
<surname>Rubin</surname>
<given-names>V. C.</given-names>
</name>
</person-group> (<year>2001</year>). <article-title>High-resolution rotation curves of low surface brightness galaxies. II. Mass models</article-title>. <source>AJ</source> <volume>122</volume>, <fpage>2396</fpage>&#x2013;<lpage>2427</lpage>. <pub-id pub-id-type="doi">10.1086/323450</pub-id>
</citation>
</ref>
<ref id="B39">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Del Popolo</surname>
<given-names>A.</given-names>
</name>
<name>
<surname>Le Delliou</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2017</year>). <article-title>Small scale problems of the &#x39b;CDM model: A short review</article-title>. <source>Galaxies</source> <volume>5</volume>, <fpage>17</fpage>. <pub-id pub-id-type="doi">10.3390/galaxies5010017</pub-id>
</citation>
</ref>
<ref id="B40">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Dicke</surname>
<given-names>R. H.</given-names>
</name>
<name>
<surname>Peebles</surname>
<given-names>P. J.</given-names>
</name>
</person-group> (<year>1964</year>). <article-title>Evolution of the solar system and the expansion of the universe</article-title>. <source>Phys. Rev. Lett.</source> <volume>12</volume>, <fpage>435</fpage>&#x2013;<lpage>437</lpage>. <pub-id pub-id-type="doi">10.1103/PhysRevLett.12.435</pub-id>
</citation>
</ref>
<ref id="B41">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Dickey</surname>
<given-names>J. O.</given-names>
</name>
<name>
<surname>Bender</surname>
<given-names>P. L.</given-names>
</name>
<name>
<surname>Faller</surname>
<given-names>J. E.</given-names>
</name>
<name>
<surname>Newhall</surname>
<given-names>X. X.</given-names>
</name>
<name>
<surname>Ricklefs</surname>
<given-names>R. L.</given-names>
</name>
<name>
<surname>Ries</surname>
<given-names>J. G.</given-names>
</name>
<etal/>
</person-group> (<year>1994</year>). <article-title>Lunar laser ranging: A continuing legacy of the Apollo program</article-title>. <source>Science</source> <volume>265</volume>, <fpage>482</fpage>&#x2013;<lpage>490</lpage>. <pub-id pub-id-type="doi">10.1126/science.265.5171.482</pub-id>
</citation>
</ref>
<ref id="B42">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Dobbs</surname>
<given-names>C.</given-names>
</name>
<name>
<surname>Baba</surname>
<given-names>J.</given-names>
</name>
</person-group> (<year>2014</year>). <article-title>Dawes review 4: Spiral structures in disc galaxies</article-title>. <source>Publ. Astron. Soc. Aust.</source>, <volume>31</volume>, <fpage>e035</fpage>. <pub-id pub-id-type="doi">10.1017/pasa.2014.31</pub-id>
</citation>
</ref>
<ref id="B43">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Draine</surname>
<given-names>B. T.</given-names>
</name>
<name>
<surname>Li</surname>
<given-names>A.</given-names>
</name>
</person-group> (<year>2007</year>). <article-title>Infrared emission from interstellar dust. IV. The silicate-graphite-PAH model in the Post-Spitzer era</article-title>. <source>ApJ</source> <volume>657</volume>, <fpage>810</fpage>&#x2013;<lpage>837</lpage>. <pub-id pub-id-type="doi">10.1086/511055</pub-id>
</citation>
</ref>
<ref id="B44">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Dubinski</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Carlberg</surname>
<given-names>R. G.</given-names>
</name>
</person-group> (<year>1991</year>). <article-title>The structure of cold dark matter halos</article-title>. <source>ApJ</source> <volume>378</volume>, <fpage>496</fpage>. <pub-id pub-id-type="doi">10.1086/170451</pub-id>
</citation>
</ref>
<ref id="B45">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Duc</surname>
<given-names>P. A.</given-names>
</name>
<name>
<surname>Paudel</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>McDermid</surname>
<given-names>R. M.</given-names>
</name>
<name>
<surname>Cuillandre</surname>
<given-names>J. C.</given-names>
</name>
<name>
<surname>Serra</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Bournaud</surname>
<given-names>F.</given-names>
</name>
<etal/>
</person-group> (<year>2014</year>). <article-title>Identification of old tidal dwarfs near early-type galaxies from deep imaging and H I observations</article-title>. <source>MNRAS</source> <volume>440</volume>, <fpage>1458</fpage>&#x2013;<lpage>1469</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/stu330</pub-id>
</citation>
</ref>
<ref id="B46">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Dumin</surname>
<given-names>Y. V.</given-names>
</name>
</person-group> (<year>2015</year>). <article-title>The faint young Sun paradox in the context of modern cosmology</article-title>. <source>Astron. Tsirkulyar</source> <volume>1623</volume>, <fpage>1</fpage>&#x2013;<lpage>5</lpage>.</citation>
</ref>
<ref id="B47">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Dunne</surname>
<given-names>L.</given-names>
</name>
<name>
<surname>Eales</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>Edmunds</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Ivison</surname>
<given-names>R.</given-names>
</name>
<name>
<surname>Alexander</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Clements</surname>
<given-names>D. L.</given-names>
</name>
</person-group> (<year>2000</year>). <article-title>The SCUBA Local Universe Galaxy Survey - I. First measurements of the submillimetre luminosity and dust mass functions</article-title>. <source>MNRAS</source> <volume>315</volume>, <fpage>115</fpage>&#x2013;<lpage>139</lpage>. <pub-id pub-id-type="doi">10.1046/j.1365-8711.2000.03386.x</pub-id>
</citation>
</ref>
<ref id="B48">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Einstein</surname>
<given-names>A.</given-names>
</name>
</person-group> (<year>1920</year>). &#x201c;<article-title>Relativity, the special and the general theory</article-title>,&#x201d; in <source>Authorized translation by</source>. Editor <person-group person-group-type="editor">
<name>
<surname>Robert</surname>
<given-names>W. L.</given-names>
</name>
</person-group> (<publisher-name>Henry Holt and Company</publisher-name>), <fpage>168</fpage>.</citation>
</ref>
<ref id="B49">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Einstein</surname>
<given-names>A.</given-names>
</name>
<name>
<surname>Straus</surname>
<given-names>E. G.</given-names>
</name>
</person-group> (<year>1945</year>). <article-title>The influence of the expansion of space on the gravitation fields surrounding the individual stars</article-title>. <source>Rev. Mod. Phys.</source> <volume>17</volume>, <fpage>120</fpage>&#x2013;<lpage>124</lpage>. <pub-id pub-id-type="doi">10.1103/RevModPhys.17.120</pub-id>
</citation>
</ref>
<ref id="B50">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Elmegreen</surname>
<given-names>D. M.</given-names>
</name>
<name>
<surname>Chromey</surname>
<given-names>F. R.</given-names>
</name>
<name>
<surname>Bissell</surname>
<given-names>B. A.</given-names>
</name>
<name>
<surname>Corrado</surname>
<given-names>K.</given-names>
</name>
</person-group> (<year>1999</year>). <article-title>
<italic>K</italic>&#x2032;-Band observations of underlying symmetric structure in flocculent galaxies</article-title>. <source>AJ</source> <volume>118</volume>, <fpage>2618</fpage>&#x2013;<lpage>2624</lpage>. <pub-id pub-id-type="doi">10.1086/301127</pub-id>
</citation>
</ref>
<ref id="B51">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Endean</surname>
<given-names>G.</given-names>
</name>
</person-group> (<year>1997</year>). <article-title>Cosmology in conformally flat spacetime</article-title>. <source>ApJ</source> <volume>479</volume>, <fpage>40</fpage>&#x2013;<lpage>45</lpage>. <pub-id pub-id-type="doi">10.1086/303862</pub-id>
</citation>
</ref>
<ref id="B52">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Endean</surname>
<given-names>G.</given-names>
</name>
</person-group> (<year>1994</year>). <article-title>Redshift and the Hubble constant in conformally flat spacetime</article-title>. <source>ApJ</source> <volume>434</volume>, <fpage>397</fpage>. <pub-id pub-id-type="doi">10.1086/174741</pub-id>
</citation>
</ref>
<ref id="B53">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Ezquiaga</surname>
<given-names>J. M.</given-names>
</name>
<name>
<surname>Zumalac&#xe1;rregui</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2017</year>). <article-title>Dark energy after GW170817: Dead ends and the road ahead</article-title>. <source>Phys. Rev. Lett.</source> <volume>119</volume>, <fpage>251304</fpage>. <pub-id pub-id-type="doi">10.1103/PhysRevLett.119.251304</pub-id>
</citation>
</ref>
<ref id="B54">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Faraoni</surname>
<given-names>V.</given-names>
</name>
<name>
<surname>Jacques</surname>
<given-names>A.</given-names>
</name>
</person-group> (<year>2007</year>). <article-title>Cosmological expansion and local physics</article-title>. <source>Phys. Rev. D.</source> <volume>76</volume>, <fpage>063510</fpage>. <pub-id pub-id-type="doi">10.1103/PhysRevD.76.063510</pub-id>
</citation>
</ref>
<ref id="B55">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Ferreras</surname>
<given-names>I.</given-names>
</name>
</person-group> (<year>2019</year>). <source>Fundamentals of galaxy dynamics</source>. <publisher-loc>London</publisher-loc>: <publisher-name>Formation and Evolution (UCL Press)</publisher-name>.</citation>
</ref>
<ref id="B56">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Freedman</surname>
<given-names>W. L.</given-names>
</name>
<name>
<surname>Madore</surname>
<given-names>B. F.</given-names>
</name>
<name>
<surname>Gibson</surname>
<given-names>B. K.</given-names>
</name>
<name>
<surname>Ferrarese</surname>
<given-names>L.</given-names>
</name>
<name>
<surname>Kelson</surname>
<given-names>D. D.</given-names>
</name>
<name>
<surname>Sakai</surname>
<given-names>S.</given-names>
</name>
<etal/>
</person-group> (<year>2001</year>). <article-title>Final results from the Hubble space telescope key project to measure the Hubble constant</article-title>. <source>ApJ</source> <volume>553</volume>, <fpage>47</fpage>&#x2013;<lpage>72</lpage>. <pub-id pub-id-type="doi">10.1086/320638</pub-id>
</citation>
</ref>
<ref id="B57">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Freedman</surname>
<given-names>W. L.</given-names>
</name>
<name>
<surname>Madore</surname>
<given-names>B. F.</given-names>
</name>
<name>
<surname>Hatt</surname>
<given-names>D.</given-names>
</name>
<name>
<surname>Hoyt</surname>
<given-names>T. J.</given-names>
</name>
<name>
<surname>Jang</surname>
<given-names>I. S.</given-names>
</name>
<name>
<surname>Beaton</surname>
<given-names>R. L.</given-names>
</name>
<etal/>
</person-group> (<year>2019</year>). <article-title>The Carnegie-Chicago Hubble program. VIII. An independent determination of the Hubble constant based on the tip of the red giant branch</article-title>. <source>ApJ</source> <volume>882</volume>, <fpage>34</fpage>. <pub-id pub-id-type="doi">10.3847/1538-4357/ab2f73</pub-id>
</citation>
</ref>
<ref id="B58">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Friedmann</surname>
<given-names>A.</given-names>
</name>
</person-group> (<year>1922</year>). <article-title>&#xdc;ber die Kr&#xfc;mmung des Raumes</article-title>. <source>Z. f&#xfc;r Phys.</source> <volume>10</volume>, <fpage>377</fpage>&#x2013;<lpage>386</lpage>. <pub-id pub-id-type="doi">10.1007/BF01332580</pub-id>
</citation>
</ref>
