<?xml version="1.0" encoding="UTF-8"?><!DOCTYPE article PUBLIC "-//NLM//DTD Journal Publishing DTD v3.0 20080202//EN" "http://dtd.nlm.nih.gov/publishing/3.0/journalpublishing3.dtd">
<article xmlns:mml="http://www.w3.org/1998/Math/MathML" xmlns:xlink="http://www.w3.org/1999/xlink" dtd-version="3.0" xml:lang="en" article-type="research article">
 <front>
  <journal-meta>
   <journal-id journal-id-type="publisher-id">
    jmp
   </journal-id>
   <journal-title-group>
    <journal-title>
     Journal of Modern Physics
    </journal-title>
   </journal-title-group>
   <issn pub-type="epub">
    2153-1196
   </issn>
   <issn publication-format="print">
    2153-120X
   </issn>
   <publisher>
    <publisher-name>
     Scientific Research Publishing
    </publisher-name>
   </publisher>
  </journal-meta>
  <article-meta>
   <article-id pub-id-type="doi">
    10.4236/jmp.2024.1512090
   </article-id>
   <article-id pub-id-type="publisher-id">
    jmp-137302
   </article-id>
   <article-categories>
    <subj-group subj-group-type="heading">
     <subject>
      Articles
     </subject>
    </subj-group>
    <subj-group subj-group-type="Discipline-v2">
     <subject>
      Physics 
     </subject>
     <subject>
       Mathematics
     </subject>
    </subj-group>
   </article-categories>
   <title-group>
    Time Dilation Cosmology 3: Mathematical Proof of the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
        3
       </mn> 
      </msqrt> 
     </mrow> 
    </math> Temporal and 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
        2
       </mn> 
      </msqrt> 
     </mrow> 
    </math> Spatial Acceleration Factors
   </title-group>
   <contrib-group>
    <contrib contrib-type="author" xlink:type="simple">
     <name name-style="western">
      <surname>
       Joseph H. Cass
      </surname>
      <given-names>
       Forrington
      </given-names>
     </name>
    </contrib>
   </contrib-group> 
   <aff id="affnull">
    <addr-line>
     aManaging Editor, Journal of Cosmology, California, USA
    </addr-line> 
   </aff> 
   <pub-date pub-type="epub">
    <day>
     01
    </day> 
    <month>
     11
    </month>
    <year>
     2024
    </year>
   </pub-date> 
   <volume>
    15
   </volume> 
   <issue>
    12
   </issue>
   <fpage>
    2228
   </fpage>
   <lpage>
    2237
   </lpage>
   <history>
    <date date-type="received">
     <day>
      8,
     </day>
     <month>
      October
     </month>
     <year>
      2024
     </year>
    </date>
    <date date-type="published">
     <day>
      9,
     </day>
     <month>
      October
     </month>
     <year>
      2024
     </year> 
    </date> 
    <date date-type="accepted">
     <day>
      9,
     </day>
     <month>
      November
     </month>
     <year>
      2024
     </year> 
    </date>
   </history>
   <permissions>
    <copyright-statement>
     © Copyright 2014 by authors and Scientific Research Publishing Inc. 
    </copyright-statement>
    <copyright-year>
     2014
    </copyright-year>
    <license>
     <license-p>
      This work is licensed under the Creative Commons Attribution International License (CC BY). http://creativecommons.org/licenses/by/4.0/
     </license-p>
    </license>
   </permissions>
   <abstract>
    This is the fifth paper in a series on Time Dilation Cosmology, TDC. TDC is an eternal holographic model of the universe based on time dilation that ties astrophysics to quantum physics and resolves all the conundrums in astrophysics and serves as a model for the unified field. In the author’s previous four TDC papers, it was demonstrated that all gravitationally induced velocities are compensation for the apparent difference in the rates of time, “dRt”, due to mass/energy densities, and, vice-versa, in all force-induced velocities the dRt is compensation for the velocity, so the uniform evolution of the continuum at c is maintained at the invariant 1 s/s rate of time of the universe as a whole. These compensations make it impossible for an event to lag behind or get ahead of the evolving continuum. When the author did the first velocity formula derivations in “General Relativity: Effects in Time as Causation” [1], the author felt the explanations for the appearance of the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
        2
       </mn> 
      </msqrt> 
     </mrow> 
    </math> spatial and the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
        3
       </mn> 
      </msqrt> 
     </mrow> 
    </math> temporal acceleration factors in the formulas were correct, but poorly explained and incomplete. This paper is a proof of the temporal and spatial acceleration factors used in the time dilation-based velocity formula derivations in the Time Dilation Cosmology model.
