Physical properties of class I compact star model for linear and Starobinsky−f(R,T) functions

2020 ◽  
Vol 30 ◽  
pp. 100620 ◽  
Author(s):  
Ksh. Newton Singh ◽  
S.K. Maurya ◽  
Abdelghani Errehymy ◽  
Farook Rahaman ◽  
Mohammed Daoud
Keyword(s):  
Physical Properties ◽  
Compact Star ◽  
Class I ◽  
Star Model

scholarly journals Compact star model in Einstein–Gauss–Bonnet gravity within the framework of Finch Skea space–time

2019 ◽  
Vol 97 (1) ◽  
pp. 30-36
Author(s):  
Iftikar Hossain Sardar
Keyword(s):  
Physical Properties ◽  
Compact Star ◽  
Space Time ◽  
Energy Conditions ◽  
Star Model ◽  
Schwarzschild Solution ◽  
Exterior Space ◽  
New Class ◽  
Physical Validity ◽  
Interior Solutions

In this article we provide a new class of interior solutions of a five-dimensional compact star in Einstein–Gauss–Bonnet (EGB) gravity within the framework of Finch–Skea space–time. The exterior space–time is described by the EGB Schwarzschild solution. To check physical validity of our model we investigate various physical properties like causality of solutions, energy conditions, mass radius relations, Tolman–Oppenheimer–Volkov (TOV) equations, etc.

Embedding class I spherically symmetric charged compact star model

2020 ◽  
Vol 365 (2) ◽  
Author(s):  
B. Dayanandan ◽  
Smitha T.T. ◽  
S. K. Maurya
Keyword(s):  
Compact Star ◽  
Class I ◽  
Spherically Symmetric ◽  
Star Model

scholarly journals A Generic Embedding Class-I Model via Karmarkar Condition in f ℛ , T Gravity

2021 ◽  
Vol 2021 ◽  
pp. 1-16
Author(s):  
M. Zubair ◽  
Saira Waheed ◽  
Hina Javaid
Keyword(s):  
Coupling Parameter ◽  
Compact Star ◽  
Momentum Tensor ◽  
Class I ◽  
Physical Parameters ◽  
Star Model ◽  
Anisotropic Matter ◽  
Symmetric Geometry ◽  
Suitable Form ◽  
Relationship Of

In the present work, we investigate the existence of compact star model in the background of f ℛ , T gravity theory, where ℛ represents the Ricci scalar and T refers to the energy-momentum tensor trace. Here, we use Karmarkar condition for the interior stellar setup so that a complete and precise model following the embedding class-I strategy can be obtained. For this purpose, we assume anisotropic matter contents along with static and spherically symmetric geometry of compact star. As Karmarkar embedding condition yields a relationship of metric potentials, therefore we assume a suitable form for one of the metric components as e ϕ = a r 2 + b n − 1 r n + 1 , where a and b represent constants and n is a free parameter, and evaluate the other. We approximate the values of physical parameters like a , A , and B by utilizing the known values of mass and radius for the compact star Vela X-1. The validity of the acquired model is then explored for different values of coupling parameter λ graphically. It is found that the resulting solution is physically interesting and well-behaved.

Self-gravitating anisotropic star using gravitational decoupling

2021 ◽  
Author(s):  
Baiju Dayanandan ◽  
T. T. Smitha ◽  
Sunil Maurya
Keyword(s):  
Compact Star ◽  
Radial Component ◽  
Energy Conditions ◽  
Regularity Conditions ◽  
Star Model ◽  
Anisotropic Solution ◽  
Seed System ◽  
The Stability ◽  
Metric Function ◽  
Anisotropic Star

