On the Quantum Birth of the Universe with a Bianchi Type-IX Metric in the Presence of an Anisotropic Fluid, a Scalar Field, and Pure Radiation

2021 ◽  
Author(s):  
E. V. Kuvshinova ◽  
O. V. Sandakova ◽  
D. M. Yanishevsky
Keyword(s):  
Scalar Field ◽  
Bianchi Type ◽  
Anisotropic Fluid ◽  
Pure Radiation ◽  
The Universe

Evolution of the Universe with two rotating fluids

2020 ◽  
Vol 35 (02n03) ◽  
pp. 2040042
Author(s):  
V. F. Panov ◽  
O. V. Sandakova ◽  
E. V. Kuvshinova ◽  
D. M. Yanishevsky
Keyword(s):  
General Relativity ◽  
Dark Energy ◽  
Scalar Field ◽  
Bianchi Type ◽  
Relativity Theory ◽  
Anisotropic Fluid ◽  
Rotating Fluids ◽  
General Relativity Theory ◽  
Exponential Expansion ◽  
The Universe

An anisotropic cosmological model with expansion and rotation and the Bianchi type IX metric has been constructed within the framework of general relativity theory. The first inflation stage of the Universe filled with a scalar field and an anisotropic fluid is considered. The model describes the Friedman stage of cosmological evolution with subsequent transition to accelerated exponential expansion observed in the present epoch. The model has two rotating fluids: the anisotropic fluid and dust-like fluid. In the approach realized in the model, the anisotropic fluid describes the rotating dark energy.

Evolution of anisotropic cosmic models in f(R,ϕ) gravity

2018 ◽  
Vol 27 (12) ◽  
pp. 1850115 ◽  
Author(s):  
M. Zubair ◽  
Farzana Kousar ◽  
Saira Waheed
Keyword(s):  
Scalar Field ◽  
Power Law ◽  
Bianchi Type ◽  
Scalar Potential ◽  
Anisotropic Fluid ◽  
Type I ◽  
Field Equations ◽  
Eos Parameter ◽  
Free Parameters ◽  
Physical Quantities

In this paper, we will discuss cosmological models using Bianchi type I for anisotropic fluid in [Formula: see text] theory of gravity which involves scalar potential. For this purpose, we consider power law assumptions of coupling function and scalar field along with the proportionality condition of expansion and shear scalars. We choose two [Formula: see text] models and obtain exact solutions of field equations in both cases. For these constructed models, the behavior of different physical quantities like EoS parameter, self-interacting potential as well as deceleration and skewness parameters are explored and illustrated graphically for the feasible ranges of free parameters. It is concluded that anisotropic fluid approaches isotropy in later cosmic times for both models.

scholarly journals EFFECTS OF ELECTROMAGNETIC FIELD ON THE DYNAMICS OF BIANCHI TYPE VI0UNIVERSE WITH ANISOTROPIC DARK ENERGY

2010 ◽  
Vol 19 (12) ◽  
pp. 1957-1972 ◽  
Author(s):  
M. SHARIF ◽  
M. ZUBAIR
Keyword(s):  
Electromagnetic Field ◽  
Dark Energy ◽  
Bianchi Type ◽  
Anisotropic Fluid ◽  
Einstein Field Equations ◽  
Anisotropic Behavior ◽  
Field Equations ◽  
Future Evolution ◽  
Anisotropic Dark Energy ◽  
The Universe

Spatially homogeneous and anisotropic Bianchi type VI0cosmological models with cosmological constant are investigated in the presence of anisotropic dark energy. We examine the effects of electromagnetic field on the dynamics of the universe and anisotropic behavior of dark energy. The law of variation of the mean Hubble parameter is used to find exact solutions of the Einstein field equations. We find that electromagnetic field promotes anisotropic behavior of dark energy which becomes isotropic for future evolution. It is concluded that the isotropic behavior of the universe model is seen even in the presence of electromagnetic field and anisotropic fluid.

scholarly journals QUANTIZATION OF THE BIANCHI TYPE IX MODEL IN N=1 SUPERGRAVITY IN THE PRESENCE OF SUPERMATTER

1996 ◽  
Vol 11 (10) ◽  
pp. 1763-1795 ◽  
Author(s):  
P.V. MONIZ
Keyword(s):  
Wave Function ◽  
Scalar Field ◽  
General Theory ◽  
Bianchi Type ◽  
Two Dimensional ◽  
Kahler Geometry ◽  
Complex Scalar ◽  
Analytical Potential ◽  
Complex Scalar Field ◽  
The Universe

