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Physics & Astronomy International Journal

Research Article Volume 4 Issue 4

A universe with a constant expansion rate

Hans J Fahr,1 Michael Heyl2

1Argelander Institut für Astronomie, Universität Bonn Auf dem Hügel 71, Germany
2Deutsches Zentrum für Luft und Raumfahrt (DLR) Königswinterer Str. 522 - 524, 53227 Bonn, Germany

Correspondence: Hans J Fahr, Argelander Institut für Astronomie, Universität Bonn Auf dem Hügel 71, 53121 Bonn, Germany

Received: July 21, 2020 | Published: August 12, 2020

Citation: Fahr HJ, Heyl M. A universe with a constant expansion rate. Phys Astron Int J. 2020;4(4):156-163. DOI: 10.15406/paij.2020.04.00215

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Abstract

One of the strongest supports for the existence of a cosmological vacuum energy density Λ is given by the SN-Ia luminosities as function of the redshift z of the host galaxies, since they seem to indicate an accelerated expansion of the universe in more recent cosmic times. In this paper, we show that one in fact, however, can start out from the astronomical observations of two-point correlation functions regulating the positions of galaxies and clusters of galaxies and derive from them the average cosmic mass density in the universe. We obtained that for the scale-invariant mass distribution derived from these correlation functions we only obtain a finite mass density for a positive curvature parameter k=+1, while for curvature parameters k=0 and k=−1 one obtains vanishing cosmic mass densities. In these latter universes one consequently would find conditions for a "coasting cosmology" fulfilled which abolishes the need for a cosmic vacuum energy Λ.

Keywords: vacuum energy density, redshift, host galaxies, accelerated expansion, coasting cosmology

Introduction

During many decades after the first Friedman-Lemaitre FLRW- cosmological models1,2 on the basis of Einstein‘s GTR field equations3,4 the expansion of the universe was assumed to occur as decelerated by the internal gravitation of the universe due to its matter and energy contents. In the recent decades, however, measurements of the luminosity of distant high-redshift type Ia supernovae seemed to show that these standard candles are looking fainter than could be expected on the basis of these classical cosmological models.5–10 For the purpose to nevertheless fit these new observations with cosmological models, an artificial term - called  and denoting the dynamical effect of a cosmic vacuum energy density of completely unknown nature - has been introduced into the earlier Friedman equations with the wholesome effect of accelerating the cosmic expansion at large scales of our present epoch. Meanwhile, however, the need for this artificial enlargement of the Friedman equations has been doubted on several grounds; one is that the interpretations of luminosities of the most distant supernovae SNe-Ia may not be correctly carried out and thus misleading in the conclusions derived with them, the other is that so-called "coastal cosmology" - models , without cosmic vacuum energy density as ingredient, can in fact be proposed that can well fit the observed SNe-Ia luminosities (e.g. see Cassado, 2020).

Most recently Kang et al.,11 have found evidences for an evolutionary trend in SN Ia supernova brightnesses which in principle were pointed out all the time since the publication by Tinsley12. Their most recent studies namely seem to have shown that the brightness of standardized SN Ia supernovae is intrinsically correlated to the morphology, the mass, and the local star formation rate of the host galaxy, while in the works by Perlmutter et al.,13 and contemporary publishers it had been assumed that the standardized SN Ia brightness does not evolve with redshift or look-back time. This indicates the problem that the present SN Ia light curve fitters supporting the standard ΛCDM cosmological models are not taking care for a correction for this population age effect which would therefore create a serious systematic bias with increasing redshift. Just those most red-shifted SN Ia objects which presently give the strongest support for an accelerating cosmic expansion and the action of a cosmic vacuum energy would be most concerned by this bias. Meanwhile Riess et al.,14 recognized that a luminosity evolution of 25 percent over a look-back-time of 5 Gyr would be sufficient to nullify the present cosmological claims.