<ref id="B59">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Galianni</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Patat</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>Higdon</surname>
<given-names>J. L.</given-names>
</name>
<name>
<surname>Mieske</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>Kroupa</surname>
<given-names>P.</given-names>
</name>
</person-group> (<year>2010</year>). <article-title>VLT observations of NGC 1097&#x2019;s &#x201c;dog-leg&#x201d; tidal stream. Dwarf spheroidals and tidal streams</article-title>. <source>Astron. Astrophys.</source> <volume>521</volume>, <fpage>A20</fpage>. <pub-id pub-id-type="doi">10.1051/0004-6361/200913518</pub-id>
</citation>
</ref>
<ref id="B60">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Goldhaber</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Deustua</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>Gabi</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>Groom</surname>
<given-names>D.</given-names>
</name>
<name>
<surname>Hook</surname>
<given-names>I.</given-names>
</name>
<name>
<surname>Kim</surname>
<given-names>A.</given-names>
</name>
<etal/>
</person-group> (<year>1997</year>). &#x201c;<article-title>Observation of cosmological time dilation using Type Ia supernovae as clocks</article-title>,&#x201d; in <source>Thermonuclear supernovae</source>. Editors <person-group person-group-type="editor">
<name>
<surname>Ruiz-Lapuente</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Canal</surname>
<given-names>R.</given-names>
</name>
<name>
<surname>Isern</surname>
<given-names>J.</given-names>
</name>
</person-group> (<publisher-loc>Dordrecht</publisher-loc>: <publisher-name>Springer</publisher-name>), <volume>486</volume>, <fpage>777</fpage>. <pub-id pub-id-type="doi">10.1007/978-94-011-5710-0_48</pub-id>
</citation>
</ref>
<ref id="B61">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Goldhaber</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Groom</surname>
<given-names>D. E.</given-names>
</name>
<name>
<surname>Kim</surname>
<given-names>A.</given-names>
</name>
<name>
<surname>Aldering</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Astier</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Conley</surname>
<given-names>A.</given-names>
</name>
<etal/>
</person-group> (<year>2001</year>). <article-title>Timescale stretch parameterization of type Ia supernova B-band light curves</article-title>. <source>ApJ</source> <volume>558</volume>, <fpage>359</fpage>&#x2013;<lpage>368</lpage>. <pub-id pub-id-type="doi">10.1086/322460</pub-id>
</citation>
</ref>
<ref id="B62">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Goobar</surname>
<given-names>A.</given-names>
</name>
<name>
<surname>Leibundgut</surname>
<given-names>B.</given-names>
</name>
</person-group> (<year>2011</year>). <article-title>Supernova cosmology: Legacy and future</article-title>. <source>Annu. Rev. Nucl. Part. Sci.</source> <volume>61</volume>, <fpage>251</fpage>&#x2013;<lpage>279</lpage>. <pub-id pub-id-type="doi">10.1146/annurev-nucl-102010-130434</pub-id>
</citation>
</ref>
<ref id="B63">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Goode</surname>
<given-names>P. R.</given-names>
</name>
<name>
<surname>Qiu</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Yurchyshyn</surname>
<given-names>V.</given-names>
</name>
<name>
<surname>Hickey</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Chu</surname>
<given-names>M. C.</given-names>
</name>
<name>
<surname>Kolbe</surname>
<given-names>E.</given-names>
</name>
<etal/>
</person-group> (<year>2001</year>). <article-title>Earthshine observations of the Earth&#x2019;s reflectance</article-title>. <source>Geophys. Res. Lett.</source> <volume>28</volume>, <fpage>1671</fpage>&#x2013;<lpage>1674</lpage>. <pub-id pub-id-type="doi">10.1029/2000GL012580</pub-id>
</citation>
</ref>
<ref id="B64">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Gr&#xf8;n</surname>
<given-names>&#xd8;.</given-names>
</name>
<name>
<surname>Johannesen</surname>
<given-names>S.</given-names>
</name>
</person-group> (<year>2011</year>). <article-title>FRW universe models in conformally flat-spacetime coordinates I: General formalism</article-title>. <source>Eur. Phys. J. Plus</source> <volume>126</volume>, <fpage>28</fpage>. <pub-id pub-id-type="doi">10.1140/epjp/i2011-11028-6</pub-id>
</citation>
</ref>
<ref id="B65">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Harada</surname>
<given-names>T.</given-names>
</name>
<name>
<surname>Carr</surname>
<given-names>B. J.</given-names>
</name>
<name>
<surname>Igata</surname>
<given-names>T.</given-names>
</name>
</person-group> (<year>2018</year>). <article-title>Complete conformal classification of the Friedmann-Lema&#xee;tre-Robertson-Walker solutions with a linear equation of state</article-title>. <source>Class. Quantum Gravity</source> <volume>35</volume>, <fpage>105011</fpage>. <pub-id pub-id-type="doi">10.1088/1361-6382/aab99f</pub-id>
</citation>
</ref>
<ref id="B66">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Holwerda</surname>
<given-names>B. W.</given-names>
</name>
<name>
<surname>Bouwens</surname>
<given-names>R.</given-names>
</name>
<name>
<surname>Oesch</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Smit</surname>
<given-names>R.</given-names>
</name>
<name>
<surname>Illingworth</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Labbe</surname>
<given-names>I.</given-names>
</name>
</person-group> (<year>2015</year>). <article-title>The sizes of candidate galaxies<italic>z</italic>&#x223c; 9&#x2212;10: confirmation of the bright CANDELS sample and relation with luminosity and mass</article-title>. <source>ApJ</source> <volume>808</volume>, <fpage>6</fpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/808/1/6</pub-id>
</citation>
</ref>
<ref id="B67">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Hubble</surname>
<given-names>E.</given-names>
</name>
</person-group> (<year>1929</year>). <article-title>A relation between distance and radial velocity among extra-galactic nebulae</article-title>. <source>Proc. Natl. Acad. Sci.</source> <volume>15</volume>, <fpage>168</fpage>&#x2013;<lpage>173</lpage>. <pub-id pub-id-type="doi">10.1073/pnas.15.3.168</pub-id>
</citation>
</ref>
<ref id="B68">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Ibison</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2007</year>). <article-title>On the conformal forms of the Robertson-Walker metric</article-title>. <source>J. Math. Phys.</source> <volume>48</volume>, <fpage>122501</fpage>. <pub-id pub-id-type="doi">10.1063/1.2815811</pub-id>
</citation>
</ref>
<ref id="B69">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Infeld</surname>
<given-names>L.</given-names>
</name>
<name>
<surname>Schild</surname>
<given-names>A.</given-names>
</name>
</person-group> (<year>1945</year>). <article-title>A new approach to kinematic cosmology</article-title>. <source>Phys. Rev.</source> <volume>68</volume>, <fpage>250</fpage>&#x2013;<lpage>272</lpage>. <pub-id pub-id-type="doi">10.1103/PhysRev.68.250</pub-id>
</citation>
</ref>
<ref id="B70">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Infeld</surname>
<given-names>L.</given-names>
</name>
<name>
<surname>Schild</surname>
<given-names>A. E.</given-names>
</name>
</person-group> (<year>1946</year>). <article-title>A new approach to kinematic cosmology-(B)</article-title>. <source>Phys. Rev.</source> <volume>70</volume>, <fpage>410</fpage>&#x2013;<lpage>425</lpage>. <pub-id pub-id-type="doi">10.1103/PhysRev.70.410</pub-id>
</citation>
</ref>
<ref id="B71">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Iorio</surname>
<given-names>L.</given-names>
</name>
</person-group> (<year>2015</year>). <article-title>Gravitational anomalies in the solar system?</article-title> <source>Int. J. Mod. Phys. D</source> <volume>24</volume>, <fpage>1530015</fpage>&#x2013;<lpage>1530343</lpage>. <pub-id pub-id-type="doi">10.1142/S0218271815300153</pub-id>
</citation>
</ref>
<ref id="B72">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Iorio</surname>
<given-names>L.</given-names>
</name>
</person-group> (<year>2013</year>). <article-title>Local cosmological effects of the order of H in the orbital motion of a binary system</article-title>. <source>MNRAS</source> <volume>429</volume>, <fpage>915</fpage>&#x2013;<lpage>922</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/sts396</pub-id>
</citation>
</ref>
<ref id="B73">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Jacoby</surname>
<given-names>G. H.</given-names>
</name>
<name>
<surname>Branch</surname>
<given-names>D.</given-names>
</name>
<name>
<surname>Ciardullo</surname>
<given-names>R.</given-names>
</name>
<name>
<surname>Davies</surname>
<given-names>R. L.</given-names>
</name>
<name>
<surname>Harris</surname>
<given-names>W. E.</given-names>
</name>
<name>
<surname>Pierce</surname>
<given-names>M. J.</given-names>
</name>
<etal/>
</person-group> (<year>1992</year>). <article-title>A critical review of selected techniques for measuring extragalactic distances</article-title>. <source>PASP</source> <volume>104</volume>, <fpage>599</fpage>. <pub-id pub-id-type="doi">10.1086/133035</pub-id>
</citation>
</ref>
<ref id="B74">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Kastrup</surname>
<given-names>H. A.</given-names>
</name>
</person-group> (<year>2008</year>). <article-title>On the advancements of conformal transformations and their associated symmetries in geometry and theoretical physics</article-title>. <source>Ann. Phys.</source> <volume>520</volume>, <fpage>631</fpage>&#x2013;<lpage>690</lpage>. <pub-id pub-id-type="doi">10.1002/andp.200852009-1005</pub-id>
</citation>
</ref>
<ref id="B75">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Kauffmann</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>White</surname>
<given-names>S. D. M.</given-names>
</name>
<name>
<surname>Guiderdoni</surname>
<given-names>B.</given-names>
</name>
</person-group> (<year>1993</year>). <article-title>The formation and evolution of galaxies within merging dark matter haloes</article-title>. <source>MNRAS</source> <volume>264</volume>, <fpage>201</fpage>&#x2013;<lpage>218</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/264.1.201</pub-id>
</citation>
</ref>
<ref id="B76">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Kawinwanichakij</surname>
<given-names>L.</given-names>
</name>
<name>
<surname>Papovich</surname>
<given-names>C.</given-names>
</name>
<name>
<surname>Ciardullo</surname>
<given-names>R.</given-names>
</name>
<name>
<surname>Finkelstein</surname>
<given-names>S. L.</given-names>
</name>
<name>
<surname>Stevans</surname>
<given-names>M. L.</given-names>
</name>
<name>
<surname>Wold</surname>
<given-names>I. G. B.</given-names>
</name>
<etal/>
</person-group> (<year>2020</year>). <article-title>On the (lack of) evolution of the stellar mass function of massive galaxies from z &#x3d; 1.5 to 0.4</article-title>. <source>ApJ</source> <volume>892</volume>, <fpage>7</fpage>. <pub-id pub-id-type="doi">10.3847/1538-4357/ab75c4</pub-id>
</citation>
</ref>
<ref id="B77">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Knauth</surname>
<given-names>L. P.</given-names>
</name>
</person-group> (<year>2005</year>). <article-title>Temperature and salinity history of the precambrian ocean: Implications for the course of microbial evolution</article-title>. <source>Palaeogeogr. Palaeoclimatol. Palaeoecol.</source> <volume>219</volume>, <fpage>53</fpage>&#x2013;<lpage>69</lpage>. <pub-id pub-id-type="doi">10.1016/j.palaeo.2004.10.014</pub-id>
