The basic blocks of the universe matter: Boltzmann fundamental particle and energy quanta of dark matter and dark energy

In order to test if there is energy transfer between dark energy (DE) and dark matter (DM), we investigate cosmological constraints on two forms of nontrivial interaction between the DM sector and the sector responsible for the acceleration of the universe, in light of the newly revised observations including OHD, CMB, BAO and SNe Ia. More precisely, we find the same tendencies for both phenomenological forms of the interaction term Q = 3γHρ, i.e. the parameter γ to be a small number, |γ| ≈ 10-2. However, concerning the sign of the interaction parameter, we observe that γ > 0 when the interaction between dark sectors is proportional to the energy density of dust matter, whereas the negative coupling (γ < 0) is preferred by observations when the interaction term is proportional to DE density. We further discuss two possible explanations to this incompatibility and apply a quantitative criteria to judge the severity of the coincidence problem. Results suggest that the γm IDE model with a positive coupling may alleviate the coincidence problem, since its coincidence index C is smaller than that for the γd IDE model, the interacting quintessence and phantom models by four orders of magnitude.

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On The Symmetry of The Universe

10.20944/preprints202007.0736.v1 ◽

2020 ◽

Author(s):

Engel Roza

Keyword(s):

Dark Matter ◽

Dark Energy ◽

Thermodynamic Equilibrium ◽

Vacuum Energy ◽

Quantum Mechanical ◽

Baryonic Matter ◽

Time Uncertainty ◽

Matter Effect ◽

Mechanical Interpretation ◽

The Universe

It is shown that the Lambda component in the cosmological Lambda-CDM model can be conceived as vacuum energy, consisting of gravitational particles subject to Heisenberg’s energy-time uncertainty. These particles can be modelled as elementary polarisable Dirac-type dipoles (“darks”) in a fluidal space at thermodynamic equilibrium, with spins that are subject to the Bekenstein-Hawking entropy. Around the baryonic kernels, uniformly distributed in the universe, the spins are polarized, thereby invoking an increase of the effective gravitational strength of the kernels. It explains the dark matter effect to the extent that the numerical value of Milgrom’s acceleration constant can be assessed by theory. Non-polarized vacuum particles beyond the baryonic kernels compose the dark energy. The result is a quantum mechanical interpretation of gravity in terms of quantitatively established shares in baryonic matter, dark matter and dark energy, which correspond with the values of the Lambda-CDM model..

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Observational constraints of a new unified dark fluid and the H0 tension

Monthly Notices of the Royal Astronomical Society ◽

10.1093/mnras/stz2753 ◽

2019 ◽

Vol 490 (2) ◽

pp. 2071-2085 ◽

Cited By ~ 10

Author(s):

Weiqiang Yang ◽

Supriya Pan ◽

Andronikos Paliathanasis ◽

Subir Ghosh ◽

Yabo Wu

Keyword(s):

Dark Matter ◽

Dark Energy ◽

Large Scale ◽

Cold Dark Matter ◽

Early Time ◽

Observational Constraints ◽

Minimal Extension ◽

Energy Evolution ◽

The Universe ◽

Different Sources

ABSTRACT Unified cosmological models have received a lot of attention in astrophysics community for explaining both the dark matter and dark energy evolution. The Chaplygin cosmologies, a well-known name in this group have been investigated matched with observations from different sources. Obviously, Chaplygin cosmologies have to obey restrictions in order to be consistent with the observational data. As a consequence, alternative unified models, differing from Chaplygin model, are of special interest. In the present work, we consider a specific example of such a unified cosmological model, that is quantified by only a single parameter μ, that can be considered as a minimal extension of the Λ-cold dark matter cosmology. We investigate its observational boundaries together with an analysis of the universe at large scale. Our study shows that at early time the model behaves like a dust, and as time evolves, it mimics a dark energy fluid depicting a clear transition from the early decelerating phase to the late cosmic accelerating phase. Finally, the model approaches the cosmological constant boundary in an asymptotic manner. We remark that for the present unified model, the estimations of H0 are slightly higher than its local estimation and thus alleviating the H0 tension.

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Do we come from a quantum anomaly?

