Dynamics of anisotropic dark energy universe embedded in one-directional magnetized fluid

2019 ◽  
Vol 28 (07) ◽  
pp. 1950093 ◽  
Author(s):  
Pratik P. Ray ◽  
B. Mishra ◽  
S. K. Tripathy
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
Power Law ◽  
Scale Factor ◽  
Mathematical Formalism ◽  
Physical Parameters ◽  
Volumetric Expansion ◽  
Anisotropic Dark Energy ◽  
Two Fluid

In this work, we have constructed an anisotropic dark energy cosmological model in a two-fluid situation, such as the usual dark energy and the magnetized fluid. We have assumed the dark energy pressure to be anisotropic in different spatial directions. In order to develop the mathematical formalism of the model, we have considered the scale factor as hybrid scale factor which is a combination of both power law and exponential volumetric expansion law. The physical parameters are derived and analyzed and found to be in agreement with the observational limits.

Holographic dark energy model with quintessence in general class of Bianchi cosmological models

2015 ◽  
Vol 93 (1) ◽  
pp. 68-79
Author(s):  
R. Chaubey ◽  
A.K. Shukla
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
General Class ◽  
Holographic Dark Energy ◽  
Scale Factor ◽  
Cosmological Models ◽  
Negative Slope ◽  
Physical Parameters ◽  
Field Equations ◽  
Dark Energy Component

In this paper, we study the general class of Bianchi cosmological models with holographic dark energy component. We have discussed three types of solutions of the average scale factor for the general class of Bianchi cosmological models by using a special law for the deceleration parameter, which is linear in time with a negative slope. The exact solutions to the corresponding field equations are also obtained. All the physical parameters are calculated and discussed in each physically viable cosmological model. For large time (i.e., t → ∞) the models tend asymptotically to an isotropic Friedmann–Robertson–Walker cosmological model. Quintessence scalar field and quintessence potential are also obtained for three different scenarios of scale factor.

Anisotropic Dark Energy Cosmological Model with Cosmic Strings

2020 ◽  
Author(s):  
T. Vinutha ◽  
V.U.M. Rao ◽  
Molla Mengesha
Keyword(s):  
Dark Energy ◽  
Equation Of State ◽  
Cosmological Model ◽  
State Parameter ◽  
Accelerated Expansion ◽  
Physical Parameters ◽  
Type I ◽  
Field Equations ◽  
Eos Parameter ◽  
Phantom Divide

The present study deals with a spatially homogeneous locally rotationally symmetric (LRS) Bianchi type-I dark energy cosmological model containing one dimensional cosmic string fluid source. The Einstein's field equations are solved by using a relation between the metric potentials and hybrid expansion law of average scale factor. We discuss accelerated expansion of our model through equation of state (ωde) and deceleration parameter (q). We observe that in the evolution of our model, the equation of state parameter starts from matter dominated phase ωde > -1/3 and ultimately attains a constant value in quintessence region (-1 < ωde < -1/3). The EoS parameter of the model never crosses the phantom divide line (ωde = 1). These facts are consistent with recent observations. We also discuss some other physical parameters.

scholarly journals GENERALIZED MODEL FOR Λ DARK ENERGY

2009 ◽  
Vol 18 (03) ◽  
pp. 389-396 ◽  
Author(s):  
UTPAL MUKHOPADHYAY ◽  
P. C. RAY ◽  
SAIBAL RAY ◽  
S. B. DUTTA CHOUDHURY
Keyword(s):  
Dark Energy ◽  
Equation Of State ◽  
Cosmological Model ◽  
A Priori ◽  
State Parameter ◽  
Spherically Symmetric ◽  
Einstein Field Equations ◽  
Field Equations ◽  
Equation Of State Parameter ◽  
Two Fluid

Einstein field equations under spherically symmetric space–times are considered here in connection with dark energy investigation. A set of solutions is obtained for a kinematic Λ model, viz. [Formula: see text], without assuming any a priori value for the curvature constant and the equation-of-state parameter ω. Some interesting results, such as the nature of cosmic density Ω and deceleration parameter q, have been obtained with the consideration of two-fluid structure instead of the usual unifluid cosmological model.

Holographic DBI-Essence Dark Energy via Power-Law Solution of the Scale Factor

2013 ◽  
Vol 52 (11) ◽  
pp. 3945-3952 ◽  
Author(s):  
Surajit Chattopadhyay ◽  
Antonio Pasqua
Keyword(s):  
Dark Energy ◽  
Power Law ◽  
Scale Factor

scholarly journals LRS Bianchi Type-I Cosmological Model with Anisotropic Dark Energy and Special Form of Deceleration Parameter

2013 ◽  
Vol 04 (08) ◽  
pp. 1037-1040 ◽  
Author(s):  
Kishor Shankarrao Adhav ◽  
Rajesh Purushottam Wankhade ◽  
Abhijit Shankarrao Bansod
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
Deceleration Parameter ◽  
Special Form ◽  
Bianchi Type ◽  
Type I ◽  
Bianchi Type I ◽  
Anisotropic Dark Energy

Tilted cosmological model consisting two forms of dark energy

2018 ◽  
Vol 33 (36) ◽  
pp. 1850213 ◽  
Author(s):  
V. J. Dagwal ◽  
D. D. Pawar
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
Power Law ◽  
Gravitational Constant ◽  
Deterministic Model ◽  
Geometrical Parameters ◽  
Tilted Cosmological Model ◽  
The Universe ◽  
Tilted Models

We have presented the tilted cosmological model consisting of two forms of dark energy. The behavior of different stages of the Universe in tilted models is studied with the help of dark energy contained in our Universe to be part of quintessence which is a homogeneous minimally coupled scalar. To get the deterministic model, we have assumed a power law of gravitational constant G. We also investigated the behavior of some physical and geometrical parameters.

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