</citation>
</ref>
<ref id="B78">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Kopp</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Lean</surname>
<given-names>J. L.</given-names>
</name>
</person-group> (<year>2011</year>). <article-title>A new, lower value of total solar irradiance: Evidence and climate significance</article-title>. <source>Geophys. Res. Lett.</source> <volume>38</volume>, <fpage>L01706</fpage>. <pub-id pub-id-type="doi">10.1029/2010GL045777</pub-id>
</citation>
</ref>
<ref id="B79">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Kormendy</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Ho</surname>
<given-names>L. C.</given-names>
</name>
</person-group> (<year>2013</year>). <article-title>Coevolution (or not) of supermassive black holes and host galaxies</article-title>. <source>Annu. Rev. Astron. Astrophys.</source> <volume>51</volume>, <fpage>511</fpage>&#x2013;<lpage>653</lpage>. <pub-id pub-id-type="doi">10.1146/annurev-astro-082708-101811</pub-id>
</citation>
</ref>
<ref id="B80">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Koyama</surname>
<given-names>K.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>Cosmological tests of modified gravity</article-title>. <source>Rep. Prog. Phys.</source> <volume>79</volume>, <fpage>046902</fpage>. <pub-id pub-id-type="doi">10.1088/0034-4885/79/4/046902</pub-id>
</citation>
</ref>
<ref id="B81">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>K&#x159;&#xed;&#x17e;ek</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2012</year>). <article-title>Dark energy and the anthropic principle</article-title>. <source>New Astron.</source> <volume>17</volume>, <fpage>1</fpage>&#x2013;<lpage>7</lpage>. <pub-id pub-id-type="doi">10.1016/j.newast.2011.05.003</pub-id>
</citation>
</ref>
<ref id="B82">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>K&#x159;&#xed;&#x17e;ek</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2009</year>). <article-title>Does a gravitational aberration contribute to the accelerated expansion of the universe?</article-title> <source>Commun. Comput. Phys.</source> <volume>5</volume>, <fpage>1030</fpage>&#x2013;<lpage>1044</lpage>.</citation>
</ref>
<ref id="B83">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>K&#x159;&#xed;&#x17e;ek</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>K&#x159;&#xed;&#x17e;ek</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>Somer</surname>
<given-names>L.</given-names>
</name>
</person-group> (<year>2015</year>). <source>Antigravity - its origin and manifestations</source>. <publisher-loc>Saarbruecken</publisher-loc>: <publisher-name>Lambert Academic Publishing</publisher-name>.</citation>
</ref>
<ref id="B84">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>K&#x159;&#xed;&#x17e;ek</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Somer</surname>
<given-names>L.</given-names>
</name>
</person-group> (<year>2022</year>). <article-title>Anthropic principle and the Hubble-Lema&#xee;tre constant</article-title>. <source>Galaxies</source> <volume>10</volume>, <fpage>71</fpage>. <pub-id pub-id-type="doi">10.3390/galaxies10030071</pub-id>
</citation>
</ref>
<ref id="B85">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>K&#x159;&#xed;&#x17e;ek</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Somer</surname>
<given-names>L.</given-names>
</name>
</person-group> (<year>2015</year>). <article-title>Manifestations of dark energy in the solar system</article-title>. <source>Gravit. Cosmol.</source> <volume>21</volume>, <fpage>59</fpage>&#x2013;<lpage>72</lpage>. <pub-id pub-id-type="doi">10.1134/S0202289315010090</pub-id>
</citation>
</ref>
<ref id="B86">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Kroupa</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Famaey</surname>
<given-names>B.</given-names>
</name>
<name>
<surname>de Boer</surname>
<given-names>K. S.</given-names>
</name>
<name>
<surname>Dabringhausen</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Pawlowski</surname>
<given-names>M. S.</given-names>
</name>
<name>
<surname>Boily</surname>
<given-names>C. M.</given-names>
</name>
<etal/>
</person-group> (<year>2010</year>). <article-title>Local-Group tests of dark-matter concordance cosmology. Towards a new paradigm for structure formation</article-title>. <source>Astron. Astrophys.</source> <volume>523</volume>, <fpage>A32</fpage>. <pub-id pub-id-type="doi">10.1051/0004-6361/201014892</pub-id>
</citation>
</ref>
<ref id="B87">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Kroupa</surname>
<given-names>P.</given-names>
</name>
</person-group> (<year>2015</year>). <article-title>Galaxies as simple dynamical systems: Observational data disfavor dark matter and stochastic star formation</article-title>. <source>Can. J. Phys.</source> <volume>93</volume>, <fpage>169</fpage>&#x2013;<lpage>202</lpage>. <pub-id pub-id-type="doi">10.1139/cjp-2014-0179</pub-id>
</citation>
</ref>
<ref id="B88">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Kroupa</surname>
<given-names>P.</given-names>
</name>
</person-group> (<year>2012</year>). <article-title>The dark matter crisis: Falsification of the current standard model of cosmology</article-title>. <source>Publ. Astron. Soc. Aust.</source>, <volume>29</volume>, <fpage>395</fpage>&#x2013;<lpage>433</lpage>. <pub-id pub-id-type="doi">10.1071/AS12005</pub-id>
</citation>
</ref>
<ref id="B89">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Lainey</surname>
<given-names>V.</given-names>
</name>
<name>
<surname>Casajus</surname>
<given-names>L. G.</given-names>
</name>
<name>
<surname>Fuller</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Zannoni</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Tortora</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Cooper</surname>
<given-names>N.</given-names>
</name>
<etal/>
</person-group> (<year>2020</year>). <article-title>Resonance locking in giant planets indicated by the rapid orbital expansion of Titan</article-title>. <source>Nat. Astron.</source> <volume>4</volume>, <fpage>1053</fpage>&#x2013;<lpage>1058</lpage>. <pub-id pub-id-type="doi">10.1038/s41550-020-1120-5</pub-id>
</citation>
</ref>
<ref id="B90">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Leibundgut</surname>
<given-names>B.</given-names>
</name>
</person-group> (<year>2001</year>). <article-title>Cosmological implications from observations of type Ia supernovae</article-title>. <source>Annu. Rev. Astron. Astrophys.</source> <volume>39</volume>, <fpage>67</fpage>&#x2013;<lpage>98</lpage>. <pub-id pub-id-type="doi">10.1146/annurev.astro.39.1.67</pub-id>
</citation>
</ref>
<ref id="B91">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Leibundgut</surname>
<given-names>B.</given-names>
</name>
<name>
<surname>Schommer</surname>
<given-names>R.</given-names>
</name>
<name>
<surname>Phillips</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Riess</surname>
<given-names>A.</given-names>
</name>
<name>
<surname>Schmidt</surname>
<given-names>B.</given-names>
</name>
<name>
<surname>Spyromilio</surname>
<given-names>J.</given-names>
</name>
<etal/>
</person-group> (<year>1996</year>). <article-title>Time dilation in the light curve of the distant type IA supernova SN 1995K</article-title>. <source>ApJ</source> <volume>466</volume>, <fpage>L21</fpage>&#x2013;<lpage>L24</lpage>. <pub-id pub-id-type="doi">10.1086/310164</pub-id>
</citation>
</ref>
<ref id="B92">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Lelli</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>McGaugh</surname>
<given-names>S. S.</given-names>
</name>
<name>
<surname>Schombert</surname>
<given-names>J. M.</given-names>
</name>
<name>
<surname>Desmond</surname>
<given-names>H.</given-names>
</name>
<name>
<surname>Katz</surname>
<given-names>H.</given-names>
</name>
</person-group> (<year>2019</year>). <article-title>The baryonic Tully-Fisher relation for different velocity definitions and implications for galaxy angular momentum</article-title>. <source>MNRAS</source> <volume>484</volume>, <fpage>3267</fpage>&#x2013;<lpage>3278</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/stz205</pub-id>
</citation>
</ref>
<ref id="B93">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Lelli</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>McGaugh</surname>
<given-names>S. S.</given-names>
</name>
<name>
<surname>Schombert</surname>
<given-names>J. M.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>Sparc: Mass models for 175 disk galaxies with Spitzer photometry and accurate rotation curves</article-title>. <source>AJ</source> <volume>152</volume>, <fpage>157</fpage>. <pub-id pub-id-type="doi">10.3847/0004-6256/152/6/157</pub-id>
</citation>
</ref>
<ref id="B94">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Lelli</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>McGaugh</surname>
<given-names>S. S.</given-names>
</name>
<name>
<surname>Schombert</surname>
<given-names>J. M.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>The small scatter of the baryonic Tully-Fisher relation</article-title>. <source>ApJ</source> <volume>816</volume>, <fpage>L14</fpage>. <pub-id pub-id-type="doi">10.3847/2041-8205/816/1/L14</pub-id>
</citation>
</ref>
<ref id="B95">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Lema&#xee;tre</surname>
<given-names>G.</given-names>
</name>
</person-group> (<year>1927</year>). <article-title>Un Univers homog&#xe8;ne de masse constante et de rayon croissant rendant compte de la vitesse radiale des n&#xe9;buleuses extra-galactiques</article-title>. <source>Ann. Soci&#xe9;t&#xe9; Sci. Brux.</source> <volume>47</volume>, <fpage>49</fpage>&#x2013;<lpage>59</lpage>.</citation>
</ref>
<ref id="B96">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Lerner</surname>
<given-names>E. J.</given-names>
</name>
</person-group> (<year>2018</year>). <article-title>Observations contradict galaxy size and surface brightness predictions that are based on the expanding universe hypothesis</article-title>. <source>MNRAS</source> <volume>477</volume>, <fpage>3185</fpage>&#x2013;<lpage>3196</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/sty728</pub-id>
</citation>
</ref>
<ref id="B97">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Lin</surname>
<given-names>C. C.</given-names>
</name>
<name>
<surname>Shu</surname>
<given-names>F. H.</given-names>
</name>
</person-group> (<year>1964</year>). <article-title>On the spiral structure of disk galaxies</article-title>. <source>ApJ</source> <volume>140</volume>, <fpage>646</fpage>. <pub-id pub-id-type="doi">10.1086/147955</pub-id>
</citation>
</ref>
<ref id="B98">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Lin</surname>
<given-names>C. C.</given-names>
</name>
<name>
<surname>Shu</surname>
<given-names>F. H.</given-names>
</name>
</person-group> (<year>1966</year>). <article-title>On the spiral structure of disk galaxies, II. Outline of a theory of density waves</article-title>. <source>Proc. Natl. Acad. Sci.</source> <volume>55</volume>, <fpage>229</fpage>&#x2013;<lpage>234</lpage>. <pub-id pub-id-type="doi">10.1073/pnas.55.2.229</pub-id>
</citation>
</ref>
<ref id="B99">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Lindblad</surname>
<given-names>B.</given-names>
</name>