   </abstract>
   <kwd-group> 
    <kwd>
     Mathematical Proof
    </kwd> 
    <kwd>
      Time Dilation Cosmology
    </kwd> 
    <kwd>
      Acceleration Factors
    </kwd>
   </kwd-group>
  </article-meta>
 </front>
 <body>
  <sec id="s1">
   <title>1. Introduction</title>
   <p>
    <xref ref-type="bibr" rid="scirp.137302-"></xref>As of this writing, the author has been advised that most of the PHD students in at least one prominent university are now being introduced to this model of the universe and download patterns indicate multiple universities are now following suit.</p>
   <p>This is the fifth paper in a series on Time Dilation Cosmology, TDC. TDC is an eternal holographic model of the universe based on time dilation. The reader should not expect it to be part of the Lamda/CDM/Big Bang, General Relativity, fixed space models. It is a spacetime/quantum continuum evolving forward at the speed of light, c, in the forward direction of time. It is a universe of light, not rock. It is strongly suggested the first-time reader refer to the author’s previous papers to clarify concepts when necessary.</p>
   <p>In the TDC model, there are two forward directions of evolution, the Fundamental Direction of Evolution, FDE, which is in the forward direction of time, and the Gravitational Direction of Evolution, GDE, which is the evolution down time dilation gradients due to differences in the rate of time. Time is the force behind these evolutions and that force is gravity, the irresistible evolutionary force of time.</p>
   <p>In the author’s previous four TDC papers <xref ref-type="bibr" rid="scirp.137302-1">
     [1]
    </xref>-<xref ref-type="bibr" rid="scirp.137302-4">
     [4]
    </xref>, it was demonstrated that all gravitationally induced velocities are compensation for the apparent difference in the rates of time, “dRt”, due to mass/energy densities, and, vice-versa, in all force-induced velocities the dRt is compensation for the velocity, so the uniform evolution of the continuum at c is maintained at the invariant 1 s/s rate of time of the universe as a whole.</p>
   <p>When the author did the first formula derivations in “General Relativity: Effects in Time as Causation” <xref ref-type="bibr" rid="scirp.137302-1">
     [1]
    </xref>, the author felt the explanations for the appearance of the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> spatial and the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         3 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> temporal acceleration factors in the formulas were correct, but poorly explained and incomplete. This paper is a proof of both acceleration factors.</p>
  </sec><sec id="s2">
   <title>2. The Lorentz and Schwarzschild-Based Formulas</title>
   <p>Since the publication of “The Unified Field”<xref ref-type="bibr" rid="scirp.137302-4">
     [4]
    </xref>, the author has been looking at different aspects arising from that paper that led back to the Lorentz factor and the Lorentz formula for time dilation:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msup> 
       <mi>
         t 
       </mi> 
       <mo>
         ′ 
       </mo> 
      </msup> 
      <mo>
        = 
      </mo> 
      <mrow> 
       <mi>
         T 
       </mi> 
       <mo>
         / 
       </mo> 
       <mrow> 
        <msqrt> 
         <mrow> 
          <mn>
            1 
          </mn> 
          <mo>
            − 
          </mo> 
          <mrow> 
           <mrow> 
            <msup> 
             <mi>
               v 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
           </mrow> 
           <mo>
             / 
           </mo> 
           <mrow> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
           </mrow> 
          </mrow> 
         </mrow> 
        </msqrt> 
       </mrow> 
      </mrow> 
     </mrow> 
    </math> (1)</p>
   <p>Note that the velocity can be derived directly from this equation without the use of the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> or 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         3 
       </mn> 
      </msqrt> 
     </mrow> 
    </math>:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        v 
      </mi> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <msqrt> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          − 
        </mo> 
        <msup> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mrow> 
             <mi>
               T 
             </mi> 
             <mo>
               / 
             </mo> 
             <msup> 
              <mi>
                t 
              </mi> 
              <mo>
                ′ 
              </mo> 
             </msup> 
            </mrow> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> (2)</p>
   <p>Also, note that:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msup> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mfrac> 
           <mi>
             T 
           </mi> 
           <msup> 
            <mi>
              t 
            </mi> 
            <mo>
              ′ 
            </mo> 
           </msup> 
          </mfrac> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mn>
         2 
       </mn> 
      </msup> 
      <mo>
        = 
      </mo> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mi>
         o 
       </mi> 
      </msub> 
     </mrow> 
    </math> (3)</p>
   <p>where T<sub>o</sub> is the time dilation factor derived by the Schwarzschild radius-based time dilation formula used in the original derivations in <xref ref-type="bibr" rid="scirp.137302-1">
     [1]
    </xref> as follows.</p>
   <p>In the Schwarzschild metric, since orbital velocity,</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         V 
       </mi> 
       <mi>
         o 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msqrt> 
       <mrow> 
        <mfrac> 
         <mrow> 
          <mi>
            G 
          </mi> 
          <mi>
            M 
          </mi> 
         </mrow> 
         <mi>
           R 
         </mi> 
        </mfrac> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math>, (4)</p>
   <p>the time dilation formulas for orbital velocities are derived from the gravitational time dilation formula,</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mi>
         o 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        T 
      </mi> 
      <msqrt> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          − 
        </mo> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mrow> 
           <mrow> 
            <mn>
              2 
            </mn> 
            <mi>
              G 
            </mi> 
            <mi>
              M 
            </mi> 
           </mrow> 
           <mo>
             / 
           </mo> 
           <mrow> 
            <mi>
              R 
            </mi> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
           </mrow> 
          </mrow> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math>, (5)</p>
   <p>which contains the velocity formula elements within it, by substituting V<sub>o</sub> for GM/R, i.e.:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mi>
         o 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        T 
      </mi> 
