Cosmology via thermodynamics of polytropic gas

2017 ◽  
Vol 32 (32) ◽  
pp. 1750177 ◽  
Author(s):  
Muzaffer Askin ◽  
Mustafa Salti ◽  
Oktay Aydogdu
Keyword(s):  
Dark Matter ◽  
Scalar Field ◽  
Energy Density ◽  
Exact Expression ◽  
Frw Universe ◽  
Polytropic Gas ◽  
Friedmann Robertson Walker ◽  
Matter Energy

We study cosmological scenarios of the polytropic gas (PG) dark matter-energy proposal in a Friedmann–Robertson–Walker (FRW) Universe. As a first step, we obtain an exact expression for the energy density of PG model by making use of the thermodynamics. Later, we investigate some cosmological quantities and perform neo-classical analyzes. Finally, we implement a connection between the PG and a homogenous minimally coupled scalar field by introducing its self-interacting potential.

scholarly journals Tachyonic matter cosmology with exponential and hyperbolic potentials

2017 ◽  
Vol 26 (02) ◽  
pp. 1750012 ◽  
Author(s):  
B. Pourhassan ◽  
J. Naji
Keyword(s):  
Scalar Field ◽  
Observational Data ◽  
Cosmological Parameters ◽  
Field Potentials ◽  
Exponential Potential ◽  
Frw Universe ◽  
Hyperbolic Cosine ◽  
Special Cases ◽  
Friedmann Robertson Walker ◽  
Type Potential

In this paper, we consider tachyonic matter in spatially flat Friedmann–Robertson–Walker (FRW) universe, and obtain behavior of some important cosmological parameters for two special cases of potentials. First, we assume the exponential potential and then consider hyperbolic cosine type potential. In both cases, we obtain behavior of the Hubble, deceleration and EoS parameters. Comparison with observational data suggest the model with hyperbolic cosine type scalar field potentials has good model to describe universe.

scholarly journals SPECTRA OF RELIC GRAVITONS AND BRANS–DICKE THEORY

2005 ◽  
Vol 20 (02) ◽  
pp. 127-134 ◽  
Author(s):  
B. K. SAHOO
Keyword(s):  
Scalar Field ◽  
Energy Density ◽  
Time Dependence ◽  
Gravitational Waves ◽  
Hubble Parameter ◽  
Frequency Dependent ◽  
Cosmological Expansion ◽  
Relic Gravitational Waves ◽  
Matter Energy ◽  
Inflationary Models

The spectra of relic gravitational waves produced as a result of cosmological expansion of the inflationary models are derived in Brans–Dicke (BD) theory of gravity. The time dependence of the very early Hubble parameter and matter energy density are derived from frequency-dependent spectrum of relic gravitational waves. Also it is found that Brans–Dicke scalar field contributes to the energy density of relic gravitons.

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

2006 ◽  
Vol 21 (15) ◽  
pp. 1241-1248 ◽  
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.

scholarly journals NEW PHYSICS AT LOW ENERGIES AND DARK MATTER-DARK ENERGY TRANSMUTATION

2005 ◽  
Vol 20 (06) ◽  
pp. 1140-1147 ◽  
Author(s):  
E. I. GUENDELMAN ◽  
A. B. KAGANOVICH
Keyword(s):  
Field Theory ◽  
Dark Matter ◽  
Dark Energy ◽  
Energy Density ◽  
Cold Dark Matter ◽  
Late Time ◽  
Frw Universe ◽  
Dark Energy Density ◽  
Total Energy Density ◽  
Fermion Fields

A field theory is proposed where the regular fermionic matter and the dark fermionic matter can be different states of the same "primordial" fermion fields. In regime of the fermion densities typical for normal particle physics, the primordial fermions split into three families identified with regular fermions. When fermion energy density becomes comparable with dark energy density, the theory allows transition to new type of states. The possibility of such Cosmo-Low Energy Physics (CLEP) states is demonstrated by means of solutions of the field theory equations describing FRW universe filled with homogeneous scalar field and uniformly distributed nonrelativistic neutrinos. Neutrinos in CLEP state are drawn into cosmological expansion by means of dynamically changing their own parameters. One of the features of the fermions in CLEP state is that in the late time universe their masses increase as a3/2 (a=a(t) is the scale factor). The energy density of the cold dark matter consisting of neutrinos in CLEP state scales as a sort of dark energy; this cold dark matter possesses negative pressure and for the late time universe its equation of state approaches that of the cosmological constant. The total energy density of such universe is less than it would be in the universe free of fermionic matter at all.

scholarly journals FORM INVARIANCE SYMMETRY GENERATES A LARGE SET OF FRW COSMOLOGIES