</person-group> (<year>1962</year>). &#x201c;<article-title>Theories of spiral structure in galaxies</article-title>,&#x201d; in <source>Problems of extra-galactic research</source>. Editor <person-group person-group-type="editor">
<name>
<surname>McVittie</surname>
<given-names>G. C.</given-names>
</name>
</person-group>, <volume>15</volume>, <fpage>146</fpage>.</citation>
</ref>
<ref id="B100">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Maddox</surname>
<given-names>S. J.</given-names>
</name>
<name>
<surname>Efstathiou</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Sutherland</surname>
<given-names>W. J.</given-names>
</name>
<name>
<surname>Loveday</surname>
<given-names>J.</given-names>
</name>
</person-group> (<year>1990</year>). <article-title>Galaxy correlations on large scales</article-title>. <source>MNRAS</source> <volume>242</volume>, <fpage>43P</fpage>&#x2013;<lpage>47P</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/242.1.43P</pub-id>
</citation>
</ref>
<ref id="B101">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Man</surname>
<given-names>A. W. S.</given-names>
</name>
<name>
<surname>Toft</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>Zirm</surname>
<given-names>A. W.</given-names>
</name>
<name>
<surname>Wuyts</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>van der Wel</surname>
<given-names>A.</given-names>
</name>
</person-group> (<year>2012</year>). <article-title>The pair fraction of massive galaxies at 0 &#x2a7d;<italic>z</italic>&#x2a7d; 3</article-title>. <source>ApJ</source> <volume>744</volume>, <fpage>85</fpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/744/2/85</pub-id>
</citation>
</ref>
<ref id="B102">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Man</surname>
<given-names>A. W. S.</given-names>
</name>
<name>
<surname>Zirm</surname>
<given-names>A. W.</given-names>
</name>
<name>
<surname>Toft</surname>
<given-names>S.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>Resolving the discrepancy of galaxy merger fraction measurements at z &#x223c; 0-3</article-title>. <source>ApJ</source> <volume>830</volume>, <fpage>89</fpage>. <pub-id pub-id-type="doi">10.3847/0004-637X/830/2/89</pub-id>
</citation>
</ref>
<ref id="B103">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Mannheim</surname>
<given-names>P. D.</given-names>
</name>
</person-group> (<year>2006</year>). <article-title>Alternatives to dark matter and dark energy</article-title>. <source>Prog. Part. Nucl. Phys.</source> <volume>56</volume>, <fpage>340</fpage>&#x2013;<lpage>445</lpage>. <pub-id pub-id-type="doi">10.1016/j.ppnp.2005.08.001</pub-id>
</citation>
</ref>
<ref id="B104">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Mannheim</surname>
<given-names>P. D.</given-names>
</name>
</person-group> (<year>1990</year>). <article-title>Conformal cosmology with no cosmological constant</article-title>. <source>General Relativ. Gravit.</source> <volume>22</volume>, <fpage>289</fpage>&#x2013;<lpage>298</lpage>. <pub-id pub-id-type="doi">10.1007/BF00756278</pub-id>
</citation>
</ref>
<ref id="B105">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Mannheim</surname>
<given-names>P. D.</given-names>
</name>
</person-group> (<year>2019</year>). <article-title>Is dark matter fact or fantasy? &#x2014; clues from the data</article-title>. <source>Int. J. Mod. Phys. D</source> <volume>28</volume>, <fpage>1944022</fpage>. <pub-id pub-id-type="doi">10.1142/S021827181944022X</pub-id>
</citation>
</ref>
<ref id="B106">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Mannheim</surname>
<given-names>P. D.</given-names>
</name>
</person-group> (<year>2012</year>). <article-title>Making the case for conformal gravity</article-title>. <source>Found. Phys.</source> <volume>42</volume>, <fpage>388</fpage>&#x2013;<lpage>420</lpage>. <pub-id pub-id-type="doi">10.1007/s10701-011-9608-6</pub-id>
</citation>
</ref>
<ref id="B107">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Mannheim</surname>
<given-names>P. D.</given-names>
</name>
<name>
<surname>O&#x2019;Brien</surname>
<given-names>J. G.</given-names>
</name>
</person-group> (<year>2012</year>). <article-title>Fitting galactic rotation curves with conformal gravity and a global quadratic potential</article-title>. <source>Phys. Rev. D.</source> <volume>85</volume>, <fpage>124020</fpage>. <pub-id pub-id-type="doi">10.1103/PhysRevD.85.124020</pub-id>
</citation>
</ref>
<ref id="B108">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Mannheim</surname>
<given-names>P. D.</given-names>
</name>
<name>
<surname>O&#x2019;Brien</surname>
<given-names>J. G.</given-names>
</name>
</person-group> (<year>2011</year>). <article-title>Impact of a global quadratic potential on galactic rotation curves</article-title>. <source>Phys. Rev. Lett.</source> <volume>106</volume>, <fpage>121101</fpage>. <pub-id pub-id-type="doi">10.1103/PhysRevLett.106.121101</pub-id>
</citation>
</ref>
<ref id="B109">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Mathewson</surname>
<given-names>D. S.</given-names>
</name>
<name>
<surname>Ford</surname>
<given-names>V. L.</given-names>
</name>
<name>
<surname>Buchhorn</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>1992</year>). <article-title>A southern sky survey of the peculiar velocities of 1355 spiral galaxies</article-title>. <source>ApJS</source> <volume>81</volume>, <fpage>413</fpage>. <pub-id pub-id-type="doi">10.1086/191700</pub-id>
</citation>
</ref>
<ref id="B110">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>McGaugh</surname>
<given-names>S. S.</given-names>
</name>
<name>
<surname>Lelli</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>Schombert</surname>
<given-names>J. M.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>Radial acceleration relation in rotationally supported galaxies</article-title>. <source>Phys. Rev. Lett.</source> <volume>117</volume>, <fpage>201101</fpage>. <pub-id pub-id-type="doi">10.1103/PhysRevLett.117.201101</pub-id>
</citation>
</ref>
<ref id="B111">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>McGaugh</surname>
<given-names>S. S.</given-names>
</name>
<name>
<surname>Li</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Lelli</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>Schombert</surname>
<given-names>J. M.</given-names>
</name>
</person-group> (<year>2018</year>). <article-title>Presence of a fundamental acceleration scale in galaxies</article-title>. <source>Nat. Astron.</source> <volume>2</volume>, <fpage>924</fpage>. <pub-id pub-id-type="doi">10.1038/s41550-018-0615-9</pub-id>
</citation>
</ref>
<ref id="B112">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>McGaugh</surname>
<given-names>S. S.</given-names>
</name>
</person-group> (<year>2019</year>). <article-title>The imprint of spiral arms on the galactic rotation curve</article-title>. <source>ApJ</source> <volume>885</volume>, <fpage>87</fpage>. <pub-id pub-id-type="doi">10.3847/1538-4357/ab479b</pub-id>
</citation>
</ref>
<ref id="B113">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>McGaugh</surname>
<given-names>S. S.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>The surface density profile of the galactic disk from the terminal velocity curve</article-title>. <source>ApJ</source> <volume>816</volume>, <fpage>42</fpage>. <pub-id pub-id-type="doi">10.3847/0004-637X/816/1/42</pub-id>
</citation>
</ref>
<ref id="B114">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>McLure</surname>
<given-names>R. J.</given-names>
</name>
<name>
<surname>Pearce</surname>
<given-names>H. J.</given-names>
</name>
<name>
<surname>Dunlop</surname>
<given-names>J. S.</given-names>
</name>
<name>
<surname>Cirasuolo</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Curtis-Lake</surname>
<given-names>E.</given-names>
</name>
<name>
<surname>Bruce</surname>
<given-names>V. A.</given-names>
</name>
<etal/>
</person-group> (<year>2013</year>). <article-title>The sizes, masses and specific star formation rates of massive galaxies at 1.3 &#x3c; z &#x3c; 1.5: Strong evidence in favour of evolution via minor mergers</article-title>. <source>MNRAS</source> <volume>428</volume>, <fpage>1088</fpage>&#x2013;<lpage>1106</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/sts092</pub-id>
</citation>
</ref>
<ref id="B115">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>McVittie</surname>
<given-names>G. C.</given-names>
</name>
</person-group> (<year>1933</year>). <article-title>The mass-particle in an expanding universe</article-title>. <source>MNRAS</source> <volume>93</volume>, <fpage>325</fpage>&#x2013;<lpage>339</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/93.5.325</pub-id>
</citation>
</ref>
<ref id="B116">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Milgrom</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>1983</year>). <article-title>A modification of the Newtonian dynamics - implications for galaxies</article-title>. <source>ApJ</source> <volume>270</volume>, <fpage>371</fpage>&#x2013;<lpage>383</lpage>. <pub-id pub-id-type="doi">10.1086/161131</pub-id>
</citation>
</ref>
<ref id="B117">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Milgrom</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>1983</year>). <article-title>A modification of the Newtonian dynamics as a possible alternative to the hidden mass hypothesis</article-title>. <source>ApJ</source> <volume>270</volume>, <fpage>365</fpage>&#x2013;<lpage>370</lpage>. <pub-id pub-id-type="doi">10.1086/161130</pub-id>
</citation>
</ref>
<ref id="B118">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Milgrom</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2010</year>). <article-title>Quasi-linear formulation of MOND</article-title>. <source>MNRAS</source> <volume>403</volume>, <fpage>886</fpage>&#x2013;<lpage>895</lpage>. <pub-id pub-id-type="doi">10.1111/j.1365-2966.2009.16184.x</pub-id>
</citation>
</ref>
<ref id="B119">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Milgrom</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2012</year>). <article-title>Testing MOND over a wide acceleration range in X-ray ellipticals</article-title>. <source>Phys. Rev. Lett.</source> <volume>109</volume>, <fpage>131101</fpage>. <pub-id pub-id-type="doi">10.1103/PhysRevLett.109.131101</pub-id>
</citation>
</ref>
<ref id="B120">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Mo</surname>
<given-names>H. J.</given-names>
</name>
<name>
<surname>Mao</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>White</surname>
<given-names>S. D. M.</given-names>
</name>
</person-group> (<year>1998</year>). <article-title>The formation of galactic discs</article-title>. <source>MNRAS</source> <volume>295</volume>, <fpage>319</fpage>&#x2013;<lpage>336</lpage>. <pub-id pub-id-type="doi">10.1046/j.1365-8711.1998.01227.x</pub-id>
</citation>
</ref>
<ref id="B121">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Moore</surname>
<given-names>B.</given-names>
</name>
<name>
<surname>Ghigna</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>Governato</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>Lake</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Quinn</surname>
<given-names>T.</given-names>
</name>
<name>
<surname>Stadel</surname>
<given-names>J.</given-names>
</name>
<etal/>
</person-group> (<year>1999</year>). <article-title>Dark matter substructure within galactic halos</article-title>. <source>ApJ</source> <volume>524</volume>, <fpage>L19</fpage>&#x2013;<lpage>L22</lpage>. <pub-id pub-id-type="doi">10.1086/312287</pub-id>
