<?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">JHEPGC</journal-id><journal-title-group><journal-title>Journal of High Energy Physics, Gravitation and Cosmology</journal-title></journal-title-group><issn pub-type="epub">2380-4327</issn><publisher><publisher-name>Scientific Research Publishing</publisher-name></publisher></journal-meta><article-meta><article-id pub-id-type="doi">10.4236/jhepgc.2023.91001</article-id><article-id pub-id-type="publisher-id">JHEPGC-121126</article-id><article-categories><subj-group subj-group-type="heading"><subject>Articles</subject></subj-group><subj-group subj-group-type="Discipline-v2"><subject>Physics&amp;Mathematics</subject></subj-group></article-categories><title-group><article-title>
 
 
  How 5 Dimensions May Fix a Deterministic Background Spatially as to Be Inserted for HUP in 3 + 1 Dimensions, and Its Relevance to the Early Universe
 
</article-title></title-group><contrib-group><contrib contrib-type="author" xlink:type="simple"><name name-style="western"><surname>Andrew</surname><given-names>Walcott Beckwith</given-names></name><xref ref-type="aff" rid="aff1"><sub>1</sub></xref><xref ref-type="corresp" rid="cor1"><sup>*</sup></xref></contrib></contrib-group><aff id="aff1"><label>1</label><addr-line>Department of Physics, College of Physics, Chongqing University Huxi Campus, Chongqing, China</addr-line></aff><pub-date pub-type="epub"><day>09</day><month>11</month><year>2022</year></pub-date><volume>09</volume><issue>01</issue><fpage>1</fpage><lpage>6</lpage><history><date date-type="received"><day>1,</day>	<month>October</month>	<year>2022</year></date><date date-type="rev-recd"><day>7,</day>	<month>November</month>	<year>2022</year>	</date><date date-type="accepted"><day>10,</day>	<month>November</month>	<year>2022</year></date></history><permissions><copyright-statement>&#169; 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><p>
 
 
  We will first of all reference a value of momentum, in the early universe. This is for 3 + 1 dimensions and is important since Wesson has an integration of this momentum with regards to a 5 dimensional parameter included in an integration of momentum over space which equals a ration of 
  L divided by small l (length) and all these times a constant. The ratio of 
  L over small l is a way of making deterministic inputs from 5 dimensions into the 3 + 1 dimensional HUP. In doing so, we come up with a very small radial component for reasons which due to an argument from Wesson is a way to deterministically fix one of the variables placed into the 3 + 1 HUP. This is a deterministic input into a derivation which is then First of all, we restate a proof of a highly localized special case of a metric tensor uncertainty principle first written up by Unruh. Unruh did not use the Roberson-Walker geometry which we do, and it so happens that the dominant metric tensor we will be examining, is variation in 
  δg<sub>tt</sub>. The metric tensor variations are given by 
  δg<sub>rr</sub>, 
  δg<sub>θθ</sub> and 
  δg<sub>φφ</sub> are negligible, as compared to the variation 
  δg<sub>tt</sub>. From there the expression for the HUP and its applications into certain cases in the early universe are strictly affected after we take into consideration a vanishingly small r spatial value in how we define 
  δg<sub>tt</sub>.
 
</p></abstract><kwd-group><kwd>Massive Gravitons</kwd><kwd> Heisenberg Uncertainty Principle (HUP)</kwd><kwd> Riemannian-Penrose Inequality</kwd></kwd-group></article-meta></front><body><sec id="s1"><title>1. Introduction: Why We Analyse Our HUP with Very Small Radial r Value. Here It Comes Directly from the 5<sup>th</sup> Dimension</title><p>Wesson in [<xref ref-type="bibr" rid="scirp.121126-ref1">1</xref>], page 105 has the following result of how the momentum is affected by a 5 dimensional input (from the fifth dimension). In other words we have the following expression, namely</p><p>∫ p α d x α = &#177; h c ⋅ L l (1)</p><p>We will