scholarly journals Bianchi type-I string cosmological model in the presence of a magnetic flux: exact and qualitative solutions

Open Physics ◽  
2010 ◽  
Vol 8 (1) ◽  
Author(s):  
Bijan Saha ◽  
Victor Rikhvitsky ◽  
Mihai Visinescu
Keyword(s):  
Magnetic Flux ◽  
Cosmological Model ◽  
Qualitative Analysis ◽  
Analytical Solutions ◽  
Present Model ◽  
Bianchi Type ◽  
Einstein Equations ◽  
Type I ◽  
Bianchi Type I ◽  
The Universe

AbstractA Bianchi type-I cosmological model in the presence of a magnetic flux along a cosmological string is investigated. The objective of this study is to generate solutions to the Einstein equations using a few tractable assumptions usually accepted in the literature. The analytical solutions are supplemented with numerical and qualitative analysis. In the frame of the present model the evolution of the Universe and other physical aspects are discussed.

A String Cosmological Model of Bianchi Type-I in the Presence of a Magnetic Flux

2009 ◽  
Author(s):  
Mihai Visinescu ◽  
Bijan Saha ◽  
Victor Rikhvitsky ◽  
Madalin Bunoiu ◽  
Iosif Malaescu
Keyword(s):  
Magnetic Flux ◽  
Cosmological Model ◽  
Bianchi Type ◽  
Type I ◽  
Bianchi Type I ◽  
String Cosmological Model

scholarly journals LOCALLY ROTATIONALLY SYMMETRIC BIANCHI TYPE-I COSMOLOGICAL MODEL IN f(T) GRAVITY: FROM EARLY TO DARK ENERGY DOMINATED UNIVERSE

2014 ◽  
Vol 23 (01) ◽  
pp. 1450004 ◽  
Author(s):  
M. E. RODRIGUES ◽  
I. G. SALAKO ◽  
M. J. S. HOUNDJO ◽  
J. TOSSA
Keyword(s):  
Dark Energy ◽  
Cosmological Model ◽  
Dark Energy Model ◽  
Bianchi Type ◽  
Rotational Symmetry ◽  
Type I ◽  
Bianchi Type I ◽  
Reconstruction Scheme ◽  
Rotationally Symmetric ◽  
The Universe

We study the locally rotational symmetry Bianchi type-I dark energy model in the framework of f(T) theory of gravity, where T denotes the torsion scalar. A viable cosmological model is undertaken and the isotropization of this latter is checked, yielding a result that reflects the real evolution of our universe. Moreover, still in the anisotropic optic, a more complicated f(T) model is obtained from the cosmological reconstruction scheme and the analysis shows that the universe is more anisotropic at the beginning if the terms of higher order in T are not considered. This means that the nonlinear model should be favored by observational data.

NON-COMMUTATIVE BIANCHI QUANTUM COSMOLOGY

2007 ◽  
Vol 16 (10) ◽  
pp. 1625-1632 ◽  
Author(s):  
W. GUZMÁN ◽  
C. ORTIZ ◽  
M. SABIDO ◽  
J. SOCORRO ◽  
MAXIMO A. AGÜERO
Keyword(s):  
Cosmological Model ◽  
Probability Density ◽  
Quantum Cosmology ◽  
Bianchi Type ◽  
Cosmological Term ◽  
Type I ◽  
Bianchi Type I ◽  
The Universe ◽  
Arbitrary Factor

Introducing non-commutative variables in the minisuperspace, we obtain the non-commutative quantum solutions to the Wheeler–DeWitt equation with an arbitrary factor ordering, for the anisotropic Bianchi type I cosmological model, coupled to barotropic matter and cosmological term Λ. From the probability density, the inclusion of non-commutativity seems to retard the isotropization of the universe.

scholarly journals Classical Bianchi Type I Cosmology in K-Essence Theory

2014 ◽  
Vol 2014 ◽  
pp. 1-11 ◽  
Author(s):  
J. Socorro ◽  
Luis O. Pimentel ◽  
Abraham Espinoza-García
Keyword(s):  
Cosmological Model ◽  
Cosmological Constant ◽  
Exact Solutions ◽  
Bianchi Type ◽  
Friedmann Equation ◽  
Matter Content ◽  
Type I ◽  
Bianchi Type I ◽  
Bianchi I ◽  
The Universe

We use one of the simplest forms of the K-essence theory and we apply it to the classical anisotropic Bianchi type I cosmological model, with a barotropic perfect fluid (p=γρ) modeling the usual matter content and with cosmological constantΛ. Classical exact solutions for anyγ≠1andΛ=0are found in closed form, whereas solutions forΛ≠0are found for particular values in the barotropic parameter. We present the possible isotropization of the cosmological model Bianchi I using the ratio between the anisotropic parameters and the volume of the universe. We also include a qualitative analysis of the analog of the Friedmann equation.

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.

scholarly journals Interaction of Bianchi type-I anisotropic cloud string cosmological model universe with electromagnetic field

2020 ◽  
Vol 17 (09) ◽  
pp. 2050133
Author(s):  
Kangujam Priyokumar Singh ◽  
Mahbubur Rahman Mollah ◽  
Rajshekhar Roy Baruah ◽  
Meher Daimary
Keyword(s):  
Electromagnetic Field ◽  
Cosmological Model ◽  
Bianchi Type ◽  
Physical Parameters ◽  
Type I ◽  
Field Equations ◽  
Rest Energy ◽  
Model Universe ◽  
Bianchi Type I ◽  
String Cosmological Model

Here, we have investigated the interaction of Bianchi type-I anisotropic cloud string cosmological model universe with electromagnetic field in the context of general relativity. In this paper, the energy-momentum tensor is assumed to be the sum of the rest energy density and string tension density with an electromagnetic field. To obtain exact solution of Einstein’s field equations, we take the average scale factor as an integrating function of time. Also, the dynamics and significance of various physical parameters of model are discussed.

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