</citation>
</ref>
<ref id="B122">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Mould</surname>
<given-names>J. R.</given-names>
</name>
<name>
<surname>Huchra</surname>
<given-names>J. P.</given-names>
</name>
<name>
<surname>Freedman</surname>
<given-names>W. L.</given-names>
</name>
<name>
<surname>Kennicutt J Robert</surname>
<given-names>C.</given-names>
</name>
<name>
<surname>Ferrarese</surname>
<given-names>L.</given-names>
</name>
<name>
<surname>Ford</surname>
<given-names>H. C.</given-names>
</name>
<etal/>
</person-group> (<year>2000</year>). <article-title>The Hubble Space Telescope Key Project on the extragalactic distance scale. XXVIII. Combining the constraints on the Hubble constant</article-title>. <source>ApJ</source> <volume>529</volume>, <fpage>786</fpage>&#x2013;<lpage>794</lpage>. <pub-id pub-id-type="doi">10.1086/308304</pub-id>
</citation>
</ref>
<ref id="B123">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Mundy</surname>
<given-names>C. J.</given-names>
</name>
<name>
<surname>Conselice</surname>
<given-names>C. J.</given-names>
</name>
<name>
<surname>Duncan</surname>
<given-names>K. J.</given-names>
</name>
<name>
<surname>Almaini</surname>
<given-names>O.</given-names>
</name>
<name>
<surname>H&#xe4;u&#xdf;ler</surname>
<given-names>B.</given-names>
</name>
<name>
<surname>Hartley</surname>
<given-names>W. G.</given-names>
</name>
</person-group> (<year>2017</year>). <article-title>A consistent measure of the merger histories of massive galaxies using close-pair statistics - I. Major mergers at z &#x3c; 3.5</article-title>. <source>MNRAS</source> <volume>470</volume>, <fpage>3507</fpage>&#x2013;<lpage>3531</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/stx1238</pub-id>
</citation>
</ref>
<ref id="B124">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Naab</surname>
<given-names>T.</given-names>
</name>
<name>
<surname>Johansson</surname>
<given-names>P. H.</given-names>
</name>
<name>
<surname>Ostriker</surname>
<given-names>J. P.</given-names>
</name>
</person-group> (<year>2009</year>). <article-title>Minor mergers and the size evolution of elliptical galaxies</article-title>. <source>ApJ</source> <volume>699</volume>, <fpage>L178</fpage>&#x2013;<lpage>L182</lpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/699/2/L178</pub-id>
</citation>
</ref>
<ref id="B125">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Nandra</surname>
<given-names>R.</given-names>
</name>
<name>
<surname>Lasenby</surname>
<given-names>A. N.</given-names>
</name>
<name>
<surname>Hobson</surname>
<given-names>M. P.</given-names>
</name>
</person-group> (<year>2012</year>). <article-title>The effect of a massive object on an expanding universe</article-title>. <source>MNRAS</source> <volume>422</volume>, <fpage>2931</fpage>&#x2013;<lpage>2944</lpage>. <pub-id pub-id-type="doi">10.1111/j.1365-2966.2012.20618.x</pub-id>
</citation>
</ref>
<ref id="B126">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Navarro</surname>
<given-names>J. F.</given-names>
</name>
<name>
<surname>Frenk</surname>
<given-names>C. S.</given-names>
</name>
<name>
<surname>White</surname>
<given-names>S. D. M.</given-names>
</name>
</person-group> (<year>1997</year>). <article-title>A universal density profile from hierarchical clustering</article-title>. <source>ApJ</source> <volume>490</volume>, <fpage>493</fpage>&#x2013;<lpage>508</lpage>. <pub-id pub-id-type="doi">10.1086/304888</pub-id>
</citation>
</ref>
<ref id="B127">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Navarro</surname>
<given-names>J. F.</given-names>
</name>
<name>
<surname>Frenk</surname>
<given-names>C. S.</given-names>
</name>
<name>
<surname>White</surname>
<given-names>S. D. M.</given-names>
</name>
</person-group> (<year>1996</year>). <article-title>The structure of cold dark matter halos</article-title>. <source>ApJ</source> <volume>462</volume>, <fpage>563</fpage>. <pub-id pub-id-type="doi">10.1086/177173</pub-id>
</citation>
</ref>
<ref id="B128">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Newman</surname>
<given-names>A. B.</given-names>
</name>
<name>
<surname>Ellis</surname>
<given-names>R. S.</given-names>
</name>
<name>
<surname>Bundy</surname>
<given-names>K.</given-names>
</name>
<name>
<surname>Treu</surname>
<given-names>T.</given-names>
</name>
</person-group> (<year>2012</year>). <article-title>Can minor merging account for the size growth of quiescent galaxies? New results from the CANDELS survey</article-title>. <source>ApJ</source> <volume>746</volume>, <fpage>162</fpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/746/2/162</pub-id>
</citation>
</ref>
<ref id="B129">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Noerdlinger</surname>
<given-names>P. D.</given-names>
</name>
<name>
<surname>Petrosian</surname>
<given-names>V.</given-names>
</name>
</person-group> (<year>1971</year>). <article-title>The effect of cosmological expansion on self-gravitating ensembles of particles</article-title>. <source>ApJ</source> <volume>168</volume>, <fpage>1</fpage>. <pub-id pub-id-type="doi">10.1086/151054</pub-id>
</citation>
</ref>
<ref id="B130">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Noordermeer</surname>
<given-names>E.</given-names>
</name>
<name>
<surname>Verheijen</surname>
<given-names>M. A. W.</given-names>
</name>
</person-group> (<year>2007</year>). <article-title>The high-mass end of the Tully-Fisher relation</article-title>. <source>MNRAS</source> <volume>381</volume>, <fpage>1463</fpage>&#x2013;<lpage>1472</lpage>. <pub-id pub-id-type="doi">10.1111/j.1365-2966.2007.12369.x</pub-id>
</citation>
</ref>
<ref id="B131">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>O&#x2019;Brien</surname>
<given-names>J. G.</given-names>
</name>
<name>
<surname>Mannheim</surname>
<given-names>P. D.</given-names>
</name>
</person-group> (<year>2012</year>). <article-title>Fitting dwarf galaxy rotation curves with conformal gravity</article-title>. <source>MNRAS</source> <volume>421</volume>, <fpage>1273</fpage>&#x2013;<lpage>1282</lpage>. <pub-id pub-id-type="doi">10.1111/j.1365-2966.2011.20386.x</pub-id>
</citation>
</ref>
<ref id="B132">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Oesch</surname>
<given-names>P. A.</given-names>
</name>
<name>
<surname>Bouwens</surname>
<given-names>R. J.</given-names>
</name>
<name>
<surname>Carollo</surname>
<given-names>C. M.</given-names>
</name>
<name>
<surname>Illingworth</surname>
<given-names>G. D.</given-names>
</name>
<name>
<surname>Trenti</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Stiavelli</surname>
<given-names>M.</given-names>
</name>
<etal/>
</person-group> (<year>2010</year>). <article-title>Structure and morphologies of z &#x223c;7-8 galaxies from ultra-deep WFC3/IR imaging of the Hubble Ultra-Deep Field</article-title>. <source>ApJ</source> <volume>709</volume>, <fpage>L21</fpage>&#x2013;<lpage>L25</lpage>. <pub-id pub-id-type="doi">10.1088/2041-8205/709/1/L21</pub-id>
</citation>
</ref>
<ref id="B133">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Pachner</surname>
<given-names>J.</given-names>
</name>
</person-group> (<year>1964</year>). <article-title>Nonconservation of energy during cosmic evolution</article-title>. <source>Phys. Rev. Lett.</source> <volume>12</volume>, <fpage>117</fpage>&#x2013;<lpage>118</lpage>. <pub-id pub-id-type="doi">10.1103/PhysRevLett.12.117</pub-id>
</citation>
</ref>
<ref id="B134">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Pawlowski</surname>
<given-names>M. S.</given-names>
</name>
<name>
<surname>Kroupa</surname>
<given-names>P.</given-names>
</name>
</person-group> (<year>2013</year>). <article-title>The rotationally stabilized VPOS and predicted proper motions of the Milky Way satellite galaxies</article-title>. <source>MNRAS</source> <volume>435</volume>, <fpage>2116</fpage>&#x2013;<lpage>2131</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/stt1429</pub-id>
</citation>
</ref>
<ref id="B135">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Pawlowski</surname>
<given-names>M. S.</given-names>
</name>
<name>
<surname>McGaugh</surname>
<given-names>S. S.</given-names>
</name>
</person-group> (<year>2014</year>). <article-title>Perseus I and the NGC 3109 association in the context of the Local Group dwarf galaxy structures</article-title>. <source>MNRAS</source> <volume>440</volume>, <fpage>908</fpage>&#x2013;<lpage>919</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/stu321</pub-id>
</citation>
</ref>
<ref id="B136">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Peacock</surname>
<given-names>J. A.</given-names>
</name>
</person-group> (<year>1999</year>). <source>Cosmological physics</source>. <publisher-loc>Cambridge</publisher-loc>: <publisher-name>Cambridge University Press</publisher-name>.</citation>
</ref>
<ref id="B137">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Persic</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Salucci</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Stel</surname>
<given-names>F.</given-names>
</name>
</person-group> (<year>1996</year>). <article-title>The universal rotation curve of spiral galaxies &#x2014; I. The dark matter connection</article-title>. <source>MNRAS</source> <volume>281</volume>, <fpage>27</fpage>&#x2013;<lpage>47</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/278.1.27</pub-id>
</citation>
</ref>
<ref id="B138">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Phillips</surname>
<given-names>M. M.</given-names>
</name>
<name>
<surname>Lira</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Suntzeff</surname>
<given-names>N. B.</given-names>
</name>
<name>
<surname>Schommer</surname>
<given-names>R. A.</given-names>
</name>
<name>
<surname>Hamuy</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Maza</surname>
<given-names>J.</given-names>
</name>
</person-group> (<year>1999</year>). <article-title>The reddening-free decline rate versus luminosity relationship for type Ia supernovae</article-title>. <source>AJ</source> <volume>118</volume>, <fpage>1766</fpage>&#x2013;<lpage>1776</lpage>. <pub-id pub-id-type="doi">10.1086/301032</pub-id>
</citation>
</ref>
<ref id="B139">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Phillips</surname>
<given-names>M. M.</given-names>
</name>
</person-group> (<year>1993</year>). <article-title>The absolute magnitudes of type IA supernovae</article-title>. <source>ApJ</source> <volume>413</volume>, <fpage>L105</fpage>. <pub-id pub-id-type="doi">10.1086/186970</pub-id>
</citation>
</ref>
<ref id="B140">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Ribas</surname>
<given-names>I.</given-names>
</name>
</person-group> (<year>2010</year>). &#x201c;<article-title>The Sun and stars as the primary energy input in planetary atmospheres</article-title>,&#x201d; in <source>Solar and stellar variability: Impact on Earth and planets</source>. Editors <person-group person-group-type="editor">
<name>
<surname>Kosovichev</surname>
<given-names>A. G.</given-names>
</name>
<name>
<surname>Andrei</surname>
<given-names>A. H.</given-names>
</name>
<name>
<surname>Rozelot</surname>
<given-names>J. P.</given-names>
</name>
</person-group>, <volume>264</volume>, <fpage>3</fpage>&#x2013;<lpage>18</lpage>. <pub-id pub-id-type="doi">10.1017/S1743921309992298</pub-id>
</citation>
</ref>
<ref id="B141">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Riofrio</surname>