be defining what the momentum p α is in our treatment of the early universe whereas the first five dimensional input value L here comes from the inverse of the square root of the cosmological constant</p><p>L ≡ 3 Λ (2)</p><p>Whereas the term l is equal to the Compton wavelength of a “particle” m for which</p><p>l ≡ h m ⋅ c (3)</p><p>So if we use the reasoning done in [<xref ref-type="bibr" rid="scirp.121126-ref2">2</xref>] in the early universe, namely [<xref ref-type="bibr" rid="scirp.121126-ref2">2</xref>] we have that due to that documents page 2, formula (9)</p><p>〈 p 〉 = − β ˜ 2 m P ⋅ ν π G ⋅ ln t ϖ c (4)</p><p>And keeping in mind the Wesson 5 dimensional line element [<xref ref-type="bibr" rid="scirp.121126-ref1">1</xref>] given by</p><p>d S 5-dim 2 = L 2 l 2 ⋅ d s 4-dim 2 − L 4 l 4 ⋅ d l 2 (5)</p><p>We get an infinitesimal r value due to from the 5<sup>th</sup> dimension fixing the value of to be very small in a deterministic fashion</p><p>∫ p α d x α = &#177; h c ⋅ L l = &#177; h c ⋅ 3 Λ m particle h = r m p l ⋅ ( 1 − log [ r ϖ ⋅ c ] ) ⇔ r ≈ ε + (6)</p><p>This is in tandem with the value of z, as to red shift showing up in [<xref ref-type="bibr" rid="scirp.121126-ref3">3</xref>] and it shows how to obtain a very small radial value in a different manner, namely in a tiny scale factor due to an enormous z red shift as given in [<xref ref-type="bibr" rid="scirp.121126-ref3">3</xref>].</p><p>Quote</p><p>Note this comes from a scale factor, if z ~ 10 55 ⇔ a scalefactor ~ 10 − 55 , i.e. 55 orders of magnitude smaller than what would normally consider, but here note that the scale factor is not zero, so we do not have a space-time singularity.</p><p>End of quote</p><p>However that scale factor being very small, with enormous red shift is in tandem with Equation (6). So go to the HUP.</p></sec><sec id="s2"><title>2. Recalling the Argument from [<xref ref-type="bibr" rid="scirp.121126-ref3">3</xref>] as to the Form of the Early Universe HUP</title><p>Note this comes from a scale factor, if z ~ 10 55 ⇔ a scalefactor ~ 10 − 55 , i.e. 55 orders of magnitude smaller than what would normally consider [<xref ref-type="bibr" rid="scirp.121126-ref3">3</xref>],</p><p>〈 ( δ g u v ) 2 ( T ^ u v ) 2 〉 ≥ ℏ 2 V Volume 2 → u v → t t 〈 ( δ g t t ) 2 ( T ^ t t ) 2 〉 ≥ ℏ 2 V Volume 2 &amp;     δ g r r ~ δ g θ θ ~ δ g ϕ ϕ ~ 0 + (7)</p><p>δ t Δ E ≥ ℏ δ g t t ≠ ℏ 2 Unless     δ g t t ~ O ( 1 ) (8)</p><p>δ g t t ~ a 2 ( t ) ⋅ ϕ ≪ 1 (9)</p><p>Then, there is no way that Equation (9) is going to come close to δ t Δ E ≥ ℏ 2 .</p></sec><sec id="s3"><title>3. How We Can Justifying Writing Very Small δ g r r ~ δ g θ θ ~ δ g ϕ ϕ ~ 0 + Values</title><p>To begin this process, we will break it down into the following co ordinates [<xref ref-type="bibr" rid="scirp.121126-ref3">3</xref>].</p><p>In the rr, θ θ and ϕ ϕ coordinates, we will use the Fluid approximation, T i i = d i a g ( ρ , − p , − p , − p ) [<xref ref-type="bibr" rid="scirp.121126-ref3">3</xref>] with</p><p>δ g r r T r r ≥ − | ℏ ⋅ a 2 ( t ) ⋅ r 2 V ( 4 ) | → a → 0 0 δ g θ θ T θ θ ≥ − | ℏ ⋅ a 2 ( t ) V ( 4 ) ( 1 − k ⋅ r 2 ) | → a → 0 0 δ g ϕ ϕ T ϕ ϕ ≥ − | ℏ ⋅ a 2 ( t ) ⋅ sin 2 θ ⋅ d ϕ 2 V ( 4 ) | → a → 0 0 (10)</p></sec><sec id="s4"><title>4. After Doing This, How Can We Obtain Values of δ g t t</title><p>We win put in different values of the scalar potential and make comments as to what this pertains to in terms of early universe physics.</p><p>The first one will be using a scalar field from inflaton physics, as presented by Padmanabhan [<xref ref-type="bibr" rid="scirp.121126-ref4">4</xref>]. For the record, Dr. Tony Scott has communicated his disapproval of involving the Padmanabhan potential to the author in communications, but this will be presented as one of the possible choices.