Gravitationally Non-Degenerate Petrov Type–I Cosmological Model Filled with Viscous Fluid in Modified Brans-Dicke Cosmology

2014 ◽  
Vol 53 (9) ◽  
pp. 2902-2911
Author(s):  
Sarfaraz Alam ◽  
Priyanka Rai ◽  
L. N. Rai ◽  
Vivek K. Singh
Keyword(s):  
Cosmological Model ◽  
Viscous Fluid ◽  
Petrov Type ◽  
Type I

scholarly journals Bianchi type I cosmological model with a viscous fluid

1985 ◽  
Vol 26 (11) ◽  
pp. 3010-3015 ◽  
Author(s):  
A. Banerjee ◽  
S. B. Duttachoudhury ◽  
Abhik Kumar Sanyal
Keyword(s):  
Cosmological Model ◽  
Viscous Fluid ◽  
Bianchi Type ◽  
Type I ◽  
Bianchi Type I

scholarly journals Dust Fluid Cosmological Model

2013 ◽  
Vol 2013 ◽  
pp. 1-5
Author(s):  
Anita Bagora (Menaria) ◽  
Rakeshwar Purohit
Keyword(s):  
Cosmological Model ◽  
Viscous Fluid ◽  
Physical Properties ◽  
Bulk Viscosity ◽  
Bianchi Type ◽  
Type I ◽  
Bulk Viscous Fluid ◽  
Bulk Viscous ◽  
Dust Fluid ◽  
Hubble Parameters

Bianchi type I tilted bulk viscous fluid cosmological model filled with dust fluid is investigated. We assume that (constant), where is the coefficient of bulk viscosity and is the expansion in the model. It has been assumed that the expansion in the model is only in two directions; that is, one of the components of Hubble parameters is zero. The physical and geometrical aspects of the model in the presence and absence of bulk viscosity are also discussed. Also, we have discussed two special models and their physical properties. From this, we present a particular example based on dust fluid.

Tilted Bulk Disordered Distribution Cosmological Model

2012 ◽  
Vol 629 ◽  
pp. 635-640
Author(s):  
Anita Bagora ◽  
Rakeshwar Purohit
Keyword(s):  
Heat Conduction ◽  
Cosmological Model ◽  
Viscous Fluid ◽  
Bulk Viscosity ◽  
Linear Relation ◽  
Bianchi Type ◽  
Type I ◽  
Bulk Viscous Fluid ◽  
Tilted Cosmological Model ◽  
Bulk Viscous

Bianchi type I bulk viscous fluid tilted cosmological model filled with disordered radiation and heat conduction is investigated. We assume that (constant), where is the coefficient of bulk viscosity and  is the expansion in the model. Here, we assume a linear relation between shear and expansion i.e. =constant, which leads to A=BC, where A, B, C are metric potentials. The physical and geometrical aspects of the model in the presence and absence of bulk viscosity are also discussed.

scholarly journals Mixed fluid cosmological model in f(R, T) gravity

2020 ◽  
Vol 98 (11) ◽  
pp. 1015-1022 ◽  
Author(s):  
Parbati Sahoo ◽  
Barkha Taori ◽  
K.L. Mahanta
Keyword(s):  
Cosmological Model ◽  
Bianchi Type ◽  
Type I ◽  
Time Varying ◽  
Eos Parameter ◽  
Barotropic Fluid ◽  
Rotationally Symmetric ◽  
Expansion Of The Universe ◽  
The Universe ◽  
Mixed Fluid

We construct a locally rotationally symmetric (LRS) Bianchi type-I cosmological model in f(R, T) theory of gravity when the source of gravitation is a mixture of barotropic fluid and dark energy (DE) by employing a time-varying deceleration parameter. We observe through the behavior of the state finder parameters (r, s) that our model begins from the Einstein static era and goes to ΛCDM era. The equation of state (EOS) parameter (ωd) for DE varies from the phantom (ω < –1) phase to quintessence (ω > –1) phase, which is consistent with observational results. It is found that the discussed model can reproduce the current accelerating phase of the expansion of the universe.

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