<given-names>L.</given-names>
</name>
</person-group> (<year>2012</year>). <article-title>Calculation of lunar orbit anomaly</article-title>. <source>Planet. Sci.</source> <volume>1</volume>, <fpage>1</fpage>. <pub-id pub-id-type="doi">10.1186/2191-2521-1-1</pub-id>
</citation>
</ref>
<ref id="B142">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Robert</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>Chaussidon</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2006</year>). <article-title>A palaeotemperature curve for the Precambrian oceans based on silicon isotopes in cherts</article-title>. <source>Nature</source> <volume>443</volume>, <fpage>969</fpage>&#x2013;<lpage>972</lpage>. <pub-id pub-id-type="doi">10.1038/nature05239</pub-id>
</citation>
</ref>
<ref id="B143">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Roberts</surname>
<given-names>J. W. W.</given-names>
</name>
<name>
<surname>Roberts</surname>
<given-names>M. S.</given-names>
</name>
<name>
<surname>Shu</surname>
<given-names>F. H.</given-names>
</name>
</person-group> (<year>1975</year>). <article-title>Density wave theory and the classification of spiral galaxies</article-title>. <source>ApJ</source> <volume>196</volume>, <fpage>381</fpage>&#x2013;<lpage>405</lpage>. <pub-id pub-id-type="doi">10.1086/153421</pub-id>
</citation>
</ref>
<ref id="B144">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Rubin</surname>
<given-names>V. C.</given-names>
</name>
<name>
<surname>Burstein</surname>
<given-names>D.</given-names>
</name>
<name>
<surname>Ford</surname>
<given-names>J. W. K.</given-names>
</name>
<name>
<surname>Thonnard</surname>
<given-names>N.</given-names>
</name>
</person-group> (<year>1985</year>). <article-title>Rotation velocities of 16 SA galaxies and a comparison of Sa, SB and SC rotation properties</article-title>. <source>ApJ</source> <volume>289</volume>, <fpage>81</fpage>&#x2013;<lpage>104</lpage>. <pub-id pub-id-type="doi">10.1086/162866</pub-id>
</citation>
</ref>
<ref id="B145">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Rubin</surname>
<given-names>V. C.</given-names>
</name>
<name>
<surname>Ford</surname>
<given-names>J. W. K.</given-names>
</name>
<name>
<surname>Thonnard</surname>
<given-names>N.</given-names>
</name>
</person-group> (<year>1980</year>). <article-title>Rotational properties of 21 SC galaxies with a large range of luminosities and radii, from NGC 4605 (R&#x3d;4 kpc) to UGC 2885 (R&#x3d;122 kpc)</article-title>. <source>ApJ</source> <volume>238</volume>, <fpage>471</fpage>&#x2013;<lpage>487</lpage>. <pub-id pub-id-type="doi">10.1086/158003</pub-id>
</citation>
</ref>
<ref id="B146">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Rubin</surname>
<given-names>V. C.</given-names>
</name>
<name>
<surname>Ford</surname>
<given-names>W. K.</given-names>
</name>
</person-group> (<year>1970</year>). <article-title>Rotation of the Andromeda nebula from a spectroscopic survey of emission regions</article-title>. <source>ApJ</source> <volume>159</volume>, <fpage>379</fpage>. <pub-id pub-id-type="doi">10.1086/150317</pub-id>
</citation>
</ref>
<ref id="B147">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Ryden</surname>
<given-names>B.</given-names>
</name>
</person-group> (<year>2016</year>). <source>Introduction to cosmology</source>. <publisher-loc>Cambridge</publisher-loc>: <publisher-name>Cambridge University Press</publisher-name>.</citation>
</ref>
<ref id="B148">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Salese</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>McMahon</surname>
<given-names>W. J.</given-names>
</name>
<name>
<surname>Balme</surname>
<given-names>M. R.</given-names>
</name>
<name>
<surname>Ansan</surname>
<given-names>V.</given-names>
</name>
<name>
<surname>Davis</surname>
<given-names>J. M.</given-names>
</name>
<name>
<surname>Kleinhans</surname>
<given-names>M. G.</given-names>
</name>
</person-group> (<year>2020</year>). <article-title>Sustained fluvial deposition recorded in Mars&#x2019; Noachian stratigraphic record</article-title>. <source>Nat. Commun.</source> <volume>11</volume>, <fpage>2067</fpage>. <pub-id pub-id-type="doi">10.1038/s41467-020-15622-0</pub-id>
</citation>
</ref>
<ref id="B149">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Sanders</surname>
<given-names>R. H.</given-names>
</name>
<name>
<surname>McGaugh</surname>
<given-names>S. S.</given-names>
</name>
</person-group> (<year>2002</year>). <article-title>Modified Newtonian dynamics as an alternative to dark matter</article-title>. <source>Annu. Rev. Astron. Astrophys.</source> <volume>40</volume>, <fpage>263</fpage>&#x2013;<lpage>317</lpage>. <pub-id pub-id-type="doi">10.1146/annurev.astro.40.060401.093923</pub-id>
</citation>
</ref>
<ref id="B150">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Sanders</surname>
<given-names>R. H.</given-names>
</name>
</person-group> (<year>1996</year>). <article-title>The published extended rotation curves of spiral galaxies: Confrontation with modified dynamics</article-title>. <source>ApJ</source> <volume>473</volume>, <fpage>117</fpage>&#x2013;<lpage>129</lpage>. <pub-id pub-id-type="doi">10.1086/178131</pub-id>
</citation>
</ref>
<ref id="B151">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Sandstrom</surname>
<given-names>K. M.</given-names>
</name>
<name>
<surname>Leroy</surname>
<given-names>A. K.</given-names>
</name>
<name>
<surname>Walter</surname>
<given-names>F.</given-names>
</name>
<name>
<surname>Bolatto</surname>
<given-names>A. D.</given-names>
</name>
<name>
<surname>Croxall</surname>
<given-names>K. V.</given-names>
</name>
<name>
<surname>Draine</surname>
<given-names>B. T.</given-names>
</name>
<etal/>
</person-group> (<year>2013</year>). <article-title>The CO-to-H<sub>2</sub> conversion factor and dust-to-gas ratio on kiloparsec scales in nearby galaxies</article-title>. <source>ApJ</source> <volume>777</volume>, <fpage>5</fpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/777/1/5</pub-id>
</citation>
</ref>
<ref id="B152">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Schneider</surname>
<given-names>P.</given-names>
</name>
</person-group> (<year>2015</year>). <source>Extragalactic Astronomy and cosmology: An introduction</source>. <publisher-loc>New York</publisher-loc>: <publisher-name>Springer</publisher-name>. <pub-id pub-id-type="doi">10.1007/978-3-642-54083-7</pub-id>
</citation>
</ref>
<ref id="B153">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Sellwood</surname>
<given-names>J. A.</given-names>
</name>
<name>
<surname>Carlberg</surname>
<given-names>R. G.</given-names>
</name>
</person-group> (<year>1984</year>). <article-title>Spiral instabilities provoked by accretion and star formation</article-title>. <source>ApJ</source> <volume>282</volume>, <fpage>61</fpage>&#x2013;<lpage>74</lpage>. <pub-id pub-id-type="doi">10.1086/162176</pub-id>
</citation>
</ref>
<ref id="B154">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Sellwood</surname>
<given-names>J. A.</given-names>
</name>
</person-group> (<year>2011</year>). <article-title>The lifetimes of spiral patterns in disc galaxies</article-title>. <source>MNRAS</source> <volume>410</volume>, <fpage>1637</fpage>&#x2013;<lpage>1646</lpage>. <pub-id pub-id-type="doi">10.1111/j.1365-2966.2010.17545.x</pub-id>
</citation>
</ref>
<ref id="B155">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Sereno</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Jetzer</surname>
<given-names>P.</given-names>
</name>
</person-group> (<year>2007</year>). <article-title>Evolution of gravitational orbits in the expanding universe</article-title>. <source>Phys. Rev. D.</source> <volume>75</volume>, <fpage>064031</fpage>. <pub-id pub-id-type="doi">10.1103/PhysRevD.75.064031</pub-id>
</citation>
</ref>
<ref id="B156">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Shibuya</surname>
<given-names>T.</given-names>
</name>
<name>
<surname>Ouchi</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Harikane</surname>
<given-names>Y.</given-names>
</name>
</person-group> (<year>2015</year>). <article-title>Morphologies of &#x223c;190,000 galaxies at z &#x3d; 0-10 revealed with HST legacy data. I. Size evolution</article-title>. <source>ApJS</source> <volume>219</volume>, <fpage>15</fpage>. <pub-id pub-id-type="doi">10.1088/0067-0049/219/2/15</pub-id>
</citation>
</ref>
<ref id="B157">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Shu</surname>
<given-names>F. H.</given-names>
</name>
</person-group> (<year>1970</year>). <article-title>On the density-wave theory of galactic spirals. I. Spiral structure as a normal mode of oscillation</article-title>. <source>ApJ</source> <volume>160</volume>, <fpage>89</fpage>. <pub-id pub-id-type="doi">10.1086/150409</pub-id>
</citation>
</ref>
<ref id="B158">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Shu</surname>
<given-names>F. H.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>Six decades of spiral density wave theory</article-title>. <source>Annu. Rev. Astron. Astrophys.</source>, <volume>54</volume>, <fpage>667</fpage>&#x2013;<lpage>724</lpage>. <pub-id pub-id-type="doi">10.1146/annurev-astro-081915-023426</pub-id>
</citation>
</ref>
<ref id="B159">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Sofue</surname>
<given-names>Y.</given-names>
</name>
</person-group> (<year>2017</year>). <article-title>Rotation and mass in the Milky Way and spiral galaxies</article-title>. <source>PASJ</source> <volume>69</volume>, <fpage>R1</fpage>. <pub-id pub-id-type="doi">10.1093/pasj/psw103</pub-id>
</citation>
</ref>
<ref id="B160">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Sofue</surname>
<given-names>Y.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>Rotation curve decomposition for size-mass relations of bulge, disk, and dark halo components in spiral galaxies</article-title>. <source>PASJ</source> <volume>68</volume>, <fpage>2</fpage>. <pub-id pub-id-type="doi">10.1093/pasj/psv103</pub-id>
</citation>
</ref>
<ref id="B161">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Sofue</surname>
<given-names>Y.</given-names>
</name>
<name>
<surname>Rubin</surname>
<given-names>V.</given-names>
</name>
</person-group> (<year>2001</year>). <article-title>Rotation curves of spiral galaxies</article-title>. <source>Annu. Rev. Astron. Astrophys.</source> <volume>39</volume>, <fpage>137</fpage>&#x2013;<lpage>174</lpage>. <pub-id pub-id-type="doi">10.1146/annurev.astro.39.1.137</pub-id>
</citation>
</ref>
<ref id="B162">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Stephenson</surname>
<given-names>F. R.</given-names>
</name>
<name>
<surname>Morrison</surname>
<given-names>L. V.</given-names>
</name>
<name>
<surname>Hohenkerk</surname>
<given-names>C. Y.</given-names>
</name>
</person-group> (<year>2016</year>). <article-title>Measurement of the Earth&#x2019;s rotation: 720 BC to AD 2015</article-title>. <source>Proc. R. Soc. Lond. Ser. A</source> <volume>472</volume>, <fpage>20160404</fpage>. <pub-id pub-id-type="doi">10.1098/rspa.2016.0404</pub-id>
</citation>
</ref>
<ref id="B163">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Swaters</surname>
<given-names>R. A.</given-names>
</name>
<name>
<surname>Madore</surname>
<given-names>B. F.</given-names>
</name>
<name>