International Journal of Modern Physics D ◽

10.1142/s0218271819440024 ◽

2019 ◽

Vol 28 (14) ◽

pp. 1944002 ◽

Cited By ~ 9

Author(s):

Spyros Basilakos ◽

Nick E. Mavromatos ◽

Joan Solà Peracaula

Keyword(s):

Dark Matter ◽

Dark Energy ◽

Energy Density ◽

Hubble Parameter ◽

Vacuum Energy ◽

Vacuum Energy Density ◽

Quantum Anomaly ◽

Inflationary Phase ◽

Axion Field ◽

The Universe

We present a string-based picture of the cosmological evolution in which (CP-violating) gravitational anomalies acting during the inflationary phase of the universe cause the vacuum energy density to “run” with the effective Hubble parameter squared, [Formula: see text], thanks to the axion field of the bosonic string multiplet. This leads to baryogenesis through leptogenesis with massive right-handed neutrinos. The generation of chiral matter after inflation helps in cancelling the anomalies in the observable radiation- and matter-dominated eras. The present era inherits the same “running vacuum” structure triggered during the inflationary time by the axion field. The current dark energy is thus predicted to be mildly dynamical, and dark matter should be made of axions. Paraphrasing Carl Sagan [ https://www.goodreads.com/author/quotes/10538.Carl_Sagan .]: we are all anomalously made from starstuff.

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RECONSTRUCTION OF 5D COSMOLOGICAL MODELS FROM RECENT OBSERVATIONS

International Journal of Modern Physics D ◽

10.1142/s021827180701095x ◽

2007 ◽

Vol 16 (10) ◽

pp. 1573-1579

Author(s):

CHENGWU ZHANG ◽

LIXIN XU ◽

YONGLI PING ◽

HONGYA LIU

Keyword(s):

Dark Matter ◽

Dark Energy ◽

Equation Of State ◽

Cosmological Solution ◽

Type Ia Supernovae ◽

Shift Parameter ◽

Type Ia ◽

Ia Supernovae ◽

Best Fit ◽

The Universe

We use a parameterized equation of state (EOS) of dark energy to a 5D Ricci-flat cosmological solution and suppose the universe contains two major components: dark matter and dark energy. Using the recent observational datasets: the latest 182 type Ia Supernovae Gold data, the three-year WMAP CMB shift parameter and the SDSS baryon acoustic peak, we obtain the best fit values of the EOS and two major components' evolution. We find that the best fit EOS crosses -1 in the near past where z ≃ 0.07, the present best fit value of wx(0) < -1 and for this model, the universe experiences the acceleration at about z ≃ 0.5.

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Cosmology from multimeasure multifield model

International Journal of Modern Physics A ◽

10.1142/s0217751x19500994 ◽

2019 ◽

Vol 34 (19) ◽

pp. 1950099 ◽

Cited By ~ 5

Author(s):

Denitsa Staicova ◽

Michail Stoilov

Keyword(s):

Dark Matter ◽

Dark Energy ◽

Model Potential ◽

Higgs Mechanism ◽

Evolution Of The Universe ◽

Slow Roll ◽

Cosmological Application ◽

Proposed Model ◽

Model Setup ◽

The Universe

We consider the cosmological application of a (variant of) relatively newly proposed model1 unifying inflation, dark energy, dark matter, and the Higgs mechanism. The model was originally defined using additional non-Riemannian measures, but it can be reformulated into effective quintessential model unifying inflation, dark energy and dark matter. Here, we demonstrate numerically that it is capable of describing the entire evolution of the Universe in a seamless way, but this requires some revision of the model setup. The main reason is that there is a strong effective friction in the model, a feature which has been neglected in the pioneer work. This improves the model potential for proper description of the evolution of the Universe, because the friction ensures a finite time inflation with dynamically maintained low-value slow-roll parameters in the realistic scenarios. In addition, the model predicts the existence of a constant scalar field in late Universe.

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The accelerating universe and dark energy

International Journal of Modern Physics D ◽

10.1142/s0218271814300122 ◽

2014 ◽

Vol 23 (06) ◽

pp. 1430012 ◽

Cited By ~ 2

Author(s):

Charles Baltay

Keyword(s):

Dark Matter ◽

Dark Energy ◽

Cosmological Parameters ◽

Accelerating Universe ◽

Heavy Particles ◽

Familiar World ◽

Acceleration Of The Universe ◽

Expansion Of The Universe ◽

The Universe ◽

Present Understanding

The recent discovery by Riess et al.1 and Perlmutter et al.2 that the expansion of the universe is accelerating is one of the most significant discoveries in cosmology in the last few decades. To explain this acceleration a mysterious new component of the universe, dark energy, was hypothesized. Using general relativity (GR), the measured rate of acceleration translates to the present understanding that the baryonic matter, of which the familiar world is made of, is a mere 4% of the total mass-energy of the universe, with nonbaryonic dark matter making up 24% and dark energy making up the majority 72%. Dark matter, by definition, has attractive gravity, and even though we presently do not know what it is, it could be made of the next heavy particles discovered by particle physicists. Dark energy, however, is much more mysterious, in that even though we do not know what it is, it must have some kind of repulsive gravity and negative pressure, very unusual properties that are not part of the present understanding of physics. Investigating the nature of dark energy is therefore one of the most important areas of cosmology. In this review, the cosmology of an expanding universe, based on GR, is discussed. The methods of studying the acceleration of the universe, and the nature of dark energy, are presented. A large amount of experimentation on this topic has taken place in the decade since the discovery of the acceleration. These are discussed and the present state of knowledge of the cosmological parameters is summarized in Table 7 below. A vigorous program to further these studies is under way. These are presented and the expected results are summarized in Table 10 below. The hope is that at the end of this program, it would be possible to tell whether dark energy is due to Einstein's cosmological constant or is some other new constituent of the universe, or alternately the apparent acceleration is due to some modification of GR.