In this respect it is highly interesting to read in the most recent publication by Cassado (2020) that the presently discussed SNe Ia data are also fitted nicely by a universe with a "coasting cosmology" which expands according to a linear expansion model R(t)t with no deceleration and no acceleration, but with a permanently vanishing deceleration parameter q=R¨R/˙R2=0. This was already found in earlier publications by Dev et.,15–18 This fact of an equally nice fit of a coasting universe compared to the prominent ΛCDM model concerning compatibility with SNe Ia data had already shown up clearly in a figure given in a publication by Perlmutter et al.19. But in his publication the author favored the fit by the ΛCDM  model as compared to disfavored coasting model, because the latter needed an empty universe with vanishing mass density (i.e. ΩM;Ωk=0) which obviously, in view of the present matter in the universe, cannot be assumed to prevail.

This latter conclusion was in principle also shared by Cassado (2020) who therefore was voting for quasi-coastal universe with a quasi-linear expansion like R(t)t(1γ) with γ1. But it should be pointed out here that an empty universe neither is in fact a severe need of the coastal universe, nor can a vanishing of the average cosmic mass density simply be excluded as we are going to show in the following part of the paper. To our knowledge one of the first authors presenting a coastal cosmology was Kolb20 who introduced a special form of matter which he called K-matter with an equation of state pK=(1/3)ρK in between the poly-tropic behavior of photonic matter and massive matter. For this form of matter the second Friedmann equation delivers

¨RR=4πG3(ρK+3pK)=0 (1)

It can be shown that this K-matter leads to a density decrease by ρKR2 and by its polytropic behaviour ρK+3pK=0 induces a coasting universe.

This form of a K-matter unfortunately is not a physically very handy and easy to understand form of matter and thus may be disfavored for that reason in offering a physically reliable cosmological solution. As was shown, however, in papers by Fahr21 and Fahr22 and this unconventional sub-adiabatic behavior of density with the scale R of the universe is naturally obtained for a Machian form of scale-related masses of cosmic particles with mR which then evidently with ρR2 leads to a coasting cosmology. But as we shall show in the following part of the paper, one does not need to believe in such a Machian mass behavior tuning the cosmic masses with the size R of the universe, but it can be shown that an empty universe with vanishing mass density ρU=0 creating a coasting cosmology is in fact physically reasonable - even in view of the cosmic masses seen around us, if the universe has a scale-invariant hierarchical structuring.

The cosmic mass density in a hierarchically structured universe

In the afore presented argumentation25 it became obvious, that the theoretical interpretation of distant high-redshift SN1a luminosity data is well possible, instead by the new ΛCDM cosmological models, as well on the basis of a coasting expansion cosmology23,24 with a linear expansion of the scale of the universe with cosmic time t according to R(t)t. The attractive advantage on one hand in the use of these latter cosmological models is that neither dark matter nor dark energy is required (i.e ΩD=ΩΛ=0) for the interpretation, the disadvantage on the other hand, as seen by many of the present main-stream cosmologists, is that such coasting models as given by Kolb et al.,20–27 have to assume an empty energy-momentum tensor Tik for the universe, i.e. a tensor with vanishing ingredients at all cosmic times t. Especially such coasting universes should have either, as we are going to show, the special Machian property of scale-related cosmic masses leading to vanishing mass densities at the largest scales, or the property that mass density ρU is zero at all relevant cosmic times due to reasons which are connected with a full compensation of contributions from masses through those from pressures in the universe.

Most cosmologists are hesitating to accept this rather unlikely balance in the Tik ingredients leading to a coasting universe. This zero-mass universe seems to be too much an artifact like the assumption of cosmic vacuum energy Λ is too. In the following section, however, just for that purpose, we want to introduce a universe leading to a vanishing cosmic mass density ρU0! at the largest cosmic distances without such artifacts which in contrast is even supported by astrophysical measurements as we are going to show below.