<surname>Trewhella</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2000</year>). <article-title>High-resolution rotation curves of low surface brightness galaxies</article-title>. <source>ApJ</source> <volume>531</volume>, <fpage>L107</fpage>&#x2013;<lpage>L110</lpage>. <pub-id pub-id-type="doi">10.1086/312540</pub-id>
</citation>
</ref>
<ref id="B164">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Swaters</surname>
<given-names>R. A.</given-names>
</name>
<name>
<surname>Madore</surname>
<given-names>B. F.</given-names>
</name>
<name>
<surname>van den Bosch</surname>
<given-names>F. C.</given-names>
</name>
<name>
<surname>Balcells</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2003</year>). <article-title>The central mass distribution in dwarf and low surface brightness galaxies</article-title>. <source>ApJ</source> <volume>583</volume>, <fpage>732</fpage>&#x2013;<lpage>751</lpage>. <pub-id pub-id-type="doi">10.1086/345426</pub-id>
</citation>
</ref>
<ref id="B165">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Taylor</surname>
<given-names>E. N.</given-names>
</name>
<name>
<surname>Franx</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Glazebrook</surname>
<given-names>K.</given-names>
</name>
<name>
<surname>Brinchmann</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>van der Wel</surname>
<given-names>A.</given-names>
</name>
<name>
<surname>van Dokkum</surname>
<given-names>P. G.</given-names>
</name>
</person-group> (<year>2010</year>). <article-title>On the dearth of compact, massive, red sequence galaxies in the local universe</article-title>. <source>ApJ</source> <volume>720</volume>, <fpage>723</fpage>&#x2013;<lpage>741</lpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/720/1/723</pub-id>
</citation>
</ref>
<ref id="B166">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Tiley</surname>
<given-names>A. L.</given-names>
</name>
<name>
<surname>Swinbank</surname>
<given-names>A. M.</given-names>
</name>
<name>
<surname>Harrison</surname>
<given-names>C. M.</given-names>
</name>
<name>
<surname>Smail</surname>
<given-names>I.</given-names>
</name>
<name>
<surname>Turner</surname>
<given-names>O. J.</given-names>
</name>
<name>
<surname>Schaller</surname>
<given-names>M.</given-names>
</name>
<etal/>
</person-group> (<year>2019</year>). <article-title>The shapes of the rotation curves of star-forming galaxies over the last &#x2248; 10 Gyr</article-title>. <source>MNRAS</source> <volume>485</volume>, <fpage>934</fpage>&#x2013;<lpage>960</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/stz428</pub-id>
</citation>
</ref>
<ref id="B167">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Toomre</surname>
<given-names>A.</given-names>
</name>
</person-group> (<year>1977</year>). <article-title>Theories of spiral structure</article-title>. <source>Annu. Rev. Astron. Astrophys.</source> <volume>15</volume>, <fpage>437</fpage>&#x2013;<lpage>478</lpage>. <pub-id pub-id-type="doi">10.1146/annurev.aa.15.090177.002253</pub-id>
</citation>
</ref>
<ref id="B168">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Trujillo</surname>
<given-names>I.</given-names>
</name>
<name>
<surname>F&#xf6;rster Schreiber</surname>
<given-names>N. M.</given-names>
</name>
<name>
<surname>Rudnick</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Barden</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Franx</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Rix</surname>
<given-names>H. W.</given-names>
</name>
<etal/>
</person-group> (<year>2006</year>). <article-title>The size evolution of galaxies since z&#x223c;3: Combining SDSS, GEMS, and FIRES</article-title>. <source>ApJ</source> <volume>650</volume>, <fpage>18</fpage>&#x2013;<lpage>41</lpage>. <pub-id pub-id-type="doi">10.1086/506464</pub-id>
</citation>
</ref>
<ref id="B169">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Tully</surname>
<given-names>R. B.</given-names>
</name>
<name>
<surname>Fisher</surname>
<given-names>J. R.</given-names>
</name>
</person-group> (<year>1977</year>). <article-title>A new method of determining distances to galaxies</article-title>. <source>Astron. Astrophys.</source> <volume>54</volume>, <fpage>661</fpage>&#x2013;<lpage>673</lpage>.</citation>
</ref>
<ref id="B170">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>van Albada</surname>
<given-names>T. S.</given-names>
</name>
<name>
<surname>Bahcall</surname>
<given-names>J. N.</given-names>
</name>
<name>
<surname>Begeman</surname>
<given-names>K.</given-names>
</name>
<name>
<surname>Sancisi</surname>
<given-names>R.</given-names>
</name>
</person-group> (<year>1985</year>). <article-title>Distribution of dark matter in the spiral galaxy NGC 3198</article-title>. <source>ApJ</source> <volume>295</volume>, <fpage>305</fpage>&#x2013;<lpage>313</lpage>. <pub-id pub-id-type="doi">10.1086/163375</pub-id>
</citation>
</ref>
<ref id="B171">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>van der Wel</surname>
<given-names>A.</given-names>
</name>
<name>
<surname>Franx</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>van Dokkum</surname>
<given-names>P. G.</given-names>
</name>
<name>
<surname>Skelton</surname>
<given-names>R. E.</given-names>
</name>
<name>
<surname>Momcheva</surname>
<given-names>I. G.</given-names>
</name>
<name>
<surname>Whitaker</surname>
<given-names>K. E.</given-names>
</name>
<etal/>
</person-group> (<year>2014</year>). <article-title>3D-HST&#x2b;CANDELS: The evolution of the galaxy size-mass distribution since z &#x3d; 3</article-title>. <source>ApJ</source> <volume>788</volume>, <fpage>28</fpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/788/1/28</pub-id>
</citation>
</ref>
<ref id="B172">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>van Dokkum</surname>
<given-names>P. G.</given-names>
</name>
<name>
<surname>Franx</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Kriek</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Holden</surname>
<given-names>B.</given-names>
</name>
<name>
<surname>Illingworth</surname>
<given-names>G. D.</given-names>
</name>
<name>
<surname>Magee</surname>
<given-names>D.</given-names>
</name>
<etal/>
</person-group> (<year>2008</year>). <article-title>Confirmation of the remarkable compactness of massive quiescent galaxies at <italic>z</italic> &#x223c; 2.3: Early-type galaxies did not form in a simple monolithic collapse</article-title>. <source>ApJ</source> <volume>677</volume>, <fpage>L5</fpage>&#x2013;<lpage>L8</lpage>. <pub-id pub-id-type="doi">10.1086/587874</pub-id>
</citation>
</ref>
<ref id="B173">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>van Dokkum</surname>
<given-names>P. G.</given-names>
</name>
<name>
<surname>Whitaker</surname>
<given-names>K. E.</given-names>
</name>
<name>
<surname>Brammer</surname>
<given-names>G.</given-names>
</name>
<name>
<surname>Franx</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Kriek</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Labb&#xe9;</surname>
<given-names>I.</given-names>
</name>
<etal/>
</person-group> (<year>2010</year>). <article-title>The growth of massive galaxies since z &#x3d; 2</article-title>. <source>ApJ</source> <volume>709</volume>, <fpage>1018</fpage>&#x2013;<lpage>1041</lpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/709/2/1018</pub-id>
</citation>
</ref>
<ref id="B175">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Vavry&#x10d;uk</surname>
<given-names>V.</given-names>
</name>
</person-group> (<year>2022a</year>). <article-title>Cosmological redshift and cosmic time dilation in the FLRW metric</article-title>. <source>Front. Phys.</source> <volume>10</volume>, <fpage>826188</fpage>. <pub-id pub-id-type="doi">10.3389/fphy.2022.826188</pub-id>
</citation>
</ref>
<ref id="B174">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Vavry&#x10d;uk</surname>
<given-names>V.</given-names>
</name>
</person-group> (<year>2022b</year>). <article-title>Considering light-matter interactions in Friedmann equations based on the conformal FLRW metric</article-title>. <source>J. Adv. Res.</source> <pub-id pub-id-type="doi">10.1016/j.jare.2022.06.015</pub-id>
</citation>
</ref>
<ref id="B176">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Verheijen</surname>
<given-names>M. A. W.</given-names>
</name>
</person-group> (<year>2001</year>). <article-title>The Ursa Major Cluster of galaxies. V. H I rotation curve shapes and the Tully-Fisher relations</article-title>. <source>ApJ</source> <volume>563</volume>, <fpage>694</fpage>&#x2013;<lpage>715</lpage>. <pub-id pub-id-type="doi">10.1086/323887</pub-id>
</citation>
</ref>
<ref id="B177">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Visser</surname>
<given-names>M.</given-names>
</name>
</person-group> (<year>2015</year>). <article-title>Conformally Friedmann-Lema&#xee;tre-Robertson-Walker cosmologies</article-title>. <source>Class. Quantum Gravity</source> <volume>32</volume>, <fpage>135007</fpage>. <pub-id pub-id-type="doi">10.1088/0264-9381/32/13/135007</pub-id>
</citation>
</ref>
<ref id="B178">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Weinberg</surname>
<given-names>D. H.</given-names>
</name>
<name>
<surname>Mortonson</surname>
<given-names>M. J.</given-names>
</name>
<name>
<surname>Eisenstein</surname>
<given-names>D. J.</given-names>
</name>
<name>
<surname>Hirata</surname>
<given-names>C.</given-names>
</name>
<name>
<surname>Riess</surname>
<given-names>A. G.</given-names>
</name>
<name>
<surname>Rozo</surname>
<given-names>E.</given-names>
</name>
</person-group> (<year>2013</year>). <article-title>Observational probes of cosmic acceleration</article-title>. <source>Phys. Rep.</source> <volume>530</volume>, <fpage>87</fpage>&#x2013;<lpage>255</lpage>. <pub-id pub-id-type="doi">10.1016/j.physrep.2013.05.001</pub-id>
</citation>
</ref>
<ref id="B179">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Weinberg</surname>
<given-names>S.</given-names>
</name>
</person-group> (<year>1972</year>). <source>Gravitation and cosmology: Principles and applications of the general theory of relativity</source>. <publisher-loc>New York</publisher-loc>: <publisher-name>John Wiley &#x26; Sons</publisher-name>.</citation>
</ref>
<ref id="B180">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>White</surname>
<given-names>S. D. M.</given-names>
</name>
<name>
<surname>Frenk</surname>
<given-names>C. S.</given-names>
</name>
<name>
<surname>Davis</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>Efstathiou</surname>
<given-names>G.</given-names>
</name>
</person-group> (<year>1987</year>). <article-title>Clusters, filaments, and voids in a universe dominated by cold dark matter</article-title>. <source>ApJ</source> <volume>313</volume>, <fpage>505</fpage>. <pub-id pub-id-type="doi">10.1086/164990</pub-id>
</citation>
</ref>
<ref id="B181">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>White</surname>
<given-names>S. D. M.</given-names>
</name>
<name>
<surname>Rees</surname>
<given-names>M. J.</given-names>
</name>
</person-group> (<year>1978</year>). <article-title>Core condensation in heavy halos: A two-stage theory for galaxy formation and clustering</article-title>. <source>MNRAS</source> <volume>183</volume>, <fpage>341</fpage>&#x2013;<lpage>358</lpage>. <pub-id pub-id-type="doi">10.1093/mnras/183.3.341</pub-id>
</citation>
</ref>
<ref id="B182">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Whitney</surname>
<given-names>A.</given-names>
</name>
<name>
<surname>Conselice</surname>
<given-names>C. J.</given-names>
</name>
<name>
<surname>Bhatawdekar</surname>
