On a family of interior solutions for relativistic fluid spheres with possible applications to highly collapsed stellar objects

1977 ◽  
Vol 18 (5) ◽  
pp. 868-869 ◽  
Author(s):  
Patrick G. Whitman
Keyword(s):  
Stellar Objects ◽  
Relativistic Fluid ◽  
Fluid Spheres ◽  
Interior Solutions

Relativistic fluid spheres applicable to neutron star models

1978 ◽  
Vol 224 ◽  
pp. 993 ◽  
Author(s):  
P. G. Whitman ◽  
R. W. Redding
Keyword(s):  
Neutron Star ◽  
Star Models ◽  
Relativistic Fluid ◽  
Fluid Spheres

General relativistic fluid spheres with variable polytropic index

1966 ◽  
Vol 6 (2) ◽  
pp. 139-147
Author(s):  
R. van der Borght
Keyword(s):  
General Relativity ◽  
Compressible Fluid ◽  
Fluid Sphere ◽  
Polytropic Index ◽  
Field Equations ◽  
Relativistic Fluid ◽  
General Relativistic ◽  
Temperature And Pressure ◽  
Fluid Spheres

AbstractIn this paper we derive solutions of the field equations of general relativity for a compressible fluid sphere which obeys density-temperature and pressure-temperature relations which allow for a variation of the polytropic index throughout the sphere.

Anisotropic fluid spheres satisfying the Karmarkar condition

2019 ◽  
Vol 34 (15) ◽  
pp. 1950113 ◽  
Author(s):  
Nayan Sarkar ◽  
Susmita Sarkar ◽  
Farook Rahaman ◽  
Ksh. Newton Singh ◽  
Hasrat Hussain Shah
Keyword(s):  
Compact Stars ◽  
Anisotropic Fluid ◽  
Stability Factor ◽  
Spherically Symmetric ◽  
Einstein Field Equations ◽  
Field Equations ◽  
Suitable Form ◽  
Fluid Spheres ◽  
Interior Solutions ◽  
Tov Equation

In this paper, we present new physically viable interior solutions of the Einstein field equations for static and spherically symmetric anisotropic compact stars satisfying the Karmarkar condition. For presenting the exact solutions, we provide a new suitable form of one of the metric potential functions. Obtained solutions satisfy all the physically acceptable properties of realistic fluid spheres and hence solutions are well-behaved and representing matter distributions are in equilibrium state and potentially stable by satisfying the TOV equation and the condition on stability factor, adiabatic indices. We analyze the solutions for two well-known compact stars Vela X-1 (Mass = 1.77 M[Formula: see text], R = 9.56 km) and Cen X-3 (Mass = 1.49 M[Formula: see text], R = 9.17 km).

Mathematical modeling of compact anisotropic relativistic fluid spheres in higher spacetime dimensions

2016 ◽  
Vol 41 (3) ◽  
pp. 1062-1067
Author(s):  
Banashree Sen ◽  
Theophanes Grammenos ◽  
Piyali Bhar ◽  
Farook Rahaman
Keyword(s):  
Mathematical Modeling ◽  
Relativistic Fluid ◽  
Fluid Spheres

Interior solutions for rotating fluid spheres

1985 ◽  
Vol 32 (8) ◽  
pp. 1857-1862 ◽  
Author(s):  
Patrick G. Whitman
Keyword(s):  
Rotating Fluid ◽  
Fluid Spheres ◽  
Interior Solutions

Slowly rotating fluid spheres in the Einstein–Yukawa theory

1983 ◽  
Vol 61 (9) ◽  
pp. 1324-1327
Author(s):  
K. D. Krori ◽  
A. R. Sheikh
Keyword(s):  
Analytic Solutions ◽  
The Other ◽  
Slow Rotation ◽  
Rotating Fluid ◽  
Physical Conditions ◽  
Fluid Spheres ◽  
Interior Solutions ◽  
Yukawa Theory

We introduce slow rotation to a solution given by Krori et al. which represents fluid spheres in the Einstein–Yukawa theory, and present two new analytic solutions which are nonsingular and satisfy physical conditions throughout the spheres. One of the interior solutions represents uniformly rotating spheres and the other represents differentially rotating spheres. We also match the interior and exterior solutions on the boundary.

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