We start from the astronomical observations carried out by Bahcall et al.,28,29 and or equally well in more recent times by Sylos-Labini et al.,30 and or Sylos-Labini31 and take their two-point correlation function ξ(l) denoting the probability to find other stellar objects at a distance l from any other arbitrarily taken stellar object. The quantity l has to be considered as the so-called distance parameter taken by astronomers to be identical with the redshift distance, making it evidently a cosmologically biased quantity. From this star-correlation function ξ(l) we will deduce in the following an associated model for the underlying cosmic matter density distribution ρU=ρU(l). This we first did for a different aspect in a recent paper Fahr etal.,32. We use the well confirmed correlation function ξ(l) based on astronomical observations of the visible star and galaxy constellation which is surrounding us seen from our cosmic vantage point, - and, according to the generally assumed cosmological principle, also should surround every other cosmic vantage point in an analogous and equivalent manner, unless the generally accepted, sacrosanct cosmological principle would turn out to be violated,- in which case, however, all the other Robertson-Walker cosmologies would as well become invalid, and even taken broader, all cosmology had to be given up.

This two-point correlation function ξ(l) defines the probability to find another star (or galaxy) at a distance lfrom our arbitrary standpoint and, based on astronomical observations, is expressed in the following mathematical form:

ξ(l)=ξ0(l0l)α      (2)

where ξ0 is a reference value valid at the reference distancel0. The correlation index α has been observationally determined by Bahcall et al.28 withα=1.8 By the way, as we do show in the appendix, this above hierarchic distribution of stars naturally explains why no Olbers Paradox (Paradox of the dark night sky!) has to be expected in such a universe.

An interesting problem connected with the above mentioned clustering is the cosmologically important point, that the validity of the above correlation function can evidently also be interpreted as an expression for the structured stellar mass density ρ=ρ(l) or stellar mass density distribution of surrounding stars or galaxies in our cosmic environment. In this view it also expresses a standpoint-oriented mass density distribution ρ=ρ(l) when it is recognized that the mass dM(l) in this case is closely associated with the number of stars with a typical average stellar or galactic mass m0 on a spherical shell at distance l, and is given for a Euklidean space geometry (i.e. a flat universe with k=0 ) by

dM(l)=4πl2m0ξ0(l0l)αdl=4πl2ρ0(l0l)αdl (3)

with ρ0 denoting the hierarchy-typical reference value of mass density.

Bahcall and Chokski29 do furthermore point out the astonishing fact that the general type of the above mentioned two-point correlation function ξ(l) is observationally confirmed as well for galaxy correlations, as for cluster correlations, as also for super-cluster correlations, with the difference that only the reference scale l0 and the reference probability ξ0 or mass density ρ0 have to be adapted from the galaxy-case up to the super-cluster case, while as a surprise the same correlation index of αG=αC=αSC=1.8 is reappearing as a number common for all these hierarchies (i.e. scale invariant structuring!).

To comprehend and correctly describe space at the largest achievable distances lSC,0 of the order 100Mpc or more, we take the largest hierarchy, i.e. super-clusters, and use the corresponding SCSC correlation function. Connected with that correlation the following, associated mass increment with distance l is given:

dM(l)=4πl2ρSC,0(lSC,0l)αSCdl                        (4)

In order to address scientifically correct the largest achievable cosmic distances lR , with R denoting the scale of the universe, we have also to pay attention to the prevailing cosmic space geometry conditions and need to face the situation that, in order to keep our considerations open to the widest generality, that we are perhaps embedded not in a Euklidean universe, but in a curved general-relativistic space-time geometry. We for the sake of this generality should pay attention to the fact that the radial distance parameter l , in the Robertson-Walker approximation of the cosmic geometry, is transformed into a geometrical distance r(l) given by the following function:33,34

r(l)=l(1+kl2)1                  (5)

i.e. the spherical area associated to the distance parameter l then is Φ(l)=4πr2(l) where k denotes the cosmic curvature parameter. The latter e.g. is determined by looking for the best fitting cosmological FLRW-model35 which supports the value k0 . This latter uncurved cosmological model is, however, associated with and enforced by specifically equilibrated average cosmic Tik -ingredients like ΩΛ,ΩM,ΩD . These latter ingredients, however, under the perspectives given here, are shown to be highly problematic quantities. Nevertheless and besides of that, anticipating the indicated curvature value k as an apriori input, one can then take account of this above geometric distance transformation by bringing the above formula for dM(l) into the following form:dM(l)=4πl2(1+kl2)2mSC,0ξSC,0(lSC,0l)α×          