</p><p>First we have from [<xref ref-type="bibr" rid="scirp.121126-ref2">2</xref>]</p><p>V ( ϕ ) = V 0 exp ( − λ ϕ m P ) ↔ V 0 exp ( − 16 π G ν ⋅ ϕ ) (11)</p><p>And also [<xref ref-type="bibr" rid="scirp.121126-ref2">2</xref>] [<xref ref-type="bibr" rid="scirp.121126-ref5">5</xref>]</p><p>a ( t ) = a initial t ν ⇒ ϕ = ln ( 8 π G V 0 ν ⋅ ( 3 ν − 1 ) ⋅ t ) ν 16 π G ⇒ ϕ ˙ = ν 4 π G ⋅ t − 1 ⇒ H 2 ϕ ˙ ≈ 4 π G ν ⋅ t ⋅ T 4 ⋅ 1.66 2 ⋅ g ∗ m P 2 ≈ 10 − 5 (12)</p><p>Where we can put in the values of Equation (12) into Equation (9). We can write an expression for V 0 from [<xref ref-type="bibr" rid="scirp.121126-ref6">6</xref>], page 153 taking the form of if the denominator is the e fold value of inflation,</p><p>V 0 1 / 4 = 0.022 m P q N e-folds (13)</p><p>And using the Starobinsky model, plus [<xref ref-type="bibr" rid="scirp.121126-ref2">2</xref>] [<xref ref-type="bibr" rid="scirp.121126-ref7">7</xref>] [<xref ref-type="bibr" rid="scirp.121126-ref8">8</xref>] to get a value of L.</p><p>And so we obtain if we have a scale factor behaving as in (12)</p><p>Λ ≈ − [ V 0 3 γ − 1 + 2 N + γ ⋅ ( 3 γ − 1 ) 8 π G ⋅ t ˜ 2 ] 1 κ ∫ − g ⋅ d 3 x + ( 6 ⋅ ( a &#168; a + ( a ˙ a ) 2 ) ) | t = t ˜ ≈ − [ V 0 3 γ − 1 + 2 V 0 ⋅ ( 1 − exp [ − q ⋅ ϕ / m P ] ) 2 + γ ⋅ ( 3 γ − 1 ) 8 π G ⋅ t ˜ 2 ] 1 κ ∫ − g ⋅ d 3 x     + 6 ⋅ − t ⋅ γ ⋅ ( 3 γ − 1 ) m P G ⋅ 1 8 π + 48 π G 3 ⋅ [ V 0 ⋅ ( 1 − exp [ − q ⋅ ϕ / m P ] ) 2 ] (14)</p><p>This can be put into the value of Equation (9), If we presume Planck time, then if the value of Equation (9) is very small which is frequently a result, we will have a very large value for change in Energy, which would in its own way confirm the enormous value of M initially confirmed as forming which is in [<xref ref-type="bibr" rid="scirp.121126-ref8">8</xref>] via the relationship of change in energy E will be proportional to the very large value of M so initially formed.</p></sec><sec id="s5"><title>5. Conclusions</title><p>Comparing with the other assumed early uncertainty principles what is in Equation (9) plus the inputs into Equation (14) put into Equation (9) which influences Equation (8) should be compared with following Uncertainty principle [<xref ref-type="bibr" rid="scirp.121126-ref9">9</xref>] [<xref ref-type="bibr" rid="scirp.121126-ref10">10</xref>] [<xref ref-type="bibr" rid="scirp.121126-ref6">6</xref>] [<xref ref-type="bibr" rid="scirp.121126-ref11">11</xref>]</p><p>Δ t ≥ ℏ Δ E + γ t P 2 Δ E ℏ ⇒ ( Δ E ) 2 − ℏ Δ t γ t P 2 ( Δ E ) 1 + ℏ 2 γ t P 2 = 0 ⇒ Δ E = ℏ Δ t 2 γ t P 2 ⋅ ( 1 + 1 − 4 ℏ 2 γ t P 2 ⋅ ( ℏ Δ t 2 γ t P 2 ) 2 ) = ℏ Δ t 2 γ t P 2 ⋅ ( 1 &#177; 1 − 16 ℏ 2 γ t P 2 ( ℏ Δ t ) 2 ) (15)</p><p>Δ E ≈ ℏ Δ t 2 γ t P 2 ⋅ ( 1 &#177; ( 1 − 8 ℏ 2 γ t P 2 ( ℏ Δ t ) 2 ) ) ⇒ Δ E ≈ either   ℏ Δ t 2 γ t P 2 ⋅ 8 ℏ 2 γ t P 2 ( ℏ Δ t ) 2 ,   or   ℏ Δ t 2 γ t P 2 ⋅ ( 2 − 8 ℏ 2 γ t P 2 ( ℏ Δ t ) 2 ) (16)</p><p>A point by point comparison of these values should be the next objective of a research project. Furthermore the items brought up in references [<xref ref-type="bibr" rid="scirp.121126-ref12">12</xref>] [<xref ref-type="bibr" rid="scirp.121126-ref13">13</xref>] [<xref ref-type="bibr" rid="scirp.121126-ref14">14</xref>] [<xref ref-type="bibr" rid="scirp.121126-ref15">15</xref>] [<xref ref-type="bibr" rid="scirp.121126-ref16">16</xref>] will be able to be vetted provided that we make the comparison between Equation (8) and Equation (9) with Equation (15) and Equation (16) in a rigorous manner.</p><p>In particular, I would look forward to eventual experimental verification, if the early universe HUP were really understood of investigating the great ideas brought up by Corda in [<xref ref-type="bibr" rid="scirp.121126-ref12">12</xref>].</p><p>Determination of that would be exciting experimental gravitational physics.</p></sec><sec id="s6"><title>Acknowledgements</title><p>This work is supported in part by National Nature Science Foundation of China grant No. 11375279.</p></sec><sec id="s7"><title>Conflicts of Interest</title><p>The author declares no conflicts of interest regarding the publication of this paper.</p></sec><sec id="s8"><title>Cite this paper</title><p>Beckwith, A.W. 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