The generalized second law of thermodynamics in viscous Ricci dark energy model

This paper is devoted to check the validity of laws of thermodynamics for Kaluza–Klein universe in the state of thermal equilibrium, composed of dark matter and dark energy. The generalized holographic dark energy and generalized Ricci dark energy models are considered here. It is proved that the first and generalized second law of thermodynamics are valid on the apparent horizon for both of these models. Further, we take a horizon of radius L with modified holographic or Ricci dark energy. We conclude that these models do not obey the first and generalized second law of thermodynamics on the horizon of fixed radius L for a specific range of model parameters.

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Generalized holographic Ricci dark energy and generalized second law of thermodynamics in Bianchi Type I universe

General Relativity and Gravitation ◽

10.1007/s10714-015-1983-4 ◽

2015 ◽

Vol 47 (11) ◽

Cited By ~ 7

Author(s):

En-Kun Li ◽

Yu Zhang ◽

Jin-Ling Geng ◽

Peng-Fei Duan

Keyword(s):

Dark Energy ◽

Bianchi Type ◽

Second Law Of Thermodynamics ◽

Second Law ◽

Type I ◽

Ricci Dark Energy ◽

Bianchi Type I ◽

Generalized Second Law ◽

Bianchi Type I Universe

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Viscous Ricci dark energy and generalized second law of thermodynamics in modified f(R, T) gravity

Modern Physics Letters A ◽

10.1142/s0217732318502255 ◽

2018 ◽

Vol 33 (38) ◽

pp. 1850225 ◽

Cited By ~ 1

Author(s):

C. P. Singh ◽

Ajay Kumar

Keyword(s):

Dark Energy ◽

Apparent Horizon ◽

Second Law Of Thermodynamics ◽

Second Law ◽

Fluid Viscosity ◽

Ricci Dark Energy ◽

Evolution Of The Universe ◽

Generalized Second Law ◽

The Future ◽

The Universe

The motivation of this paper is to study the bulk viscosity effect in Ricci dark energy (RDE) model within the framework of modified f(R, T) gravity, where R is the Ricci scalar and T is the trace of the energy–momentum tensor. As most studies assume that the universe is filled with a perfect fluid, viscosity is expected to present at least during some stages, especially in the early stage of the evolution of the universe but it could still become significant in the future. We assume the universe is filled with viscous RDE and pressureless dark matter. We consider the total bulk viscous coefficient is in the form of [Formula: see text][Formula: see text]H, where [Formula: see text] and [Formula: see text] are the constants. We obtain the solutions to the modified field equations by assuming a form f(R, T) = R [Formula: see text] T, where [Formula: see text] is a constant. We find the scale factor and deceleration parameter, and classify all possible evolutions of the universe. We briefly discuss the future finite-time singularity and show that the Big Rip singularity appears in viscous RDE model. We investigate two geometrical diagnostics, statefinder parameter and Om to analyze the dynamics of evolution of the universe. The trajectories of statefinder parameter reveal that the model behaves like quintessence for small [Formula: see text], and for large [Formula: see text] it shows the Chaplygin gas-like. However, in late time both the models approach [Formula: see text]CDM. The model shows a transition from decelerated phase to accelerated phase. Similarly, the Om analysis reveals that the model behaves like quintessence for small [Formula: see text] and phantom-like for large [Formula: see text]. We extend our study to analyze the time evolution of the total entropy and generalized second law of thermodynamics of viscous RDE model in f(R, T) theory inside the apparent horizon. Our study shows that the generalized second law of thermodynamics always preserves in viscous RDE model in a region enclosed by the apparent horizon under the suitable constraints of viscous coefficients.

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f(T) GRAVITY FROM HOLOGRAPHIC RICCI DARK ENERGY MODEL WITH NEW BOUNDARY CONDITIONS

Modern Physics Letters A ◽

10.1142/s021773231350171x ◽

2013 ◽

Vol 28 (39) ◽

pp. 1350171 ◽

Cited By ~ 2

Author(s):

PENG HUANG ◽

YONG-CHANG HUANG ◽

FANG-FANG YUAN

Keyword(s):

Dark Energy ◽

Boundary Conditions ◽

Dark Energy Model ◽

Energy Model ◽

Ricci Dark Energy ◽

Expected Information ◽

Better Than

Commonly used boundary conditions in reconstructing f(T) gravity from holographic Ricci dark energy (RDE) model are found to cause some problem, we therefore propose new boundary conditions in this paper. By reconstructing f(T) gravity from the RDE with these new boundary conditions, we show that the new ones are better than the present commonly used ones since they can give the physically expected information, which is lost when the commonly used ones are taken in the reconstruction, of the resulting f(T) theory. Thus, the new boundary conditions proposed here are more suitable for the reconstruction of f(T) gravity.

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Constraints on the Ricci dark energy cosmologies in Bianchi type I model

International Journal of Geometric Methods in Modern Physics ◽

10.1142/s021988782150095x ◽

2021 ◽

pp. 2150095

Author(s):

H. Hossienkhani ◽

N. Azimi ◽

H. Yousefi

Keyword(s):

Dark Energy ◽

Dark Energy Model ◽

Bianchi Type ◽

Energy Model ◽

Accelerated Expansion ◽

Likelihood Method ◽

Type I ◽

Ricci Dark Energy ◽

Bianchi Type I ◽

The Impact

The impact of anisotropy on the Ricci dark energy cosmologies is investigated where it is assumed that the geometry of the universe is described by Bianchi type I (BI) metric. The main goal is to determine the astrophysical constraints on the model by using the current available data as type Ia supernovae (SNIa), the Baryon Acoustic Oscillation (BAO), and the Hubble parameter [Formula: see text] data. In this regard, a maximum likelihood method is applied to constrain the cosmological parameters. Combining the data, it is found out that the allowed range for the density parameter of the model stands in [Formula: see text]. With the help of the Supernova Legacy Survey (SNLS) sample, we estimate the possible dipole anisotropy of the Ricci dark energy model. Then, by using a standard [Formula: see text] minimization method, it is realized that the transition epoch from early decelerated to current accelerated expansion occurs faster in Ricci dark energy model than [Formula: see text]CDM model. The results indicate that the BI model for the Ricci dark energy is consistent with the observational data.

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