×(1kl2)(1+kl2)2dl                         (6)

and after a little rearrangement of the terms.

dM(l)=4πρSC,0(lSC,0l)α(1kl2)(1+kl2)4l2dl]                           (7)

The cosmic curvature parameter k can be restricted to values of k=0 or k=±1 , if l is scaled with the cosmic scale parameter R=R(t) by k=KR2 , K being the cosmic curvature scalar or the contracted Ricci tensor K=Rii . Therefore, besides the Euklidean case k=0 , favored by Benett et al.,35 one should also consider the following two more options:

dM(l)=4πρSC,0lαSC,0[(1l2R2)(1±l2R2)4l2αdl]                             (8)

After this inspection one can then state that the expression for the average cosmic density in such a hierarchically structured universe, for instance with k=±1 finally takes the following form:

ρ(l)=M(l)V(l)4πρSC,0lαSC,0λ0[(1μλ2P2)(1+λ2P2)2λ2αδλ]λ0[(1μλ2P2)(1+λ2P2)2λ2δλ]=4πρSC,0lαSC,0RαΞ0[(1μξ2)(1+ξ2)4ξ2αδξ]Ξ0[(1ξ2)(1+ξ2)4ξ2δξ]                 (9)

In Figure 1 we show the quantity ρ(l) as function of l , for all relevant cosmic geometries, i.e. k=±1 and k=0 .

Figure 1 Shown is the average cosmic density ρ(1) in units of the super-cluster density ρSC,0 as function of the averaging scale l/R for three different cosmic geometries characterized by curvature values k = 0 and k =±1.

As one can see in Figure 1 there exists only one model which leads to a finite cosmic density at large scales, namely for the positively curved universe with k=+1 ; the other two models with k=0 k=1 show cosmic densities which fall below every lower density limit with increasing scales, i.e. at largest scales they fall down to a density value of ρU0!

Coming back to the question whether coasting universes should be considered as a physical possibility, one can thus see from the above considerations that in universes with curvatures k=0 or k=1 and a hierarchical mass distribution one finds the appropriate prerequisites fulfilled for a coasting universe with a vanishing average cosmic mass density, i.e. ρU=0 !, despite the visible stars and galaxies around us. One more cosmological possibility might perhaps need to be considered here, namely that the hierarchical structuring of masses in the universe which was considered in the above calculation could perhaps also be a time-invariant cosmic structuring, meaning that even though the universe undergoes an expansion in cosmic time, its hierarchical structuring endures or persists. Of course an expanding hierarchical universe must also change its mass density, however in such a way that the hierarchical structuring of matter persists, i.e. a time-invariant scale-invariance under these auspices must be considered. This form of a structure persistence is given when only the reference density of the reference structure undergoes an associated cosmological time-dependence. Under these auspices the mass increment dM(l) derived above would then instead now be given by the expression:

dM(l)=4πl2ρSC,0(t)(lSC,0(t)l)αSCdl                              (10)

One may assume that the dimension lSC,0(t) of super-clusters increases with cosmic time t like the cosmic scale parameter, i.e.lSC,0(t)R(t). The reference value for the super-cluster density on the other hand most probably scales according to

ρSC,0(t)=ρSC,0(R0/R(t))3                                (11)

which then all-together leads to a mixed expression in time t and distance l given by:

dM(l)=4πl2ρSC,0(R0/R(t))3(R(t)l)αSCdl                     (12)

and again herewith brings up the already well-identified problem that in the cosmological GTR field equations time-averaging and space-averaging cannot be exchanged.36–38 One way to overcome this problem in the above described case would be to connect distances of cosmic masses with the time it takes to bring over the information on their mass locations by their gravity signals, i.e. gravitons, through the velocity c of light by correspondingly retarding the relevant evolutionary state of the universe. This would then lead to the easily integrable expression:

dM(l)=4πl2ρSC,0(R0R(t0l/c))3(R(t0l/c)l)αSCdl                     (13)

and shows that influences of the distant matter structures now are attaining a cosmologically historical pronunciation making the universe by this view a really authentic space-time unity. To further evaluate the above expression one would need to know the scale evolution R=R(t) in this universe. The latter, however, depends on the prevailing cosmic energy ingredients as especially the average mass density of cosmic matter ρ(l) which, however, is only found from the integration of expression (13). Not knowing in advance what the integrated expression starting with Equ. (13) will deliver, we can make two alternative assumptions in advance:

  1. The average mass density is positive and finite with ρ(l)=ρ.

or

  1. The average mass density is ρ(l)=0

The correctness of the assumption a) or b) will then be proven a posteriori after having carried out the necessary integrations. Starting with case a) we would be based on a matter-dominated flat universe (k=0) the scale evolution of which is known to follow the law R(t)t2/3 .39 Thus in this case one has

R(t)=R0(tt0)23=R0(t0l/ct0)23                         (14)

when using R(t)=R(t0l/c) witht=t0l/c. This then leads Equ. (13) to:

dM(l)=4πl2ρSC,0((t0t0l/c)23)3(R0l)αSC×               

×(t0l/ct0)2αSC3dl                  (15)

or      

dM(l)=4πl2ρSC,0(11l/ct0)2(R0l)αSC×

×(1l/ct0)2αSC3dl               (16)

We now use the substitutionz=1l/ct0, hereby keeping in mind that the relation t=t0l/c leads to l(t=0)=ct0 and l(t=t0)=0 which means z=0 for l(t=0)=ct0 and z=1 forl(t=t0)=0. Furthermore, dl is given bydl=ct0dz. This finally results in the following equation:

M=4π(ct0)3(R0ct0)αSCρSC,0×               

×10(1z)(2αSC)z(23αSC2)dz                   (17)

The retarded average density ρ(lR) is then given by:               

ρ(R)=M(R)V(R)=4π(ct0)3(R0ct0)αSCρSC,0×

×(ct0)3(R0ct0)αSCρSC,010(1z)(2αSC)z(23αSC2)dzct00l2dl                             (18)

Now, with the typical correlation index αSC=1.8 mentioned before in section 2 of this paper, and expressing the volume V by 4π3(cto)3 we get:

ρ=3(R0ct0)αSCρSC,010(1z)0.2z0.8dz

3(R0ct0)αSCρSC,04.75                          (19)

This shows that in case a) for the universe with a time-invariant and scale-invariant matter structuring one obtains a finite and positive average mass density which then a posteriori also justifies the use of the scale evolution law Rt2/3 valid for the matter-dominated universe.

Case b):

For this case we in advance want to assume that one obtains a vanishing average cosmic mass density with ρ(lR)=0. Consequently the scale evolution law for this universe is a "coasting cosmology evolution" given by the law R(t)t , and by carrying out the analogue calculation of the mass density as above for this universe we should be able to a posteriori prove that in this case the associated average density in fact is ρ(lR)=0 !But in fact we have carried out this alternative integration for case b) and it turns out that the resulting average mass density is again positive and even greater than in case a). But this then means that the use of the coasting cosmology scale law R(t)t is not a posteriori justified in this case b).

Deceleration of differential mass motions with respect to the local standard of rest

Let us consider now a single mass m embedded in a homogeneous, infinite universe. Then one may want to study the question: What will happen in case this mass m has a peculiar motion by a certain velocity U with respect to the local standard of rest of the ambient universe? How does this velocity behave in time? For the case that this peculiar motion is changing in time by an amountb=dU/dt, a local force must be identifiable causing this de-/ac-celerationb. In the absence of any viscous forces or electromagnetic forces etc. one may be able to reduce the force candidate to some effective force caused by the net gravitational pull of all the cosmic masses surrounding this peculiar mass , and one should be able to quantify a locally acting force as due to the net gravitational force of the ambient universe influencing this peculiar mass m at its peculiar motion U.

