Remaining Problems in Interpretation of the Cosmic Microwave Background

Fahr, H. J.; Sokaliwska, Michael

doi:10.1155/2015/503106

Cited by 10 publications

(7 citation statements)

References 44 publications

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“…[12]; [13]). This cooling is expected to explain the present-day CMB temperature T (z = 0) = T 0 ≈ 2.7 K. For a Planck spectrum the energy density γ of the CMB photons and the associated photon number density n γ are given by the well known equations (see [14]; [15]):…”

Section: Energy Density Of Cosmic Photons After the Recombination Eramentioning

confidence: 99%

How are Cosmic Photons Redshifted?

Fahr¹,

Heyl²

2017

AdAp

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According to present cosmological views, the energy density of CMB (Cosmic Microwave Background) photons, freely propagating through the expanding cosmos, varies proportional to 1/S 4 with S being the scale factor of the universe. This behavior is expected because General Theory of Relativity, in application to FLRW-(Friedmann-Lemaitre-Robertson-Walker) cosmological universes, leads to the conclusion that the photon wavelengths increase during their free passage through the spacetime metrics of the universe by the same factor as does the scale factor S. This appears to be a reasonable explanation for the presently observed Planckian CMB spectrum with its actual temperature of about 2.7 K, while at the time of its origin after the last scattering during the recombination phase its temperature should have been about 3000 K, at an epoch of about 380 ky after the Big Bang, when the scale of the universe Sr was smaller by roughly a factor of S/Sr = 1 + zr = 1100 compared to the present scale S = S0 of the universe. In this paper we start from putting the question whether the scale-behavior of the CMB energy density that enters the energy-momentum tensor of the field equations describing the expanding universe is really falling off like S −4 and, if in fact a deviation from a behavior according to S −4 would occur, why do we nevertheless presently observe a CMB energy density which appears to be in accordance with such a S −4 -scaling? This question arises from another basic and fundamental question, namely: Can we really assume that the wavelength of the freely propagating photon during its travel all the way along its light geodetic is permanently affected by the expansion of the universe, i.e continuously recognizes the expansion of the cosmic scale S? With other words: Do freely propagating photons really undergo a permanent change of their wavelengths when freely traveling through cosmic space-time or is the observationally apparent energy loss of cosmologically red-shifted photons an effect which only occurs just in the moment of photon registration at some specific world point? If the latter would prove to be true , then it would mean that the energy density of freely propagating, non-interacting CMB photons, due to non-changing, conserved wavelengths, is behaving with respect to cosmic scale variation different from conventional expectations, but rather would turn out to behave just like the energy density of matter, namely according to S −3 . Hence the photon part of the energy momentum tensor would become different and associated solutions of FLRW-equations would undergo corresponding modifications. In consequence, the CMB energy density as far as it enters the energy-momentum tensor generated by freely propagating CMB photons during the expansion period of the universe after the recombination era would no longer become negligible for the cosmic dynamics, since its value would stay in the same order of magnitude as that of baryonic or dark matter.

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Section: Energy Density Of Cosmic Photons After the Recombination Eramentioning

confidence: 99%

How are Cosmic Photons Redshifted?

Fahr¹,

Heyl²

2017

AdAp

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“…According to the standard model of cosmology, the spectral character of local thermodynamic equilibrium (LTE) photons created during the phase of recombination just before the last photon scattering, say at z r ≈ 1,100 under conventional CMB assumptions, can be described by a Planck distribution with a temperature T r ≈ 3000 K. Because of the expansion of the Universe, the wavelengths of the free CMB photons are usually assumed to increase, and only because of that the spectrum stays Planckian, since then the Planck temperature of the CMB photons decreases according to T(z) = (1 + z) ⋅ T 0 (see e.g., Fahr & Sokaliwska, 2015;Fahr & Zoennchen, 2009). This cooling is expected to explain the present-day CMB temperature T(z = 0) = T 0 ≈ 2.7 K. For a Planck spectrum, the energy density of the CMB photons and the associated photon number density n are given by the following well-known equations (see Peebles, 1993;Sciama, 1971):…”

