Bianchi type-I and -III modified holographic Ricci Dark energy models in Saez-Ballester theory

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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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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Anisotropic universe and reconstructing f(R, T) theory from holographic Ricci dark energy

Canadian Journal of Physics ◽

10.1139/cjp-2016-0735 ◽

2017 ◽

Vol 95 (5) ◽

pp. 524-534 ◽

Cited By ~ 5

Author(s):

V. Fayaz ◽

H. Hossienkhani ◽

Z. Zarei ◽

M. Ganji ◽

N. Azimi

Keyword(s):

Dark Energy ◽

Bianchi Type ◽

Equations Of State ◽

State Parameter ◽

Accelerated Expansion ◽

Anisotropic Universe ◽

Density Parameter ◽

Type I ◽

Ricci Dark Energy ◽

Bianchi Type I

In this work, we regard f(R, T) gravity as an effective description of the acceleration of the universe and reconstruct the function f(R, T) from the holographic Ricci dark energy by considering a Bianchi type I universe. So the connection gives us an opportunity to redefine the Hubble parameter, the pressure, the equations of state parameter, and the energy density parameter representation by considering Bianchi type I models for holographic Ricci dark energy. We wrap up the evolution of the accelerated expansion of the anisotropic universe, which is faster than the evolution of the FRW and ΛCDM models.

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A new class of holographic dark energy models in LRS Bianchi Type-I

International Journal of Modern Physics A ◽

10.1142/s0217751x21502560 ◽

2021 ◽

Author(s):

Anirudh Pradhan ◽

Vinod Kumar Bhardwaj ◽

Archana Dixit ◽

Syamala Krishnannair

Keyword(s):

Dark Energy ◽

Bianchi Type ◽

Holographic Dark Energy ◽

Cosmological Solution ◽

Type I ◽

Field Equations ◽

Eos Parameter ◽

Bianchi Type I ◽

New Class ◽

Energy Models

In this paper, we examine the LRS Bianchi-type-I cosmological model with holographic dark energy. The exact solutions to the corresponding field equations are obtained by using the generalized hybrid expansion law (HEL). The EoS parameter [Formula: see text] for DE is found to be time-dependent and redshift-dependent and its exiting range for derived model is agreeing well with the current observations. Here, we likewise apply two mathematical diagnostics, the statefinders ([Formula: see text]) and [Formula: see text] plan to segregate HDE model from the [Formula: see text]CDM model. Here, the [Formula: see text] diagnostic trajectories are good tools to classify the dynamical DE model. We found that our model lies in both thawing region and freezing region. We also construct the potential as well as dynamics of the quintessence and tachyon scalar field. Some physical and geometric properties of this model along with the physical acceptability of cosmological solution have been discussed in detail.

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