Modeling of compact stars: an anisotropic approach

We present here a new class of singularity free interior solutions relevant for the description of realistic anisotropic compact stellar objects with spherically symmetric matter distribution. In this geometric approach, specific choices of one of the metric functions and a selective anisotropic pro...

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Bibliographic Details
Published in:General relativity and gravitation Vol. 53; no. 3
Main Authors: Das, Shyam, Singh, Ksh. Newton, Baskey, Lipi, Rahaman, Farook, Aria, Anil K.
Format: Journal Article
Language:English
Published: New York Springer US 01.03.2021
Springer Nature B.V
Subjects:
Astronomy
Astrophysics and Cosmology
Binary stars
Classical and Quantum Gravitation
Density
Differential Geometry
Einstein equations
Gravitational waves
Gravity
Mathematical and Computational Physics
Moments of inertia
Physics
Physics and Astronomy
Pulsars
Quantum Physics
Relativity Theory
Research Article
Singularity (mathematics)
Stars
Stellar models
Tables (data)
Theoretical
Anisotropic
Stability
Einstein field equation
ISSN:0001-7701, 1572-9532
Online Access:Get full text
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Summary:We present here a new class of singularity free interior solutions relevant for the description of realistic anisotropic compact stellar objects with spherically symmetric matter distribution. In this geometric approach, specific choices of one of the metric functions and a selective anisotropic profile allow us to develop a stellar model by solving Einstein Field equations. The interior solutions thus obtained are matched with the Schwarzschild exterior metric over the bounding surface of a compact star. These matching conditions together with the condition that the radial pressure vanishes at the boundary are used to fix the model parameters. The different physical features for the developed model explicitly studied from the aspect of the pulsar 4U 1820 - 30 with its current estimated data (mass = 1.46 ± 0.21 M ⊙ and radius = 11.1 ± 1.8  km (Özel et al.: ApJ 820(1): 28, 2016) ). Analysis has shown that all the physical aspects are acceptable demanded for a physically admissible star and satisfy all the required physical conditions. The stability of the model is also explored in the context of causality conditions, adiabatic index, generalized Tolman–Oppenheimer–Volkov (TOV) equation, Buchdahl Condition and Herrera Cracking Method. To show that the developed model is compatible with a wide range of recently observed pulsars, various relevant physical variables are also highlighted in tabular form. The data studied here are in agreement with the observation of gravitational waves from the first binary merger event. Assuming a particular surface density ( 7.5 × 10 14 gm cm - 3 ), the mass-radius ( M - b ) relationship and the radius-central density relationship ( b - ρ ( 0 ) ) of the compact stellar object are analyzed for this model. Additionally, comparing the results with a slow rotating configuration, we have also discussed moment of inertia and the time period using Bejger-Haensel idea.
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ISSN:0001-7701
1572-9532
DOI:10.1007/s10714-021-02792-5