In order to study this problem more quantitatively one could follow the approach that already was used by Thirring40 or Soergel-Fabricius41 to study centrifugal forces acting on a mass rotating with respect to the rest of a universe with a homogeneous mass distribution. The idea there was to represent the mass of the universe as a system of congruent spherical mass shells. While Thirring40 or later Fahr24 and along this way had faced the problem of a rotating central mass to study the origin of cosmic centrifugal forces, we here instead have to look for a solution of the problem connected with a central mass m in peculiar motionU with respect to the rest of the universe. Question: Would this motion persist unchanged in time or will it undergo a temporal change and by what amount would it do it?

To answer this question on the basis of post-Newtonian SRT gravity one has to realize that due to the finite propagation speed of gravitons, communicating the surrounding mass constellation by gravitons to the position of the moving central mass m with the velocity of lightc, the individual mass sources δMU of the surrounding gravity field of the universe are all effectively acting from "apparently retarded" positions when judged from the position of the moving central mass (a phenomenon analogous to stars appearing at positions shifted from their true positions due to the motion of the observer: i.e. stellar aberration). That means, if the mass elementδMU on a spherical mass shell is seen by a central object at rest under an angleθ, it instead acts effectively from the aberration angle θ' on the central object, when the latter moves with the velocityU with respect to the local standard of rest. According to STR relations these two angles are connected by the following STR Doppler relation:

cosθ'=cosθ+β1+βcosθ                  (20)

where β is given by β=U/c.

Assuming a homogeneous and constant cosmic mass density distribution withρ=ρU, then one arrives at the following effective gravitational force K=(KUU)/U, aligned with the direction of the peculiar velocity U, acting in the direction (U) on the central mass m, due to the net gravitational pull of the surrounding cosmic mass assembly of the universe:         

K=Rmax0dRUπ0dθ×

×2π0dϕρUR2UGmR2Ucosθsinθ                                (21)

evidently leading to

K=2πρUGmRmax0δΡΥπ0cosθ' sinθdθ                               (22)

and to

K=2πρYΓμRmaxπ0cosθ'sinθdθ                      (23)

This expression already in this form reveals that K can only be a finite quantity, if the product ρURmax stays finite, requiring that the average density should be either strictly zero or proportional to ρUR1max in an infinite universe.

On the other way, with the average cosmic density ρU, expressed through the total mass MU for the Euclidean universe, given byρU=(3/4π)MU/R3max, - Rmax being the radius of the matter-filled universe -, leads to the following expression:

K=32GmMUR2maxπ0cosθ+β1+βcosθsinθdθ                  (24)

and, to obtain a finite quantityK, would then require MUR2max . For a positively/negatively curved space k=+1/1 we would instead find the following relation:

ρU=(3/4π)MU/(R3max(1/5)(k/r2)r5+...)=(3/20π)MU/R3max/(18/20π)MU/R3max.:

By substituting coordinates θ by x=cosθ one obtains:

K=32GmMUR2max11x+β1+βxdx                               (25)

K=32GmMUR2max11[x1+βx+β1+βx]dx                               (26)

which can be further integrated to yield:          

K=32GmMUR2max[1β2×1β1+β(y1)dyy+[n(1β)ln(1+β)]                              (27)

and:

K=32GmMUR2max[1β2β+βζδζζ+1+ln1β1+β]                               (28)

or finally leading to:

K(β)=32GmMUR2max[1β2β2ln(1+β1β)2β]                         (29)

From Figure 2 it becomes evident that this force K is vanishing for β0 which is a natural requirement, since for an object at rest, the masses of the homogeneous universe around, due to symmetry reasons, should not induce any net force. Interestingly enough, one can also calculate the typical cosmic braking period τ(β)=β/dβ/dt until differential motions die out given by:

Figure 2 The bracket term [1β2β2ln(1+β1β)2β] of the cosmic braking powerK in Eq. (29) as function of β=U/c decelerating peculiar motions U of stars or galaxies in a universe with a constant value of fracMUR2max .

τ(β)=23R2maxGMuβ[1β2β2ln(1+β1β)2β]                                (30)

which for MUR2max is a finite time period and in general determines the time after which all peculiar galaxy motions should have died out in the universe, i.e. only the rigorous Hubble motion continues to exist in such a "crystalline" universe after that period. This time evidently is dependent on the cosmic value prevalent for R2max/MU or equivalently forρURmax. If these latter values are finite, then the cosmic braking period τ(β) is finite too, and when the universe has an age τH=1/H=R/˙R larger than this period, then all peculiar motions in this universe should have died out.

