scholarly journals Bianchi type-V cosmology with magnetized anisotropic dark energy

2017 ◽  
Vol 95 (3) ◽  
pp. 274-282
Author(s):  
M. Farasat Shamir ◽  
Asad Ali
Keyword(s):  
Magnetic Field ◽  
Dark Energy ◽  
Bianchi Type ◽  
Anisotropic Fluid ◽  
Physical Parameters ◽  
Anisotropic Universe ◽  
Field Equations ◽  
Constant Deceleration Parameter ◽  
Type V ◽  
Bianchi Type V

We study anisotropic universe in the presence of magnetized dark energy. Bianchi type-V cosmological model is considered for this purpose. The energy–momentum tensor consists of anisotropic fluid with uniform magnetic field of energy density ρB. Exact solutions to the field equations are obtained without using conventional assumptions like constant deceleration parameter. In particular, a general solution is obtained that further provides different classes of solutions. Only three cases have been discussed for the present analysis: linear, quadratic, and exponential. Graphical analyses of the solutions are done for all the three classes. The behavior of the model using some important physical parameters is discussed in the presence of magnetic field.

BIANCHI TYPE V COSMOLOGICAL MODELS WITH PERFECT FLUID AND HEAT CONDUCTION IN LYRA'S GEOMETRY

2008 ◽  
Vol 23 (31) ◽  
pp. 4991-5005 ◽  
Author(s):  
SHRI RAM ◽  
MOHD. ZEYAUDDIN ◽  
C. P. SINGH
Keyword(s):  
Perfect Fluid ◽  
Bianchi Type ◽  
Displacement Vector ◽  
Hubble’S Parameter ◽  
Field Equations ◽  
Constant Deceleration Parameter ◽  
Displacement Vector Field ◽  
Lyra’S Geometry ◽  
Type V ◽  
Bianchi Type V

The field equations within the framework of Lyra's geometry with a time-dependent displacement vector field for a Bianchi type-V space–time filled with a perfect fluid and heat flow are presented. Two different classes of physically viable solutions are obtained by using a special law of variation for the generalized mean Hubble's parameter which correspond to singular and nonsingular models with constant deceleration parameter. These models are found to be consistent with the observations on the present day universe. Some thermodynamical relations are studied. The physical and kinematical behaviors of the models are also discussed.

scholarly journals ACCELERATING DARK ENERGY MODELS IN BIANCHI TYPE-V SPACETIME

2011 ◽  
Vol 26 (30) ◽  
pp. 2261-2275 ◽  
Author(s):  
ANIRUDH PRADHAN ◽  
HASSAN AMIRHASHCHI
Keyword(s):  
Dark Energy ◽  
Bianchi Type ◽  
Late Time ◽  
Field Equations ◽  
Future Evolution ◽  
New Exact Solutions ◽  
Spatially Homogeneous ◽  
Type V ◽  
The Universe ◽  
Bianchi Type V

Some new exact solutions of Einstein's field equations in a spatially homogeneous and anisotropic Bianchi type-V spacetime with minimally interaction of perfect fluid and dark energy components have been obtained. To prevail the deterministic solution we choose the scale factor [Formula: see text], which yields a time-dependent deceleration parameter (DP), representing a model which generates a transition of the universe from the early decelerating phase to the recent accelerating phase. We find that for n ≥ 1, the quintessence model is reproducible with present and expected future evolution of the universe. The other models (for n < 1), we observe the phantom scenario. The quintessence as well as phantom models approach to isotropy at late time. For different values of n, we can generate a class of physically viable DE models. The cosmic jerk parameter in our descended model is also found to be in good concordance with the recent data of astrophysical observations under appropriate condition. The physical and geometric properties of spatially homogeneous and anisotropic cosmological models are discussed.

scholarly journals Viability of Bianchi type V universe in f(R,T) = f1(R) + f2(R)f3(T) gravity

2020 ◽  
Vol 17 (07) ◽  
pp. 2050111
Author(s):  
Lokesh Kumar Sharma ◽  
Benoy Kumar Singh ◽  
Anil Kumar Yadav
Keyword(s):  
Bianchi Type ◽  
Hubble Constant ◽  
Lagrangian Model ◽  
Energy Conditions ◽  
Physical Parameters ◽  
Field Equations ◽  
Eos Parameter ◽  
Bianchi Type V Universe ◽  
Type V ◽  
Bianchi Type V

In this paper, we examine the viability of Bianchi type V universe in [Formula: see text] theory of gravitation. To solve the field equations, we have considered the power law for scale factor and constructed a singular Lagrangian model which is based on the coupling between Ricci scalar [Formula: see text] and trace of energy–momentum tensor [Formula: see text]. We find the constraints on Hubble constant [Formula: see text] and free parameter [Formula: see text] with 46 observational Hubble dataset and obtain pretty satisfactory results. The physical features of the model and transitional behavior of equation of state (EOS) parameter are analyzed. We examine the nature of physical parameters and validity of energy conditions as well as stability condition. We also present the Om[Formula: see text] and statefinder diagnostic analysis for the derived model.

SOME COSMOLOGICAL MODELS IN SCALAR–TENSOR THEORIES

2010 ◽  
Vol 25 (27) ◽  
pp. 2363-2371 ◽  
Author(s):  
J. K. SINGH
Keyword(s):  
Magnetic Field ◽  
Bianchi Type ◽  
Cosmological Models ◽  
Energy Conditions ◽  
Einstein Field Equations ◽  
Field Equations ◽  
Static Solutions ◽  
Type V ◽  
The Magnetic Field ◽  
Bianchi Type V

A class of non-static solutions to the Einstein field equations has been investigated in the context of Bianchi type-V spacetime in a family of scalar–tensor theories in the presence as well as absence of the magnetic field. The physical and kinematical behaviors of the models have been discussed. The energy conditions of the models 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.

SOME BIANCHI TYPE-V COSMOLOGICAL MODELS IN BRANS–DICKE THEORY

2010 ◽  
Vol 25 (18n19) ◽  
pp. 3817-3824 ◽  
Author(s):  
J. K. SINGH
Keyword(s):  
Magnetic Field ◽  
Bianchi Type ◽  
Cosmological Models ◽  
Energy Conditions ◽  
Type V ◽  
The Magnetic Field ◽  
Bianchi Type V

The Bianchi type-V cosmological models have been investigated in the context of Brans–Dicke theory in the presence as well as absence of the magnetic field. The physical and kinematical behaviors of the models have been discussed. The energy conditions of the models have also been examined.

THE BIANCHI TYPE V MAGNETIZED STRING DUST COSMOLOGICAL MODEL IN GENERAL RELATIVITY

2007 ◽  
Vol 16 (11) ◽  
pp. 1769-1781 ◽  
Author(s):  
RAJ BALI ◽  
SHILPI JAIN
Keyword(s):  
Magnetic Field ◽  
Electrical Conductivity ◽  
General Relativity ◽  
Cosmological Model ◽  
Bianchi Type ◽  
Fluid Distribution ◽  
Type V ◽  
The Magnetic Field ◽  
Bianchi Type V ◽  
Nonvanishing Component

The Bianchi type V magnetized string dust cosmological model for perfect fluid distribution is investigated. We assume that the magnetic field is along the x direction, so F23 is the only nonvanishing component of Fij. We also find that F14 = 0 = F24 = F34 due to the assumption of infinite electrical conductivity. The behavior of the model in the presence and the absence of a magnetic field is also discussed.

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