Abstract This paper addresses a new gravitationally decoupled anisotropic solution for the compact star model via the minimal geometric deformation (MGD) approach. We consider a non-singular well-behaved gravitational potential corresponding to the radial component of the seed spacetime and embedding class I condition that determines the temporal metric function to solve the seed system completely. However, two different well-known mimic approaches such as pr = Θ1 1 and ρ = Θ0 0 have been employed to determine the deformation function which gives the solution of the second system corresponding to the extra source. In order to test the physical viability of the solution, we have checked several conditions such as regularity conditions, energy conditions, causality conditions, hydrostatic equilibrium, etc. Moreover, the stability of the solutions has been also discussed by the adiabatic index and its critical value. We find that the solutions set seems viable as far as observational data are concerned.

scholarly journals A new class of relativistic model of compact stars of embedding class I

2017 ◽  
Vol 26 (09) ◽  
pp. 1750090 ◽  
Author(s):  
Piyali Bhar ◽  
Ksh. Newton Singh ◽  
Tuhina Manna
Keyword(s):  
Compact Star ◽  
Mass Function ◽  
Static Stability ◽  
Compact Stars ◽  
Stable Region ◽  
Energy Conditions ◽  
Arbitrary Form ◽  
Star Model ◽  
Field Equations ◽  
Anisotropic Matter

In the present paper, we have constructed a new relativistic anisotropic compact star model having a spherically symmetric metric of embedding class one. Here we have assumed an arbitrary form of metric function [Formula: see text] and solved the Einstein’s relativistic field equations with the help of Karmarkar condition for an anisotropic matter distribution. The physical properties of our model such as pressure, density, mass function, surface red-shift, gravitational redshift are investigated and the stability of the stellar configuration is discussed in details. Our model is free from central singularities and satisfies all energy conditions. The model we present here satisfy the static stability criterion, i.e. [Formula: see text] for [Formula: see text][Formula: see text]g/cm3(stable region) and for [Formula: see text][Formula: see text]g/cm3, the region is unstable i.e. [Formula: see text].

scholarly journals Quintessences compact star with Durgapal potential

2020 ◽  
Vol 35 (17) ◽  
pp. 2050144 ◽  
Author(s):  
Gabino Estevez-Delgado ◽  
Joaquin Estevez-Delgado ◽  
Aurelio Tamez Murguía ◽  
Rafael Soto-Espitia ◽  
Arthur Cleary-Balderas
Keyword(s):  
Compact Star ◽  
Radial Pressure ◽  
State Equation ◽  
Central Density ◽  
Star Model ◽  
Tangential Pressure ◽  
State Equations ◽  
Ordinary Matter ◽  
Linear State ◽  
Anisotropic Pressures

A compact star model formed by quintessence and ordinary matter is presented, both sources have anisotropic pressures and are described by linear state equations, also the state equation of the tangential pressure for the ordinary matter incorporates the effect of the quintessence. It is shown that depending on the compactness of the star [Formula: see text] the constant of proportionality [Formula: see text] between the density of the ordinary matter and the radial pressure, [Formula: see text], has an interval of values which is consistent with the possibility that the matter is formed by a mixture of particles like quarks, neutrons and electrons and not only by one type of them. The geometry is described by the Durgapal metric for [Formula: see text] and each one of the pressures and densities is positive, finite and monotonic decreasing, as well as satisfying the condition of causality and of stability [Formula: see text], which makes our model physically acceptable. The maximum compactness that we have is [Formula: see text], so we can apply our solution considering the observational data of mass and radii [Formula: see text], [Formula: see text] km which generate a compactness [Formula: see text] associated to the star PSR J0348[Formula: see text]+[Formula: see text]0432. In this case, the interval of [Formula: see text] and its maximum central density [Formula: see text] and in the surface [Formula: see text] of the star are [Formula: see text] and [Formula: see text], respectively, meanwhile the central density of the quintessence [Formula: see text].

scholarly journals PHYSICAL PROPERTIES OF COMPACT STAR-FORMING GALAXIES ATz∼ 2–3

2015 ◽  
Vol 807 (2) ◽  
pp. 139 ◽  
Author(s):  
Guanwen Fang ◽  
Zhongyang Ma ◽  
Xu Kong ◽  
Lulu Fan
Keyword(s):  
Physical Properties ◽  
Compact Star ◽  
Star Forming
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