<given-names>R.</given-names>
</name>
<name>
<surname>Duncan</surname>
<given-names>K.</given-names>
</name>
</person-group> (<year>2019</year>). <article-title>Unbiased differential size evolution and the inside-out growth of galaxies in the deep CANDELS GOODS fields at 1 &#x2264; z &#x2264; 7</article-title>. <source>ApJ</source> <volume>887</volume>, <fpage>113</fpage>. <pub-id pub-id-type="doi">10.3847/1538-4357/ab53d4</pub-id>
</citation>
</ref>
<ref id="B183">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Williams</surname>
<given-names>R. J.</given-names>
</name>
<name>
<surname>Quadri</surname>
<given-names>R. F.</given-names>
</name>
<name>
<surname>Franx</surname>
<given-names>M.</given-names>
</name>
<name>
<surname>van Dokkum</surname>
<given-names>P.</given-names>
</name>
<name>
<surname>Toft</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>Kriek</surname>
<given-names>M.</given-names>
</name>
<etal/>
</person-group> (<year>2010</year>). <article-title>The evolving relations between size, mass, surface density, and star formation in 3 &#xd7; 10<sup>4</sup> galaxies since z &#x3d; 2</article-title>. <source>ApJ</source> <volume>713</volume>, <fpage>738</fpage>&#x2013;<lpage>750</lpage>. <pub-id pub-id-type="doi">10.1088/0004-637X/713/2/738</pub-id>
</citation>
</ref>
<ref id="B184">
<citation citation-type="book">
<person-group person-group-type="author">
<name>
<surname>Windley</surname>
<given-names>B. F.</given-names>
</name>
</person-group> (<year>1984</year>). <source>The evolving continents/2nd revised and enlarged</source>. <edition>edition/</edition>. <publisher-loc>New York</publisher-loc>: <publisher-name>Wiley</publisher-name>.</citation>
</ref>
<ref id="B185">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Zaritsky</surname>
<given-names>D.</given-names>
</name>
<name>
<surname>Courtois</surname>
<given-names>H.</given-names>
</name>
<name>
<surname>Mu&#xf1;oz-Mateos</surname>
<given-names>J. C.</given-names>
</name>
<name>
<surname>Sorce</surname>
<given-names>J.</given-names>
</name>
<name>
<surname>Erroz-Ferrer</surname>
<given-names>S.</given-names>
</name>
<name>
<surname>Comer&#xf3;n</surname>
<given-names>S.</given-names>
</name>
<etal/>
</person-group> (<year>2014</year>). <article-title>The baryonic Tully-Fisher relationship for S<sup>4</sup>G galaxies and the &#x201c;condensed&#x201d; baryon fraction of galaxies</article-title>. <source>AJ</source> <volume>147</volume>, <fpage>134</fpage>. <pub-id pub-id-type="doi">10.1088/0004-6256/147/6/134</pub-id>
</citation>
</ref>
<ref id="B186">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Zhang</surname>
<given-names>W.</given-names>
</name>
<name>
<surname>Li</surname>
<given-names>Z.</given-names>
</name>
<name>
<surname>Lei</surname>
<given-names>Y.</given-names>
</name>
</person-group> (<year>2010</year>). <article-title>Experimental measurement of growth patterns on fossil corals: Secular variation in ancient Earth-Sun distances</article-title>. <source>Chin. Sci. Bull.</source> <volume>55</volume>, <fpage>4010</fpage>&#x2013;<lpage>4017</lpage>. <pub-id pub-id-type="doi">10.1007/s11434-010-4197-x</pub-id>
</citation>
</ref>
<ref id="B187">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Zwicky</surname>
<given-names>F.</given-names>
</name>
</person-group> (<year>1937</year>). <article-title>On the masses of nebulae and of clusters of nebulae</article-title>. <source>ApJ</source> <volume>86</volume>, <fpage>217</fpage>. <pub-id pub-id-type="doi">10.1086/143864</pub-id>
</citation>
</ref>
<ref id="B188">
<citation citation-type="journal">
<person-group person-group-type="author">
<name>
<surname>Zwicky</surname>
<given-names>F.</given-names>
</name>
</person-group> (<year>2009</year>). <article-title>Republication of: The redshift of extragalactic nebulae</article-title>. <source>General Relativ. Gravit.</source> <volume>41</volume>, <fpage>207</fpage>&#x2013;<lpage>224</lpage>. <pub-id pub-id-type="doi">10.1007/s10714-008-0707-4</pub-id>
</citation>
</ref>
</ref-list>
<app-group>
<app id="app1">
<title>Appendix A Gravitational orbits in the expanding Universe described by the FLRW metric</title>
<p>The metric tensor <italic>g</italic>
<sub>
<italic>&#x3bc;&#x3bd;</italic>
</sub> of a gravitational field produced by a point mass <italic>M</italic> situated in space obeying the FLRW metric reads (<xref ref-type="bibr" rid="B129">Noerdlinger and Petrosian, 1971</xref>, their Eq. 11)<disp-formula id="eA_1">
<mml:math id="m51">
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>s</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2b;</mml:mo>
<mml:mn>2</mml:mn>
<mml:mi>&#x3b1;</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>T</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mi>T</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:mn>2</mml:mn>
<mml:mi>&#x3b1;</mml:mi>
</mml:mrow>
</mml:mfenced>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:mn>1</mml:mn>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>k</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mi>d</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x3a9;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfenced>
<mml:mo>,</mml:mo>
</mml:math>
<label>(A-1)</label>
</disp-formula>where <italic>T</italic> is the proper time and<disp-formula id="eA_2">
<mml:math id="m52">
<mml:mi>&#x3b1;</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>G</mml:mi>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>r</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mi>c</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>,</mml:mo>
<mml:mspace width="0.17em"/>
<mml:mo stretchy="false">&#x7c;</mml:mo>
<mml:mi>&#x3b1;</mml:mi>
<mml:mo stretchy="false">&#x7c;</mml:mo>
<mml:mo>&#x226a;</mml:mo>
<mml:mn>1</mml:mn>
<mml:mo>,</mml:mo>
</mml:math>
<label>(A-2)</label>
</disp-formula>is the Newtonian gravitational potential normalized to <italic>c</italic>
<sup>2</sup>, and <italic>G</italic> is the gravitational constant. Assuming a massive non-relativistic particle (<italic>v</italic> &#x226a; <italic>c</italic>) orbiting in the gravitational field in the plane defined by <italic>&#x3d5;</italic> &#x3d; 0 and calculating the Christoffel symbols <inline-formula id="inf16">
<mml:math id="m53">
<mml:msubsup>
<mml:mrow>
<mml:mi mathvariant="normal">&#x393;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3b1;</mml:mi>
<mml:mi>&#x3b2;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>&#x3bc;</mml:mi>
</mml:mrow>
</mml:msubsup>
</mml:math>
</inline-formula> in the geodesic Eq.&#xa0;<xref ref-type="disp-formula" rid="e9">9</xref>, we get the following approximate equations<disp-formula id="eA_3">
<mml:math id="m54">
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x2212;</mml:mo>
<mml:mi>r</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>G</mml:mi>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>&#x3b1;</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>3</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:mn>2</mml:mn>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>0</mml:mn>
<mml:mo>,</mml:mo>
</mml:math>
<label>(A-3)</label>
</disp-formula>
<disp-formula id="eA_4">
<mml:math id="m55">
<mml:mi>r</mml:mi>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x2b;</mml:mo>
<mml:mn>2</mml:mn>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x2b;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>r</mml:mi>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>0</mml:mn>
<mml:mo>,</mml:mo>
</mml:math>
<label>(A-4)</label>
</disp-formula>where dots over quantities mean derivatives with respect to time <italic>T</italic>. Inserting the proper distance <italic>R</italic> &#x3d; <italic>a</italic>(<italic>T</italic>)<italic>r</italic> into Eq.&#xa0;<xref ref-type="disp-formula" rid="eA_3">A-3</xref> we get<disp-formula id="eA_5">
<mml:math id="m56">
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>G</mml:mi>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:mi>R</mml:mi>
<mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mo>&#x2b;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>R</mml:mi>
<mml:mo>.</mml:mo>
</mml:math>
<label>(A-5)</label>
</disp-formula>Similarly, Eq.&#xa0;<xref ref-type="disp-formula" rid="eA_4">A-4</xref> can be rewritten as<disp-formula id="eA_6">
<mml:math id="m57">
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>T</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:msup>
<mml:mrow>
<mml:mi>r</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>T</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mfenced open="(" close=")">
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>&#x3d5;</mml:mi>
</mml:mrow>
<mml:mo>&#x307;</mml:mo>
</mml:mover>
</mml:mrow>
</mml:mrow>
</mml:mfenced>
<mml:mo>&#x3d;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>d</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mi>d</mml:mi>
<mml:mi>T</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>L</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mn>0</mml:mn>
<mml:mo>,</mml:mo>
</mml:math>
<label>(A-6)</label>
</disp-formula>where <italic>L</italic> &#x3d; <italic>RV</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> is the proper angular momentum, and <italic>V</italic>
<sup>
<italic>&#x3d5;</italic>
</sup> is the proper tangential velocity. Consequently, we can write (<xref ref-type="bibr" rid="B27">Carrera and Giulini, 2010</xref>, their Eq.&#xa0;12a,&#xa0;b)<disp-formula id="eA_7">
<mml:math id="m58">
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mo>&#x3d;</mml:mo>
<mml:mo>&#x2212;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mi>G</mml:mi>
<mml:mi>M</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>L</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>2</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
<mml:mrow>
<mml:msup>
<mml:mrow>
<mml:mi>R</mml:mi>
</mml:mrow>
<mml:mrow>
<mml:mn>3</mml:mn>
</mml:mrow>
</mml:msup>
</mml:mrow>
</mml:mfrac>
<mml:mo>&#x2b;</mml:mo>
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>R</mml:mi>
<mml:mo>,</mml:mo>
</mml:math>
<label>(A-7)</label>
</disp-formula>
<disp-formula id="eA_8">
<mml:math id="m59">
<mml:mi>L</mml:mi>
<mml:mo>&#x3d;</mml:mo>
<mml:mi mathvariant="normal">c</mml:mi>
<mml:mi mathvariant="normal">o</mml:mi>
<mml:mi mathvariant="normal">n</mml:mi>
<mml:mi mathvariant="normal">s</mml:mi>
<mml:mi mathvariant="normal">t</mml:mi>
<mml:mo>.</mml:mo>
</mml:math>
<label>(A-8)</label>
</disp-formula>The equations are called the modified Newtonian equations and they differ from the standard Newtonian equations describing the Kepler orbits by term <inline-formula id="inf17">
<mml:math id="m60">
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>R</mml:mi>
</mml:math>
</inline-formula> in Eq.&#xa0;<xref ref-type="disp-formula" rid="eA_7">A-7</xref> related to the space expansion. The analysis of the modified Newtonian equations applied to the galaxy dynamics shows that assuming a constant <italic>L</italic>, the expansion term <inline-formula id="inf18">
<mml:math id="m61">
<mml:mfrac>
<mml:mrow>
<mml:mover accent="true">
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
<mml:mo>&#x308;</mml:mo>
</mml:mover>
</mml:mrow>
<mml:mrow>
<mml:mi>a</mml:mi>
</mml:mrow>
</mml:mfrac>
<mml:mi>R</mml:mi>
</mml:math>
</inline-formula> affects the orbits within galaxies negligibly (<xref ref-type="bibr" rid="B54">Faraoni and Jacques, 2007</xref>).</p>
</app>
</app-group>
</back>
</article>