Section: Energy Density Of Photons After the Recombination Eramentioning

confidence: 99%

Retracted: New aspects of photon propagation in expanding universes

Fahr

Heyl

2017

Astron Nachr

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Background: Modern cosmology assumes that the cosmic microwave background (CMB) radiation is a relict of the much hotter electromagnetic radiation field from the early recombination era of the universe. Its present very low radiation temperature T CMB = 2.735 K thereby is explained by the fact that the cosmic photons in the expanding universe undergo a wavelength stretching according to 𝜆/𝜆0 = S/S 0 , where S denotes the scale of the universe. The present-day CMB temperature hence simply expresses the factor by which the universe has grown since the recombination era. Materials and Methods: On the basis of well-known facts of Special and General Relativity (SRT and GRT), we reinvestigate the behavior of freely propagating cosmic photons in dynamic Robertson-Walker spacetime geometries and show that in the system of the propagating photon, due to the fact that no time lapses in this proper system, the photon does not change its initial state, that is, its wavelength and energy. We do, however, also show that the global beat of the time changes with the cosmic world time or the cosmic scale S. That means cosmic photons do not change their state, till they are registered by a local detector, that is, a local clock. Results: We claim that the energy density of cosmic photons which enters the energy-momentum tensor of Einstein's GRT field equations does not scale like S −4 as assumed in present-day cosmology, but like S −3 , that is, identically to the behavior of the energy densities of baryonic or dark matter, meaning that the energy density of photons in the present-day universe cannot be neglected, but counts substantially for the expansion history of the universe. Nevertheless, we show that cosmic photons measured with a present-day detector (local clock) locally will show their cosmological redshift, explaining the present-day CMB Planck spectrum with a Planck temperature of 2.735 K. Conclusions: As the energy density of cosmic photons cannot be neglected, their contribution in the GRT energy-momentum tensor is important over all phases of the expansion of the universe. They are thus acting identical to the way how dark matter acts and influences cosmic expansion. This means that the present-day claim for a dark matter contribution in cosmic expansion by Ω dark ≃ 0.23 can be substantially relaxed.

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“…For Planckian emitters like stars and the CMB the famous Wien's law of spectral maximum shifts would then require the following relation between Planckian spectral peak wave lengths λ max (z = 0) at the origin and λ max (z = z g ) at present time, respectively, given by the following relation [18]: Taking the temperature of the initial Planck emitter to be T CMB (z = 0) = 3000K and the temperature of the presently seen CMB emitter as T CMB (z = zg) = 3K this would mean the following request:…”

Section: Thinking Of the Most Distant Emitters And The Cosmic Microwamentioning

confidence: 99%

Untitled

2020

ATCP

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Cosmologists present clear observational evidences that stellar objects like stars and galaxies do carry out pronounced proper motions, and the question may be raising how these peculiar motions might evolve in time. In this article we study these peculiar motions of single objects, independent whether of microscopic or macroscopic nature, embedded in a globally homogeneous, static, massive universe with inherent gravity. Aims: We show that these objects at their motions, even in a homogeneous universe around them, are permanently subject to net gravitational forces due to the fact that in a post-Newtonian relativistic treatment the sources of cosmic masses are seen under retarded positions, retarded by the time it takes to communicate via gravitons the positions of these masses to the moving object. Methods: This "aberrational" recognition of massive source points on the one hand leads to a braking power permanently decelerating the peculiar motion of any cosmic object, on the other hand it also effects the wave lengths of all photons freely propagating through cosmic space under the action of cosmic gravity. Photons, even in a static homogeneous universe, undergo a permanent red-shifting, since working permanently against a net gravitational force from the direction opposite to the photon's propagation direction. Results: We do show that the observationally confirmed redshifts of photons from distant galaxies under the new auspices appear as a pure measure of the distance which the photons passed from its galactic emitter to us. In this view redshifts have nothing to do with the Hubble dynamics of the universe and its emitters. Since, however, the existence of Hubble-induced redshifts cannot be excluded, we also look into a combination of both, gravitationally induced redshifts zg and Hubble-induced redshifts zH. We show that gravitationally induced redshifts zg of course also appear in an expanding universe, and it can be demonstrated that for instance in a "coasting universe" with a constant expansion rate R˙ and with R α t both these redshifts zg and zH would lead to similar results.

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Remaining Problems in Interpretation of the Cosmic Microwave Background

Cited by 10 publications

References 44 publications

How are Cosmic Photons Redshifted?

How are Cosmic Photons Redshifted?

Retracted: New aspects of photon propagation in expanding universes

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