      <msqrt> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          − 
        </mo> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mrow> 
           <mn>
             2 
           </mn> 
           <mo>
             / 
           </mo> 
           <mrow> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
           </mrow> 
          </mrow> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
        <msub> 
         <mi>
           V 
         </mi> 
         <mi>
           o 
         </mi> 
        </msub> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> (6)</p>
   <p>resulting in:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         V 
       </mi> 
       <mrow> 
        <mi>
          o 
        </mi> 
        <mi>
          p 
        </mi> 
       </mrow> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
      <mo>
        ∗ 
      </mo> 
      <msqrt> 
       <mrow> 
        <mrow> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mi>
              T 
            </mi> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
            <mo> 
            </mo> 
            <mo>
              – 
            </mo> 
            <mo> 
            </mo> 
            <msub> 
             <mi>
               T 
             </mi> 
             <mi>
               o 
             </mi> 
            </msub> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mo>
           / 
         </mo> 
         <mrow> 
          <mn>
            2 
          </mn> 
          <mi>
            T 
          </mi> 
         </mrow> 
        </mrow> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> (7)</p>
   <p>for nearly circular orbital velocities, where T = 1 is the distant observer’s invariant rate of universal time, T<sub>0</sub> is the rate of time of the coordinate point, and 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> is the spatial acceleration factor. Since T = 1, this formula reduces to:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         V 
       </mi> 
       <mrow> 
        <mi>
          o 
        </mi> 
        <mi>
          p 
        </mi> 
       </mrow> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msqrt> 
       <mrow> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mn>
            1 
          </mn> 
          <mo>
            − 
          </mo> 
          <msub> 
           <mi>
             T 
           </mi> 
           <mi>
             o 
           </mi> 
          </msub> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> (8)</p>
   <p>And, where “dRt” = the difference in the rate of time between the invariant 1 s/s rate of the universe as a whole and the coordinate point,</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mn>
        1 
      </mn> 
      <mo>
        − 
      </mo> 
      <msub> 
       <mi>
         T 
       </mi> 
       <mi>
         o 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        d 
      </mi> 
      <mi>
        R 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> (9)</p>
   <p>so, we end up with:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         V 
       </mi> 
       <mrow> 
        <mi>
          o 
        </mi> 
        <mi>
          p 
        </mi> 
       </mrow> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <msqrt> 
       <mrow> 
        <mi>
          d 
        </mi> 
        <mi>
          R 
        </mi> 
        <mi>
          t 
        </mi> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> (10)</p>
   <p>for objects in nearly circular orbits.</p>
   <p>So, where did the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> acceleration factor come from? Since the gravitationally induced velocities are compensation for the slower rates of time at the coordinate point, there has to be an acceleration inducing the velocities and the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> is a component of Einstein’s Fundamental Metric, wherein X, Y, Z and T all equal 1, as in <xref ref-type="fig" rid="fig1">
     Figure 1
    </xref>.</p>
   <p>If we look at (6) again, we see that V<sub>o</sub> = GM/R, but GM/R is not the velocity; 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mrow> 
        <mrow> 
         <mrow> 
          <mi>
            G 
          </mi> 
          <mi>
            M 
          </mi> 
         </mrow> 
         <mo>
           / 
         </mo> 
         <mi>
           R 
         </mi> 
        </mrow> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> is. So if we look at (7) again, but without the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math>, V<sub>op</sub> should equal v<sup>2</sup>:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         V 
       </mi> 
       <mrow> 
        <mi>
          o 
        </mi> 
        <mi>
          p 
        </mi> 
       </mrow> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msqrt> 
       <mrow> 
        <mrow> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mi>
              T 
            </mi> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
            <mo> 
            </mo> 
            <mo>
              – 
            </mo> 
            <mo> 
            </mo> 
            <msub> 
             <mi>
               T 
             </mi> 
             <mi>
               o 
             </mi> 
            </msub> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mo>
           / 
         </mo> 
         <mrow> 
          <mn>
            2 
          </mn> 
          <mi>
            T 
          </mi> 
         </mrow> 
        </mrow> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> (11)</p>
   <p>But when we solve it for the Earth, when T = 1, we get:</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mtable> 
      <mtr> 
       <mtd> 
        <msub> 
         <mi>
           V 
         </mi> 
         <mrow> 
          <mi>
            o 
          </mi> 
          <mi>
            p 
          </mi> 
         </mrow> 
        </msub> 
        <mo>
          = 
        </mo> 
        <msqrt> 
         <mrow> 
          <mrow> 
           <mrow> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
            <mrow> 
             <mo>
               ( 
             </mo> 
             <mrow> 
              <mn>
                1 
              </mn> 
              <mo>
                − 
              </mo> 
              <msub> 
               <mi>
                 T 
               </mi> 
               <mi>
                 o 
               </mi> 
              </msub> 
             </mrow> 
             <mo>
               ) 
             </mo> 
            </mrow> 
           </mrow> 
           <mo>
             / 
           </mo> 
           <mn>
             2 
           </mn> 
          </mrow> 
         </mrow> 
        </msqrt> 
        <mo>
          = 
        </mo> 
        <msqrt> 
         <mrow> 
          <msup> 
           <mrow> 
            <mn>
              299792.458 
            </mn> 
           </mrow> 
           <mn>
             2 
           </mn> 
          </msup> 
          <mrow> 
           <mrow> 
            <mrow> 
             <mo>
               ( 
             </mo> 
             <mrow> 
              <mn>