2013 ◽  
Vol 28 (04) ◽  
pp. 1250236 ◽  
Author(s):  
LUIS P. CHIMENTO ◽  
MARTÍN G. RICHARTE ◽  
IVÁN E. SÁNCHEZ
Keyword(s):  
Scalar Field ◽  
Energy Density ◽  
Group Structure ◽  
Kinetic Energy Density ◽  
Large Set ◽  
Field Equations ◽  
Form Invariance ◽  
Hubble Expansion ◽  
Large Sets ◽  
Friedmann Robertson Walker

We show that Einstein's field equations for spatially flat Friedmann–Robertson–Walker (FRW) spacetimes have a form invariance symmetry (FIS) realized by the form invariance transformations (FIT) which are indeed generated by an invertible function of the source energy density. These transformations act on the Hubble expansion rate, the energy density and pressure of the cosmic fluid; likewise such transformations are endowed with a Lie group structure. Each representation of this group is associated with a particular fluid and consequently a determined cosmology, so that, the FIS defines a set of equivalent cosmological models. We focus our seek in the FIT generated by a linear function because it provides a natural framework to express the duality and also produces large sets of cosmologies, starting from a seed one, in several contexts as for instance in the cases of a perfect fluid source and a scalar field driven by a potential depending linearly on the scalar field kinetic energy density.

scholarly journals Updating the axion cold dark matter energy density

2008 ◽  
Vol 2008 (09) ◽  
pp. 005 ◽  
Author(s):  
Kyu Jung Bae ◽  
Ji-Haeng Huh ◽  
Jihn E Kim
Keyword(s):  
Dark Matter ◽  
Energy Density ◽  
Cold Dark Matter ◽  
Matter Energy

scholarly journals Reconstruction of the New Agegraphic Polytropic Gas Dark Energy Model in the Flat Friedmann Robertson Walker (FRW) Universe

2021 ◽  
Vol 13 (3) ◽  
pp. 779-784
Author(s):  
P. Das ◽  
K. P. Singh
Keyword(s):  
Dark Energy ◽  
Dark Energy Model ◽  
Scalar Fields ◽  
Energy Model ◽  
Accelerated Expansion ◽  
Frw Universe ◽  
Agegraphic Dark Energy ◽  
New Agegraphic Dark Energy ◽  
Polytropic Gas ◽  
Friedmann Robertson Walker

In this paper, we study the Polytropic Gas Dark Energy model and New Agegraphic Dark Energy model in the flat Friedmann Robertson Walker (FRW) Universe and establish a correspondence between them for the scalar fields. This correspondence allows reconstructing the potential of the Polytropic Gas scalar fields and dynamics of the scalar fields according to the evolutions of the New Agegraphic Dark Energy, which describes the accelerated expansion of the Universe.

scholarly journals On multifluid perturbations in scalar–tensor cosmology

2020 ◽  
pp. 2050120
Author(s):  
Joseph Ntahompagaze ◽  
Shambel Sahlu ◽  
Amare Abebe ◽  
Manasse R. Mbonye
Keyword(s):  
Scalar Field ◽  
Energy Density ◽  
Power Law ◽  
Scalar Tensor Theory ◽  
Frw Cosmology ◽  
Static Approximation ◽  
Covariant Approach ◽  
Tensor Theory ◽  
Text Model ◽  
Friedmann Robertson Walker

In this paper, the scalar–tensor theory is applied to the study of perturbations in a multifluid universe, using the [Formula: see text] covariant approach. Both scalar and harmonic decompositions are instituted on the perturbation equations. In particular, as an application, we study perturbations on a background Friedmann-Robertson-Walker (FRW) cosmology consisting of both radiation and dust in the presence of a scalar field. We consider both radiation-dominated and dust-dominated epochs, respectively, and study the results. During the analysis, quasi-static approximation is instituted. It is observed that the fluctuations of the energy density decrease with increasing redshift, for different values of [Formula: see text] of a power-law [Formula: see text] model.

scholarly journals ACCELERATING UNIVERSES WITH SCALING DARK MATTER

2001 ◽  
Vol 10 (02) ◽  
pp. 213-223 ◽  
Author(s):  
MICHEL CHEVALLIER ◽  
DAVID POLARSKI
Keyword(s):  
Dark Matter ◽  
Equation Of State ◽  
Energy Density ◽  
Critical Points ◽  
Equations Of State ◽  
Large Fraction ◽  
Accurate Knowledge ◽  
Friedmann Robertson Walker

Friedmann–Robertson–Walker universes with a presently large fraction of the energy density stored in an X-component with wX<-1/3, are considered. We find all the critical points of the system for constant equations of state in that range. We consider further several background quantities that can distinguish the models with different wXvalues. Using a simple toy model with a varying equation of state, we show that even a large variation of wXat small redshifts is very difficult to observe with dL(z) measurements up to z~1. Therefore, it will require accurate measurements in the range 1<z<2 and independent accurate knowledge of Ωm,0(and/or ΩX,0) in order to resolve a variable wXfrom a constant wX.

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