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Pilgrim dark energy models in fractal universe

International Journal of Modern Physics D ◽

10.1142/s0218271817500493 ◽

2016 ◽

Vol 26 (06) ◽

pp. 1750049 ◽

Cited By ~ 2

Author(s):

Abdul Jawad ◽

Shamaila Rani ◽

Ines G. Salako ◽

Faiza Gulshan

Keyword(s):

Dark Matter ◽

Dark Energy ◽

Cold Dark Matter ◽

Accelerated Expansion ◽

Freezing And Thawing ◽

Eos Parameter ◽

Pilgrim Dark Energy ◽

Energy Models ◽

Expansion Behavior ◽

The Universe

We discuss the cosmological implications of interacting pilgrim dark energy (PDE) models (with Hubble, Granda–Oliveros and generalized ghost cutoffs) with cold dark matter ([Formula: see text]CDM) in fractal cosmology by assuming the flat universe. We observe that the Hubble parameter lies within observational suggested ranges while deceleration parameter represents the accelerated expansion behavior of the universe. The equation of state (EoS) parameter ([Formula: see text]) corresponds to the quintessence region and phantom region for different cases of [Formula: see text]. Further, we can see that [Formula: see text]–[Formula: see text] (where prime indicates the derivative with respect to natural logarithmic of scale factor) plane describes the freezing and thawing regions and also corresponds to [Formula: see text] limit for some cases of [Formula: see text] (PDE parameter). It is also noted that the [Formula: see text]–[Formula: see text] (state-finder parameters) plane corresponds to [Formula: see text] limit and also shows the Chaplygin as well as phantom/quintessence behavior. It is observed that pilgrim dark energy models in fractal cosmology expressed the consistent behavior with recent observational schemes.

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THE HIGGS PORTAL AND AN UNIFIED MODEL FOR DARK ENERGY AND DARK MATTER

International Journal of Modern Physics A ◽

10.1142/s0217751x08042675 ◽

2008 ◽

Vol 23 (30) ◽

pp. 4817-4827 ◽

Cited By ~ 45

Author(s):

O. BERTOLAMI ◽

R. ROSENFELD

Keyword(s):

Dark Matter ◽

Dark Energy ◽

Higgs Boson ◽

Higgs Field ◽

Vacuum Expectation ◽

Classical Field ◽

Dark Matter Candidate ◽

Hidden Sector ◽

Quintessence Field ◽

The Universe

We examine a scenario where the Higgs boson is coupled to an additional Standard Model singlet scalar field from a hidden sector. We show that, in the case where this field is very light and has already relaxed to its nonzero vacuum expectation value, one gets a very stringent limit on the mixing angle between the hidden sector scalar and the Higgs field from fifth force experiments. However, this limit does not imply in a small coupling due to the large difference of vacuum expectation values. In the case that the hidden sector scalar is identified with the quintessence field, responsible for the recent acceleration of the universe, the most natural potential describing the interaction is disfavored since it results in a time-variation of the Fermi scale. We show that an ad hoc modification of the potential describing the Higgs interaction with the quintessence field may result in an unified picture of dark matter and dark energy, where dark energy is the zero-mode classical field rolling the usual quintessence potential and the dark matter candidate is the quantum excitation (particle) of the field, which is produced in the universe due to its coupling to the Higgs boson. This coupling also generates a mass for the new particle that, contrary to usual quintessence models, does not have to be small, since it does not affect the evolution of classical field. In this scenario, a feasible dark matter density can be, under conditions, obtained.

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CAN BRANS–DICKE SCALAR FIELD ACCOUNT FOR DARK ENERGY AND DARK MATTER?

Modern Physics Letters A ◽

10.1142/s021773230602055x ◽

2006 ◽

Vol 21 (15) ◽

pp. 1241-1248 ◽

Cited By ~ 32

Author(s):

M. ARIK ◽

M. C. ÇALIK

Keyword(s):

Dark Matter ◽

Dark Energy ◽

Scalar Field ◽

Energy Density ◽

Late Time ◽

Energy Contribution ◽

Time Solution ◽

The Universe

By using a linearized non-vacuum late time solution in Brans–Dicke cosmology, we account for the 75% dark energy contribution but not for approximately 23% dark matter contribution to the present day energy density of the universe.

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