                0.0000000098706030 
              </mn> 
             </mrow> 
             <mo>
               ) 
             </mo> 
            </mrow> 
           </mrow> 
           <mo>
             / 
           </mo> 
           <mn>
             2 
           </mn> 
          </mrow> 
         </mrow> 
        </msqrt> 
       </mtd> 
      </mtr> 
      <mtr> 
       <mtd> 
        <mo>
          = 
        </mo> 
        <mn>
          21.06 
        </mn> 
        <mtext>
            
        </mtext> 
        <mrow> 
         <mrow> 
          <mtext>
            km 
          </mtext> 
         </mrow> 
         <mo>
           / 
         </mo> 
         <mtext>
           s 
         </mtext> 
        </mrow> 
       </mtd> 
      </mtr> 
     </mtable> 
    </math> (12)</p>
   <p>and taking the square root of this result does not get us the velocity. Only multiplying it by the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> acceleration factor gives us the correct answer.</p>
   <p>We can understand the source of 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> more plainly in the galactic rotation velocity formula derivation, where it is the denominator in the secant y/x in <xref ref-type="fig" rid="fig1">
     Figure 1
    </xref>.</p>
   <fig id="fig1" position="float">
    <label>Figure 1</label>
    <caption>
     <title>Figure 1. Einstein’s fundamental metric.</title>
    </caption>
    <graphic mimetype="image" position="float" xlink:type="simple" xlink:href="https://html.scirp.org/file/7505456-rId78.jpeg?20241112105328" />
   </fig>
   <p>Assigning 1 unit of length for each side and assuming 1 unit of time, we see that y = 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         3 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> and x = 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math>, and we find that using</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         V 
       </mi> 
       <mrow> 
        <mi>
          o 
        </mi> 
        <mi>
          g 
        </mi> 
       </mrow> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <msqrt> 
         <mrow> 
          <mfrac> 
           <mrow> 
            <mi>
              T 
            </mi> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
            <mo>
              – 
            </mo> 
            <msub> 
             <mi>
               T 
             </mi> 
             <mi>
               o 
             </mi> 
            </msub> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
           </mrow> 
           <mrow> 
            <mn>
              2 
            </mn> 
            <mi>
              T 
            </mi> 
           </mrow> 
          </mfrac> 
         </mrow> 
        </msqrt> 
       </mrow> 
       <mrow> 
        <mfrac> 
         <mrow> 
          <msqrt> 
           <mn>
             3 
           </mn> 
          </msqrt> 
         </mrow> 
         <mrow> 
          <msqrt> 
           <mn>
             2 
           </mn> 
          </msqrt> 
         </mrow> 
        </mfrac> 
       </mrow> 
      </mfrac> 
      <mo>
        = 
      </mo> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
      <mo>
        ∗ 
      </mo> 
      <mrow> 
       <mrow> 
        <msqrt> 
         <mrow> 
          <mrow> 
           <mrow> 
            <mrow> 
             <mo>
               ( 
             </mo> 
             <mrow> 
              <mi>
                T 
              </mi> 
              <msup> 
               <mi>
                 c 
               </mi> 
               <mn>
                 2 
               </mn> 
              </msup> 
              <mo>
                − 
              </mo> 
              <msub> 
               <mi>
                 T 
               </mi> 
               <mi>
                 o 
               </mi> 
              </msub> 
              <msup> 
               <mi>
                 c 
               </mi> 
               <mn>
                 2 
               </mn> 
              </msup> 
             </mrow> 
             <mo>
               ) 
             </mo> 
            </mrow> 
           </mrow> 
           <mo>
             / 
           </mo> 
           <mrow> 
            <mn>
              2 
            </mn> 
            <mi>
              T 
            </mi> 
           </mrow> 
          </mrow> 
         </mrow> 
        </msqrt> 
       </mrow> 
       <mo>
         / 
       </mo> 
       <mrow> 
        <msqrt> 
         <mn>
           3 
         </mn> 
        </msqrt> 
       </mrow> 
      </mrow> 
      <mo>
        , 
      </mo> 
     </mrow> 
    </math> (13)</p>
   <p>and using the Sun’s surface time dilation factor, T<sub>o</sub>, gives us the actual rotational velocity of 230.94 Km/s for the Sun. (The 0.9999982197599103142 dilation factor is for a radius of 8.22428833 * 10<sup>8</sup> m, which is 1.27192 * 10<sup>8</sup> m = 0.00018 of the radius above the surface of the Sun. The author believes this is acceptable considering the Sun’s dynamic nature and varying densities within its mass.)</p>
   <p>Note that it is necessary to divide by the secant, 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mrow> 
       <mrow> 
        <msqrt> 
         <mn>
           3 
         </mn> 
        </msqrt> 
       </mrow> 
       <mo>
         / 
       </mo> 
       <mrow> 
        <msqrt> 
         <mn>
           2 
         </mn> 
        </msqrt> 
       </mrow> 
      </mrow> 
     </mrow> 
    </math>, of the angle of the fundamental direction of evolution, FDE, along y, to obtain the correct result and that this introduces the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> as the spatial acceleration factor, as in the V<sub>op</sub> formula derivation.</p>
   <p>The reason the acceleration factors are not needed in deriving the velocities using the Lorentz time dilation formula, is that it is based solely on the velocities to begin with and those velocities already include the acceleration factors. As the dRt is unique to each velocity and since both the Lorentz and Schwarzschild formulas derive the same dRt, they must also derive the same velocity. The only way to get the same result is to divide by the secant containing both acceleration factors. This necessary scaling using the secant is proof of the validity of both the temporal 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         3 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> and spatial 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> acceleration factors.</p>
   <p>This is also a proof that the cube in <xref ref-type="fig" rid="fig1">
     Figure 1
    </xref> is a more complete model of the Fundamental Metric that includes the fundamental direction and acceleration factor of time and the spatial acceleration factor.</p>
   <p>The validity is demonstrated by how the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         3 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> scales back the velocity in the FDE, which includes the acceleration components, so it is evenly distributed in the 3 spatial dimensions.</p>
   <p>The V<sub>op</sub> formula gives us a result of 400 Km/s for the Sun. When we divide by the 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         3 