The general theory of N=1 supergravity with supermatter is applied to a Bianchi type IX diagonal model. The supermatter is constituted by a complex scalar field and its [Formula: see text] fermionic partners. The Kähler geometry is chosen to be a two-dimensional flat one. The Lorentz-invariant ansatz for the wave function of the universe is taken to be as simple as possible in order to obtain new solutions. The set of differential equations derived from the quantum constraints are analyzed in two different cases: if the supermatter terms include an analytical potential or not. In the latter the wave function is found to have a simple form.

scholarly journals Anisotropic solution in phantom cosmology via Noether symmetry approach

2018 ◽  
Vol 96 (7) ◽  
pp. 677-680 ◽  
Author(s):  
I. Basaran Oz ◽  
Y. Kucukakca ◽  
N. Unal
Keyword(s):  
Scalar Field ◽  
Bianchi Type ◽  
Space Time ◽  
Noether Symmetry ◽  
Type I ◽  
Field Equations ◽  
Anisotropic Solution ◽  
Bianchi Type I ◽  
Symmetry Approach ◽  
The Universe

In this study, we consider a phantom cosmology in which a scalar field is minimally coupled to gravity. For anisotropic locally rotational symmetric (LRS) Bianchi type I space–time, we use the Noether symmetry approach to determine the potential of such a theory. It is shown that the potential must be in the trigonometric form as a function of the scalar field. We solved the field equations of the theory using the result obtained from the Noether symmetry. Our solution shows that the universe has an accelerating expanding phase.

Power law inflation with anisotropic fluid in Lyra’s manifold

2017 ◽  
Vol 95 (8) ◽  
pp. 748-752 ◽  
Author(s):  
S. Surendra Singh ◽  
Y. Bembem Devi ◽  
M. Saratchandra Singh
Keyword(s):  
Power Law ◽  
Bianchi Type ◽  
Anisotropic Fluid ◽  
Type I ◽  
Field Equations ◽  
Volumetric Expansion ◽  
Lyra’S Manifold ◽  
Rotationally Symmetric ◽  
Age Of The Universe ◽  
The Universe

Field equations of the locally rotationally symmetric (LRS) Bianchi type-I metric with anisotropic fluid are constructed within the framework of Lyra’s manifold. Power-law volumetric expansion is used to obtain exact solutions of the models for constant and time-dependent displacement field. We discuss the asymptotic behaviors of the derived models, anisotropic behavior of the fluid, expansion parameter, and the evolution of the model with the age of the universe.

Bianchi type-III holographic dark energy model with quintessence

2018 ◽  
Vol 15 (09) ◽  
pp. 1850161 ◽  
Author(s):  
M. Vijaya Santhi ◽  
V. U. M. Rao ◽  
Daba Meshesha Gusu ◽  
Y. Aditya
Keyword(s):  
Dark Energy ◽  
Scalar Field ◽  
Equation Of State ◽  
Dark Energy Model ◽  
Bianchi Type ◽  
Holographic Dark Energy ◽  
Scale Factor ◽  
Holographic Dark Energy Model ◽  
The Universe ◽  
Average Scale Factor

In this study, we investigate an anisotropic Bianchi type-[Formula: see text] space-time in the presence of matter and holographic dark energy components within the framework of general relativity. We obtained the solution of the field equations by assuming (i) the expansion scalar [Formula: see text] in the model is proportional to shear scalar [Formula: see text], (ii) hybrid expansion law for average scale factor (keeping an eye on the recent scenario of accelerating nature of the universe). We develop cosmological parameters like deceleration and equation of state parameters. These parameters are plotted versus redshift [Formula: see text] for different values of power component of average scale factor [Formula: see text]. We observe that the equation of state varies in quintessence region ([Formula: see text]) and ultimately tends to [Formula: see text]CDM model ([Formula: see text]). The deceleration parameter exhibits a smooth transition from early decelerated epoch to present accelerated era. In addition, we establish the correspondence between our holographic dark energy model and quintessence scalar field. We also express the self-interacting potential [Formula: see text] and scalar field [Formula: see text] of quintessence model as functions of cosmic time [Formula: see text], which describes the accelerated expansion of the universe.

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