scholarly journals Bianchi type-V modified f(R,T) gravity model in Lyra geometry with varying deceleration parameter

2021 ◽  
Keyword(s):  
Gravity Model ◽  
Deceleration Parameter ◽  
Bianchi Type ◽  
Lyra Geometry ◽  
Type V ◽  
Bianchi Type V

Bianchi type VI cosmological model with electromagnetic field in Lyra geometry

2016 ◽  
Vol 94 (10) ◽  
pp. 992-1000 ◽  
Author(s):  
M. Abdel-Megied ◽  
E.A. Hegazy
Keyword(s):  
Electromagnetic Field ◽  
Cosmological Model ◽  
Bianchi Type ◽  
Lyra Geometry ◽  
Geometrical Properties ◽  
Special Cases ◽  
Type V ◽  
Tensor Formula ◽  
Shear Tensor ◽  
Bianchi Type V

Bianchi type VI cosmological model in the presence of electromagnetic field with variable magnetic permeability in the framework of Lyra geometry is presented. An exact solution is introduced by considering that the eigenvalue [Formula: see text] of the shear tensor [Formula: see text] is proportional to the scalar expansion Θ of the model, that is, C = (AB)L, where A, B, and C are the coefficients of the metric and L is a constant. Bianchi type V, III, and I cosmological models are given as special cases of Bianchi type VI. Physical and geometrical properties of the models are discussed.

scholarly journals Homothetic Motion in a Bianchi Type –V Model in Lyra Geometry

2017 ◽  
Vol 1 (4) ◽  
Author(s):  
F. El-Sabbagh  - R. M. Gad, F. Abd.El-Bsseer, H. H. Moustafa
Keyword(s):  
Vector Field ◽  
Equation Of State ◽  
Bianchi Type ◽  
Displacement Vector ◽  
Lyra Geometry ◽  
Type I ◽  
Bianchi Type I ◽  
Homothetic Vector ◽  
Type V ◽  
Bianchi Type V

In this paper we study a homothetic vector field of a Bianchi type-V model based on Lyra geometry. The aim of this paper is to get the components of  homothetic vector field  in Lyra geometry for Bianchi type-V, compare between it and the case of  Bianchi type-I. Using ordinary method and Computer program to get the components of  the vector . The results are compatible in the two methods and get the condition that the results  tends to the case of  Bianchi type-I.  The cases when a displacement vector is a function of  t and when it is constant are considered. In both two cases we investigate the equation of state.

scholarly journals Bianchi Type-V Bulk Viscous Cosmic String inf(R,T)Gravity with Time Varying Deceleration Parameter

2015 ◽  
Vol 2015 ◽  
pp. 1-8 ◽  
Author(s):  
Bïnaya K. Bishi ◽  
K. L. Mahanta
Keyword(s):  
Deceleration Parameter ◽  
Bianchi Type ◽  
Cosmic Strings ◽  
The Other ◽  
Time Varying ◽  
Constant Deceleration Parameter ◽  
Linearly Varying Deceleration Parameter ◽  
Bulk Viscous ◽  
Type V ◽  
Bianchi Type V

We study the Bianchi type-V string cosmological model with bulk viscosity inf(R,T)theory of gravity by considering a special form and linearly varying deceleration parameter. This is an extension of the earlier work of Naidu et al., 2013, where they have constructed the model by considering a constant deceleration parameter. Here we find that the cosmic strings do not survive in both models. In addition we study some physical and kinematical properties of both models. We observe that in one of our models these properties are identical to the model obtained by Naidu et al., 2013, and in the other model the behavior of these parameters is different.

scholarly journals Bianchi type-V modified holographic Ricci dark energy models in Saez–Ballester theory of gravitation

2017 ◽  
Vol 95 (2) ◽  
pp. 145-150 ◽  
Author(s):  
D.R.K. Reddy
Keyword(s):  
Dark Energy ◽  
Deceleration Parameter ◽  
Bianchi Type ◽  
Ricci Dark Energy ◽  
Theor Phys ◽  
Linearly Varying Deceleration Parameter ◽  
Theory Of Gravitation ◽  
Bianchi Type V Universe ◽  
Type V ◽  
Bianchi Type V

We have investigated Bianchi type-V universe filled with matter and modified holographic Ricci dark energy in a scalar–tensor theory proposed by Saez–Ballester (Phys. Lett. A, 113, 467 (1986)). To get a determinate solution, we have used (i) hybrid expansion law (Akarsu et al. JCAP, 01, 022 (2014)), (ii) varying deceleration parameter (Mishra et al. Int. J. Theor. Phys. 52, 2546 (2013)), and (iii) linearly varying deceleration parameter (Akarsu and Dereli. Int. J. Theor. Phys. 51, 612 (2012)). The various physical and geometrical aspects of the models are also discussed.

SOME BIANCHI TYPE COSMOLOGICAL MODELS IN LYRA GEOMETRY

2008 ◽  
Vol 23 (30) ◽  
pp. 4925-4931 ◽  
Author(s):  
J. K. SINGH
Keyword(s):  
Bianchi Type ◽  
Lyra Geometry ◽  
Energy Conditions ◽  
Geometrical Parameters ◽  
Einstein Field Equations ◽  
Field Equations ◽  
Massive Scalar Field ◽  
Normal Gauge ◽  
Type V ◽  
Bianchi Type V

A class of nonstatic solutions for Einstein field equations has been investigated in the context of Bianchi type-V space–time in the theory based on Lyra's geometry in Gauss normal gauge and in the presence of an attractive massive scalar field. The results have been studied through various physical and geometrical parameters. The energy conditions of the model have also been verified.

Interacting holographic dark energy in Bianchi type-V and IX universes with variable deceleration parameter

2020 ◽  
Vol 17 (10) ◽  
pp. 2050160
Author(s):  
H. Eser ◽  
C. B. Kilinc
Keyword(s):  
Dark Energy ◽  
Equation Of State ◽  
Deceleration Parameter ◽  
Bianchi Type ◽  
Holographic Dark Energy ◽  
Cosmological Parameters ◽  
Field Equations ◽  
Variable Deceleration Parameter ◽  
Type V ◽  
Bianchi Type V

In this paper, we study spatially homogeneous and anisotropic Bianchi type-V and IX universes filled with interacting dark matter and holographic dark energy. We obtained the solution of the field equations by using the variable deceleration parameter in the form [Formula: see text]. The cosmological parameters of the models like deceleration and equation of state are obtained. We observe that the deceleration parameter tends to [Formula: see text] which shows an accelerated universe, and the equation of state tends to [Formula: see text] which belongs to [Formula: see text]CDM model. Moreover, we establish the correspondence between holographic dark energy model and quintessence scalar field.

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