       </mn> 
      </msqrt> 
     </mrow> 
    </math> we get 230.94 Km/s. That is the same as proportioning the velocity in the forward direction of time between the 3 spatial dimensions. The proportion of the length of y to the sides is 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mrow> 
       <mrow> 
        <msqrt> 
         <mn>
           3 
         </mn> 
        </msqrt> 
       </mrow> 
       <mo>
         / 
       </mo> 
       <mn>
         1 
       </mn> 
      </mrow> 
     </mrow> 
    </math>.</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mfrac> 
       <mrow> 
        <msqrt> 
         <mn>
           3 
         </mn> 
        </msqrt> 
       </mrow> 
       <mn>
         3 
       </mn> 
      </mfrac> 
      <mo>
        = 
      </mo> 
      <mo> 
      </mo> 
      <mn>
        0.5773502691896257667 
      </mn> 
     </mrow> 
    </math> (14)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mn>
        0.5773502691896257667 
      </mn> 
      <mo>
        ∗ 
      </mo> 
      <mn>
        400 
      </mn> 
      <mo>
        = 
      </mo> 
      <mn>
        230.94 
      </mn> 
     </mrow> 
    </math> (15)</p>
   <p>The difference between the planets and the Sun is that the planets’ velocities are relative to the Sun and the Sun’s dilation gradient in the plane of the ecliptic and their velocities are part of a system evolving forward as a whole. As noted in Appendix A, when we also consider the velocity of the system, in this case relative to the Cosmic Microwave Background, CMB, the helical distances travelled by the planets give them velocities equal to the Sun on the grander scale.</p>
   <p>The Sun, however, is outside the dominance of the galactic dilation gradient and not a part of the system like the stars inside the Keplar Zone and the planets in stellar systems. The gravitational direction of evolution, GDE, is still acting perpendicular to the FDE, curving the Sun’s orbit around the galactic center, <xref ref-type="fig" rid="fig2">
     Figure 2
    </xref>, but its own dilation factor is determining its velocity in the FDE.</p>
   <fig id="fig2" position="float">
    <label>Figure 2</label>
    <caption>
     <title>Figure 2. The GDE Bending the FDE.</title>
    </caption>
    <graphic mimetype="image" position="float" xlink:type="simple" xlink:href="https://html.scirp.org/file/7505456-rId103.jpeg?20241112105328" />
   </fig>
   <p>Again, looking at <xref ref-type="fig" rid="fig1">
     Figure 1
    </xref>, y is the Fundamental Direction of Evolution. The planets appear accelerated in the spatial planes of the ecliptic at 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math>, which is x. The stellar system as a whole, centered on the Sun, is also being accelerated by a factor of 
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         2 
       </mn> 
      </msqrt> 
     </mrow> 
    </math>, but it is along y, in the FDE, so the planetary result is divided by 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msqrt> 
       <mn>
         3 
       </mn> 
      </msqrt> 
     </mrow> 
    </math>. This keeps the planets in the same plane of evolution as the Sun and is the apparent velocity in the x,y,z dimensions.</p>
   <p>Further reducing formula (11), we get;</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         V 
       </mi> 
       <mrow> 
        <mi>
          o 
        </mi> 
        <mi>
          g 
        </mi> 
       </mrow> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mrow> 
       <mrow> 
        <mi>
          c 
        </mi> 
        <msqrt> 
         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
         </mrow> 
        </msqrt> 
       </mrow> 
       <mo>
         / 
       </mo> 
       <mrow> 
        <msqrt> 
         <mn>
           3 
         </mn> 
        </msqrt> 
       </mrow> 
      </mrow> 
     </mrow> 
    </math> (16)</p>
   <p>for bodies whose own dilation factors are determining their velocities.</p>
  </sec><sec id="s3">
   <title>3. Time Dilation-Based Formulas</title>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         V 
       </mi> 
       <mrow> 
        <mi>
          C 
        </mi> 
        <mi>
          o 
        </mi> 
       </mrow> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mi>
        c 
      </mi> 
      <msqrt> 
       <mrow> 
        <mi>
          d 
        </mi> 
        <mi>
          R 
        </mi> 
        <mi>
          t 
        </mi> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> for simple, nearly circular, orbits within a Kepler Zone. (17)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         V 
       </mi> 
       <mrow> 
        <mi>
          E 
        </mi> 
        <mi>
          o 
        </mi> 
       </mrow> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msqrt> 
       <mrow> 
        <mn>
          2 
        </mn> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
        <mo>
          − 
        </mo> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
          <mi>
            α 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> for elliptical orbits within a Kepler Zone. (18)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         V 
       </mi> 
       <mrow> 
        <mi>
          G 
        </mi> 
        <mi>
          o 
        </mi> 
       </mrow> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mrow> 
       <mrow> 
        <mi>
          c 
        </mi> 
        <msqrt> 
         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
         </mrow> 
        </msqrt> 
       </mrow> 
       <mo>
         / 
       </mo> 
       <mrow> 
        <msqrt> 
         <mn>
           3 
         </mn> 
        </msqrt> 
       </mrow> 
      </mrow> 
     </mrow> 
    </math> for galactic rotation velocities for stars outside the Kepler Zone. This is the fundamental compensatory velocity formula. (19)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         F 
       </mi> 
       <mi>
         T 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <msup> 
       <mi>
         c 
       </mi> 
       <mn>
         2 
       </mn> 
      </msup> 
      <mo>
        ∗ 
      </mo> 
      <mi>
        d 
      </mi> 
      <mi>
        R 
      </mi> 
      <mi>
        t 
      </mi> 
     </mrow> 
    </math> for the force of time in Newtons in the FDE. (20)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        E 
      </mi> 
      <mo>
        = 
      </mo> 
      <mi>
        m 
      </mi> 
      <msup> 
       <mi>
         c 
       </mi> 
       <mn>
         2 
       </mn> 
      </msup> 
      <msqrt> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          + 
        </mo> 
        <mi>
          d 
        </mi> 
        <mi>
          R 
        </mi> 
        <mi>
          t 
        </mi> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> for Einstein’s energy formula. (21)</p>
   <p>
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        E 
      </mi> 
      <mo>
        = 
      </mo> 
      <mi>
        m 
      </mi> 
      <msup> 
       <mi>
         c 
       </mi> 
       <mn>
         2 
       </mn> 
      </msup> 
      <mrow> 