In an infinite universe Rmax with finite density the expression for K(β) can only be finite, if the density in such a universe scales withρU1/Rmax. Otherwise, if such a physical connection cannot be supported and required with physical sense, the density in such a universe should then simply vanish; i.e.ρU=0!, as it does in a scale-invariant hierarchically structured universe (see Figure 1 in the section above for k=0;k=1).

This above consideration may become a little bit more complicated, if also hereby the problem of the expanding universe has to be taken into account in this problem. Then looking into larger distances may mean that evolutionary earlier cosmic phases of cosmic matter distribution are determining the considered gravitational influences. This means that, with growing distances and longer times it takes to communicate through gravitons the cosmic mass positions to the local position, gravitational influences of earlier evolutionary states of the universe with a higher mass density physically come into the game. This may be taken into account by modifying the above expression for the braking power by:

K=2πGm0ρY(τ)δRUπ0cosθ sinθdθ                              (31)

leading by inclusion of the cosmologically retarded densities to the following expression:

K=2πGm0ρ(t0Ru/c)dRUπ0cosθ' sinθdθ                                (32)

leading with RU0=RU(t0) to:       

K=2πGmρU00(RU0RU(t0Ru/c)3dRU×

×π0cosθ'sinθdθ                   (33)

K=0dRUπ0dθ2π0dϕ.ρUR2UGmR2Ucosθ' sinθ                        (34)

This expression, in a hierarchically structured universe, would write the following way:

K=Gm0ρUdRUπ0δθ2π0dϕ.cosθ 'sinθ                              (35)

and with the differential mass increase in a hierarchic universe given by:

dM(l)=4πρSC,0(lSC,0l)α(1kl2)(1+kl2)4l2dl]                           (36)

then would lead to:       

K=Gm104πρSC,0 . [(lSC,0l)α××(1k(l/Ru)2)1+k(l/Ru)2)dl]π0dθ2π0dϕ . cosθ' . sinθ                          (37)

showing that under a hierarchically structured universe this force K in any case is finite.

Redshifting of cosmic photons

In the above sections the asymmetric action of cosmic mass distributions on a single mass m with a peculiar motion by a velocity U with respect to the rest of the universe (i.e. local standard of rest) was considered, and with β=U/c the following expression has been derived for the net gravitational force that acts on this mass

K(β)=32GmMUR2max[1β2β2ln(1+β1β)2β]                         (38)

As one can see in Figure 2 this expression can also be evaluated forβ1, i.e. relativistic particles or photons moving with the velocityU=c. For photons one would obtain the following result:

K(β=1)=32GmMUR2max[2]                  (39)

Talking about photons here, one can interpret this equation as stating that the temporal change of the momentum of the photon dPν/dt=d/dt(hν/c) is given as the function of the mass of the photon, i.e.m=hν/c2 by

hcdνdt=3Ghνc2MUR2max                             (40)

or describing the change of the photon frequency ν by

dνdt=3GνcMUR2max                  (41)

yielding the following solution for the cosmic frequency shift of cosmic photons during the course of cosmic time:

ν(t)=ν(t0)exp[3GMUcR2max(tt0)]                     (42)

Interestingly enough, this result must be interpreted as a photon redshift which is caused by the asymmetric action of cosmic gravity during the mere passage time or travel distance of the photon since its emission. This cosmic redshift would thus be a pure indicator of the distance which the photon has covered since its emission, and would not have anything to do with the cosmic expansion dynamics of the universe. Galactic photon redshifts could thus not be ascribed to the recession velocity of the photon emitting galaxies. We now use λν=c and λ0ν0=c for a photon with wavelength λ and frequency ν as well as λ=λ0(1+z) at a given redshift z and the above mentioned travel distance D=c(tt0) to get:

1+z=exp[3GMUcR2max(tt0)]=exp[3GMUc2R2maxD]                               (43)

or:

MUR2max=c23GDln(1+z)                            (44)

With z=0.5 und D=300Mpc1025m as typical given values for a galaxy33 the expression MU/R2max yields:     

MUR2max(3108)236.6710111025ln(1.5)kgm2

3006.670.4kgm218kgm2                             (45)

With z=0.1 and D=500Mpc we get 3kgm2.