       <mo>
         ( 
       </mo> 
       <mrow> 
        <mn>
          1 
        </mn> 
        <mo>
          + 
        </mo> 
        <mi>
          d 
        </mi> 
        <mi>
          R 
        </mi> 
        <mi>
          t 
        </mi> 
       </mrow> 
       <mo>
         ) 
       </mo> 
      </mrow> 
     </mrow> 
    </math> for charged elementary particles. (22)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        F 
      </mi> 
      <mo>
        = 
      </mo> 
      <mrow> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mi>
            m 
          </mi> 
          <msup> 
           <mi>
             c 
           </mi> 
           <mn>
             2 
           </mn> 
          </msup> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mo>
         / 
       </mo> 
       <mi>
         r 
       </mi> 
      </mrow> 
     </mrow> 
    </math> for centripetal force &amp; gravity. (23)</p>
   <p>
    <xref ref-type="bibr" rid="scirp.137302-"></xref> 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        F 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mi>
            M 
          </mi> 
          <mi>
            m 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
        <msub> 
         <mi>
           r 
         </mi> 
         <mn>
           1 
         </mn> 
        </msub> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <msub> 
         <mi>
           M 
         </mi> 
         <mo>
           ⊙ 
         </mo> 
        </msub> 
        <msup> 
         <mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <msub> 
             <mi>
               r 
             </mi> 
             <mn>
               2 
             </mn> 
            </msub> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mn>
           2 
         </mn> 
        </msup> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> for the force in Newton’s for 2-body systems. (24)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        F 
      </mi> 
      <mo>
        = 
      </mo> 
      <mrow> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
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          <mi>
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          <mi>
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         <mo>
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        </mrow> 
        <msub> 
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         </mi> 
         <mi>
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        </msub> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mrow> 
         <mo>
           ( 
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         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <msub> 
           <mi>
             t 
           </mi> 
           <mi>
             E 
           </mi> 
          </msub> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mo>
         / 
       </mo> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <msub> 
           <mi>
             M 
           </mi> 
           <mo>
             ⊙ 
           </mo> 
          </msub> 
          <msup> 
           <mrow> 
            <mrow> 
             <mo>
               ( 
             </mo> 
             <mrow> 
              <mi>
                R 
              </mi> 
              <mi>
                M 
              </mi> 
             </mrow> 
             <mo>
               ) 
             </mo> 
            </mrow> 
           </mrow> 
           <mn>
             2 
           </mn> 
          </msup> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
      </mrow> 
     </mrow> 
    </math> for a 3-body solution for the force in Newton’s for 2-body systems, in this case Earth, Moon and Sun. (25)</p>
   <p>
    <xref ref-type="bibr" rid="scirp.137302-"></xref> 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <msub> 
       <mi>
         M 
       </mi> 
       <mi>
         � 
       </mi> 
      </msub> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mrow> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mi>
            R 
          </mi> 
          <mo>
            – 
          </mo> 
          <msub> 
           <mi>
             T 
           </mi> 
           <mn>
             0 
           </mn> 
          </msub> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mi>
         G 
       </mi> 
      </mfrac> 
     </mrow> 
    </math> for the mass inside a stellar circle. (26)</p>
   <p>
    <xref ref-type="bibr" rid="scirp.137302-"></xref> 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        G 
      </mi> 
      <mo>
        = 
      </mo> 
      <mrow> 
       <mrow> 
        <mi>
          r 
        </mi> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mo>
         / 
       </mo> 
       <mi>
         M 
       </mi> 
      </mrow> 
     </mrow> 
    </math> for the empirical gravitational constant. (27)</p>
   <p>
    <xref ref-type="bibr" rid="scirp.137302-"></xref> 
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mfrac> 
       <mi>
         M 
       </mi> 
       <mi>
         R 
       </mi> 
      </mfrac> 
      <mo>
        = 
      </mo> 
      <mrow> 
       <mrow> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mrow> 
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         <mrow> 
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            1 
          </mn> 
          <mo>
            − 
          </mo> 
          <msup> 
           <mrow> 
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               ( 
             </mo> 
             <mrow> 
              <mn>
                1 
              </mn> 
              <mo>
                − 
              </mo> 
              <mfrac> 
               <mrow> 
                <mn>
                  3 
                </mn> 
                <mo>
                  ∗ 
                </mo> 
                <msup> 
                 <mrow> 
                  <mrow> 
                   <mo>
                     ( 
                   </mo> 
                   <mrow> 
                    <msub> 
                     <mi>
                       V 
                     </mi> 
                     <mrow> 
                      <mi>
                        G 
                      </mi> 
                      <mi>
                        o 
                      </mi> 
                     </mrow> 
                    </msub> 
                   </mrow> 
                   <mo>
                     ) 
                   </mo> 
                  </mrow> 
                 </mrow> 
                 <mn>
                   2 
                 </mn> 
                </msup> 
               </mrow> 
               <mrow> 
                <msup> 
                 <mi>
                   c 
                 </mi> 
                 <mn>
                   2 
                 </mn> 
                </msup> 
               </mrow> 
              </mfrac> 
             </mrow> 
             <mo>
               ) 
             </mo> 
            </mrow> 
           </mrow> 
           <mn>
             2 
           </mn> 
          </msup> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mo>
         / 
       </mo> 
       <mrow> 
        <mn>
          2 
        </mn> 
        <mi>
          G 
        </mi> 
       </mrow> 
      </mrow> 
     </mrow> 
    </math> for the Mass/Radius ratio of stars outside the Kepler Zone in spiral galaxies. (28)</p>
   <p>
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        H 
      </mi> 
      <mo>
        = 
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      <mstyle displaystyle="true"> 
       <msub> 
        <mo>
          ∑ 
        </mo> 
        <mi>
          i 
        </mi> 
       </msub> 
       <mrow> 
        <mfrac> 
         <mrow> 
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           <mo>
             ( 
           </mo> 
           <mrow> 
            <msub> 
             <mi>
               m 
             </mi> 
             <mi>
               i 
             </mi> 
            </msub> 
            <msup> 
             <mi>
               c 
             </mi> 
             <mn>
               2 
             </mn> 
            </msup> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <mi>
              d 
            </mi> 
            <mi>
              R 
            </mi> 
            <mi>
              t 
            </mi> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mn>
           2 
         </mn> 
        </mfrac> 
       </mrow> 
      </mstyle> 
      <mo>
        + 
      </mo> 
      <mstyle displaystyle="true"> 
       <msub> 
        <mo>
          ∑ 
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        <mrow> 
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         </mi> 
         <mo>
           &lt; 
         </mo> 
         <mi>
           j 
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        </mrow> 
       </msub> 
       <mrow> 
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           ( 
         </mo> 
         <mrow> 
          <msub> 
           <mi>
             m 
           </mi> 
           <mi>
             i 
           </mi> 
          </msub> 
          <msup> 
           <mi>
             c 
           </mi> 
           <mn>
             2 
           </mn> 
          </msup> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <msub> 
           <mi>
             r 
           </mi> 
           <mi>
             i 
           </mi> 
          </msub> 
          <mo>
            − 
          </mo> 
          <msub> 
           <mi>
             r 
           </mi> 
           <mi>
             j 
           </mi> 
          </msub> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
      </mstyle> 
     </mrow> 
    </math> for the Hamiltonian. (29)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        u 
      </mi> 
      <mo>
        = 
      </mo> 
      <mrow> 
       <mrow> 
        <mi>
          c 
        </mi> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <msqrt> 
           <mrow> 
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              d 
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            </mi> 
            <msub> 
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               t 
             </mi> 
             <mi>
               v 
             </mi> 
            </msub> 
           </mrow> 
          </msqrt> 
          <mo>
            + 
          </mo> 
          <msqrt> 
           <mrow> 
            <mi>
              d 
            </mi> 
            <mi>
              R 
            </mi> 
            <msub> 
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               t 
             </mi> 
             <msup> 
              <mi>
                u 
              </mi> 
              <mo>
                ′ 
              </mo> 
             </msup> 
            </msub> 
           </mrow> 
          </msqrt> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mo>
         / 
       </mo> 
       <mrow> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mn>
            1 
          </mn> 
          <mo>
            + 
          </mo> 
          <mrow> 
           <mo>
             ( 
           </mo> 
           <mrow> 
            <msqrt> 
             <mrow> 
              <mi>
                d 
              </mi> 
              <mi>
                R 
              </mi> 
              <msub> 
               <mi>
                 t 
               </mi> 
               <mi>
                 v 
               </mi> 
              </msub> 
             </mrow> 
            </msqrt> 
            <mo>
              ∗ 
            </mo> 
            <msqrt> 
             <mrow> 
              <mi>
                d 
              </mi> 
              <mi>
                R 
              </mi> 
              <msub> 
               <mi>
                 t 
               </mi> 
               <msup> 
                <mi>
                  u 
                </mi> 
                <mo>
                  ′ 
                </mo> 
               </msup> 
              </msub> 
             </mrow> 
            </msqrt> 
           </mrow> 
           <mo>
             ) 
           </mo> 
          </mrow> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
      </mrow> 
     </mrow> 
    </math> for summing relativistic velocities. (30)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        γ 
      </mi> 
      <mo>
        = 
      </mo> 
      <mfrac> 
       <mn>
         1 
       </mn> 
       <mrow> 
        <msqrt> 
         <mrow> 
          <mn>
            1 
          </mn> 
          <mo>
            − 
          </mo> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
         </mrow> 
        </msqrt> 
       </mrow> 
      </mfrac> 
      <mo>
        = 
      </mo> 
      <mrow> 
       <mn>
         1 
       </mn> 
       <mo>
         / 
       </mo> 
       <mrow> 
        <msqrt> 
         <mrow> 
          <msub> 
           <mi>
             T 
           </mi> 
           <mn>
             0 
           </mn> 
          </msub> 
         </mrow> 
        </msqrt> 
       </mrow> 
      </mrow> 
     </mrow> 
    </math> for the Lorentz Factor. (31)</p>
   <p>
    <math display="inline" xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        u 
      </mi> 
      <mo>
        = 
      </mo> 
      <mrow> 
       <mo>
         ‖ 
       </mo> 
       <mover accent="true"> 
        <mi>
          u 
        </mi> 
        <mo>
          → 
        </mo> 
       </mover> 
       <mo>
         ‖ 
       </mo> 
      </mrow> 
      <mo>
        = 
      </mo> 
      <msqrt> 
       <mrow> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mi>
          d 
        </mi> 
        <mi>
          R 
        </mi> 
        <msub> 
         <mi>
           t 
         </mi> 
         <mi>
           x 
         </mi> 
        </msub> 
        <mo>
          + 
        </mo> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mi>
          d 
        </mi> 
        <mi>
          R 
        </mi> 
        <msub> 
         <mi>
           t 
         </mi> 
         <mi>
           y 
         </mi> 
        </msub> 
        <mo>
          + 
        </mo> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mi>
          d 
        </mi> 
        <mi>
          R 
        </mi> 
        <msub> 
         <mi>
           t 
         </mi> 