On the other hand, we can also calculate the expression MU/R2max with typical values of MU1053kg and Rmaxcto1026m 33 - with t0 the age of the universe - to retrieve:

MUR2max10531052=10kgm2                             (46)

which is a very satisfying result since it is in the same order of magnitude.

Conclusion

 In this paper we have picked up the idea of Cassado25 that a "coasting universe", i.e. a universe with an unaccelerated scale expansion velocity˙R=const, may well explain the redshifts of distant supernovae SN-Ia. These puzzling redshifts had led authors like Perlmutter et al.,5–10 to the conclusion that in the more recent cosmic evolution times the universe shows an accelerated expansion and thus requires a non-vanishing positive vacuum energy densityΛ. In order, however, to accept a coasting universe one would need to see very specific cosmic conditions as fulfilled. Kolb20 was the first to study such conditions and concluded that, for this case to be fulfilled, pressure P and matter density ρ of the relevant cosmic matter should be related by a poly-tropic relation of the formP=(1/3)ρ. This then, as shown by the second Friedman equation, leads to a vanishing scale acceleration ¨R. The needed poly-tropic relation, as Kolb20 showed, would characterize a form of matter behavior between baryonic and photonic matter, called by him "K-matter" (Koino-matter). In more recent papers by Fahr et al.,21,22 it was then shown that a coasting universe also results for the Machian case of scale-related cosmic masses leading to a mass density behavior according toρR2. In this paper here we looked into a further possibility to have a coasting universe realized, namely by having a vanishing cosmic mass density. This, at a first glance, looks quite unlikely in view of the stars around us, but as we do show here, such an "empty universe" with ρR=0 naturally results for universes with a pervasive scale-invariant mass structuring as indicated by the observed two-point correlation functions describing stellar or galactic positions (Bahcall et al., 1988). For such universes we can show that the average mass density ρR only is finite for a positively curved universe withk=+1, while for universes with k=0 or k=1 the mass density vanishes , i.e.ρR=0!. These latter universes would be "coasting ones" and thus would, as pointed out by Cassado25 explain the distances of supernovae of type SN-Ia without any need for a vacuum energy Λ.

Appendix: The Olbers paradox in a hierarchically structured universe

The result for the stellar density distribution in a hierarchically structured universe has an interesting consequence for the night-sky luminosity which we want to mention here: If we may assume here that this form of a stellar or galactic clustering continues to larger and larger cosmic distances (i.e.: scale-invariant clustering!), then this fact perhaps could give an evident solution of the Olbers paradox,41 namely the fact that the sky during night is dark. Several other possible solutions meanwhile have been offered, all perhaps worth a discussion, but none convincing up to the present, only one has been overlooked up to now. Because under these above mentioned conditions of a scale-invariant stellar clustering one would simply obtain the following growth O(l) of the illuminated part of the sky in any arbitrary direction with a view cone ofd2Ω:                     

O(l)=1l2d2Ωll0l2d2Ωξ(l)πr2sl2dl=

1l2ll0l2. ξ(l)πr2sl2dl==πr2sl20ξ0. lα0ll01lαdl

=πr2sξ0lα20l1α01α[(ll0)1α1]                            (47)

with rs the standard radius of a standard light candle. First here one can see that for α=0 (i.e. no structuring; homogeneous matter distribution!) one would have the following result

O(l)=πr2sξ0l10[(ll0)1]                  (48)

clearly showing that for increasing values of (l/l0) the sky coverage would grow to O(l)>1 (i.e. illuminated sky =Olbers paradox!). To the contrast, however, for values as observationally confirmed, namely=1.8 , one can see that O(l) always leads to values O(l)<1 (i.e. non-illuminated sky = no Olbers paradox!).43

Acknowledgments

None.

Conflicts of interest

The author declares there is no conflict of interest.

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