         <mi>
           z 
         </mi> 
        </msub> 
       </mrow> 
      </msqrt> 
     </mrow> 
    </math> for the Euclidean norm of the 3d velocity vector. (32)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        U 
      </mi> 
      <mo>
        = 
      </mo> 
      <mi>
        γ 
      </mi> 
      <mrow> 
       <mo>
         ( 
       </mo> 
       <mrow> 
        <mi>
          c 
        </mi> 
        <mo>
          , 
        </mo> 
        <mover accent="true"> 
         <mi>
           u 
         </mi> 
         <mo>
           → 
         </mo> 
        </mover> 
       </mrow> 
       <mo>
         ) 
       </mo> 
      </mrow> 
     </mrow> 
    </math> for the Four-Velocity. (33)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mfrac> 
       <mrow> 
        <mn>
          8 
        </mn> 
        <mi>
          π 
        </mi> 
        <mi>
          r 
        </mi> 
        <mrow> 
         <mo>
           ( 
         </mo> 
         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
         </mrow> 
         <mo>
           ) 
         </mo> 
        </mrow> 
       </mrow> 
       <mrow> 
        <msup> 
         <mi>
           c 
         </mi> 
         <mn>
           2 
         </mn> 
        </msup> 
        <mi>
          M 
        </mi> 
       </mrow> 
      </mfrac> 
     </mrow> 
    </math> for Einstein’s Gravitational Constant. (34)</p>
   <p>
    <math xmlns="http://www.w3.org/1998/Math/MathML"> <mrow> 
      <mi>
        F 
      </mi> 
      <mo>
        = 
      </mo> 
      <mi>
        q 
      </mi> 
      <mrow> 
       <mo>
         ( 
       </mo> 
       <mrow> 
        <mi>
          E 
        </mi> 
        <mo>
          + 
        </mo> 
        <mi>
          c 
        </mi> 
        <msqrt> 
         <mrow> 
          <mi>
            d 
          </mi> 
          <mi>
            R 
          </mi> 
          <mi>
            t 
          </mi> 
         </mrow> 
        </msqrt> 
        <mo>
          ∗ 
        </mo> 
        <mi>
          B 
        </mi> 
       </mrow> 
       <mo>
         ) 
       </mo> 
      </mrow> 
     </mrow> 
    </math> For the Lorentz Force. (35)</p>
  </sec><sec id="s4">
   <title>Appendix A. Relative Velocities of the Planets from Different Perspectives</title>
   <p>Since relative velocity changes with a change in perspective, the relative rate of time must, too.</p>
   <p>Considering relative velocity and rates of evolution within the continuum, in the following computations:</p>
   <p>Planetary orbital lengths and periods are as per NASA.</p>
   <p>Orbital periods are related to 1 Earth year.</p>
   <p>Orbital lengths are as perceived “around the Sun”.</p>
   <p>Helical orbital lengths are computed using the following formula:</p>
   <p>(Distance travelled by the Sun)<sup>2</sup> + (Orbital length)<sup>2</sup> = (Helical length)<sup>2</sup></p>
   <p>The distance travelled by the Sun is relative to the CMBR.</p>
   <p>Sun velocity = 368 km/s = 11.60672 * 10<sup>9</sup> km/yr.</p>
   <p>Considering the perspective of the orbits of Mercury and Venus relative to the plane of the ecliptic, we assign Mercury a velocity of 47.89 km/s and Venus one of 35.03 km/s, a large difference.</p>
   <p>But if we consider the velocity of the Sun and its forward evolution in time relative to the CMB, and the helical distances travelled by the planets we get a much different perspective:</p>
   <p>Mercury:</p>
   <p>Orbital length: 57.909227 * 10<sup>6</sup> km</p>
   <p>Orbital period = .24 yr</p>
   <p>Orbits/yr = 4.1666</p>
   <p>Total orbital length = 241.249839 * 10<sup>6</sup> km</p>
   <p>Helical length = 11.609226961 * 10<sup>9</sup> km</p>
   <p>Velocity = 368.07948 km/s vs 47.89 km/s</p>
   <p>Venus:</p>
   <p>Orbital length: 10.8209475 * 10<sup>7</sup> km</p>
   <p>Orbital period = .62 yr</p>
   <p>Orbits/yr = 1.6129</p>
   <p>Total orbital length = 17.4531062 * 10<sup>7</sup> km</p>
   <p>Helical length = 11.608032143 * 10<sup>9</sup> km</p>
   <p>Velocity = 368.04160 km/s vs 35.03 km/s</p>
   <p>Earth:</p>
   <p>Orbital length: 14.9598262 * 10<sup>7</sup> km</p>
   <p>Orbital period = 1 yr</p>
   <p>Orbits/yr = 1</p>
   <p>Total orbital length = 14.9598262 * 10<sup>7</sup> km</p>
   <p>Helical length = 11.607684041 * 10<sup>9</sup> km</p>
   <p>Velocity = 368.03056 km/s vs 29.79</p>
   <p>Mars:</p>
   <p>Orbital length: 22.7943824 * 10<sup>7</sup> km</p>
   <p>Orbital period = 1.88 yr</p>
   <p>Orbits/yr = 0.5319</p>
   <p>Total orbital length = 121.2467148 * 10<sup>6</sup> km</p>
   <p>Helical length = 11.607353269 * 10<sup>9</sup> km</p>
   <p>Velocity = 368.02007 km/s vs 24.13</p>
   <p>Jupiter:</p>
   <p>Orbital length: 778.340821 * 10<sup>6</sup> km</p>
   <p>Orbital period = 11.86 yr</p>
   <p>Orbits/yr = 0.0843</p>
   <p>Total orbital length = 65.6273879 * 10<sup>6</sup> km</p>
   <p>Helical length = 11.606905535 * 10<sup>9</sup> km</p>
   <p>Velocity = 368.00588 km/s vs 13.06</p>
   <p>Saturn:</p>
   <p>Orbital length: 142.6666422 * 10<sup>7</sup> km</p>
   <p>Orbital period = 29.46 yr</p>
   <p>Orbits/yr = 0.0339</p>
   <p>Total orbital length = 484.27237 * 10<sup>5</sup> km</p>
   <p>Helical length = 11.606821027 * 10<sup>9</sup> km 12576482920</p>
   <p>Velocity = 368.00320 km/s vs 9.64</p>
   <p>Uranus:</p>
   <p>Orbital length: 287.0658186 * 10<sup>7</sup> km</p>
   <p>Orbital period = 84.01 yr</p>
   <p>Orbits/yr = .0199</p>
   <p>Total orbital length = 341.70434 * 10<sup>5</sup> km</p>
   <p>Helical length = 11.606770299 * 10<sup>9</sup> km</p>
   <p>Velocity = 368.00159 km/s vs 6.81</p>
   <p>Neptune</p>
   <p>Orbital length: 449.8396441 * 10<sup>7</sup> km</p>
   <p>Orbital period = 164.8 yr</p>
   <p>Orbits/yr = 0.0060</p>
   <p>Total orbital length = 272.96094 * 10<sup>5</sup> km</p>
   <p>Helical length = 11.606752096 * 10<sup>9</sup> km</p>
   <p>Velocity = 368.00101 km/s vs 5.43</p>
   <p>From this perspective, the velocities, or rate of evolution, of Mercury and Venus are only 0.038 km/s different. There would be no difference if the tilt of the ecliptic and the fact that the orbits are elliptical and not circular were taken into consideration. Note also that as we increase distance from the Sun, the velocities decrease until Neptune has a velocity only 0.001 km/s different from the base velocity of the Sun. Relative velocities equalize with a larger perspective. If we shift out to the local group and its apparent motion relative to the CMB of 627 km/s, the difference between the Sun and Neptune’s velocity is only 0.00059 km/s.</p>
   <p>In both perspectives, the velocity and acceleration are directly related to the dRt/distance so are higher in steeper gradients, and this higher apparent acceleration of events in slower time frames maintains their relative positions within the overall continuum as it evolves forward as viewed from both perspectives.</p>
   <p>This means GR is describing the forward evolution of the continuum and the events occurring within it, rather than the evolution of events through pre-existing “curved spacetime”. It is not the masses that determine relative velocities and trajectories, but the dynamics and perspectives in time.</p>
  </sec>
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</article>