Anisotropic strange star with Tolman–Kuchowicz metric under f(R, T) gravity

Abstract

In the current article, we study anisotropic spherically symmetric strange star under the background of f (R, T ) gravity using the metric potentials of Tolman-Kuchowicz type [1,2] as λ(r) = ln(1 + ar 2 + br 4 ) and ν(r) = Br 2 + 2 ln C which are free from singularity, satisfy stability criteria and also well behaved. We calculate the value of constants a, b, B and C using matching conditions and the observed values of the masses and radii of known samples. To describe the strange quark matter (SQM) distribution, here we have used the phenomenological MIT bag model equation of state (EOS) where the density profile (ρ) is related to the radial pressure (p r ) as p r (r) = 1 3 (ρ − 4B g ). Here quark pressure is responsible for generation of bag constant B g . Motivation behind this study lies in finding out a nonsingular physically acceptable solution having various properties of strange stars. The model shows consistency with various energy conditions, TOV equation, Herrera's cracking condition and also with Harrison-Zel ′ dovich-Novikov's static stability criteria. Numerical values of EOS parameter and the adiabatic index also enhance the acceptability of our model.

Relativistic compact stars in Tolman spacetime via an anisotropic approach

“…On the other hand, we now discuss about the use of this metric potential in the context of modified gravity. This metric potential was used earlier by Bhar et al [54] to model compact object in Einstein-Gauss-Bonnet gravity and Javed et al [66] used this metric potential to model anisotropic spheres in f (R, G) modified gravity, Biswas et al [67] obtained an anisotropic strange star with f (R, T ) gravity, Majid and Sharif [68] obtained quark stars in massive Brans-Dicke gravity, Naz and Shamir [69] found the stellar model in f (G) gravity, Farasat Shamir and Fayyaz [70] obtained the model of charged compact star in f (R) gravity, Rej et al [71] studied the charged compact star in the context of f (R, T ) gravity. Since one can obtain the results in the background of GR as a limiting case of the result in different modified theories of gravity, one can conclude that all the obtained results in modified gravity are also consistent in the background of GR.…”

Study on Anisotropic Strange Stars in f ( T , T ) Gravity

“…According to Biswas et al [61], the compactness of the anisotropic fluid model is given by the compactification factor (70) and the twice of the compactification factor [? ] is followed by…”

“…The anisotropic compact stars with a quintessence field and modified Chaplygin gas in the framework of f (T) gravity model has been studied by Saha and Debnath [53]. On the other hand, strange stars as well as gravastars in f (R, T ) gravity have been studied in [54][55][56][57][58][59][60][61], where T is the trace of the energy-momentum tensor.…”

Study on Anisotropic Strange Stars in <em>f</em>(T,<em>T</em>) Gravity

“…According to Biswas et al [58], the compactness of the anisotropic fluid model is given by the compactification factor (71) and the twice of the compactification factor [100] is followed by…”

“…The anisotropic compact stars with quintessence field and modified Chaplygin gas in the framework of f (T) gravity model has been studied by Saha and Debnath [50]. On the other hand, strange stars as well as gravastars in f (R, T ) gravity have been studied in [51][52][53][54][55][56][57][58], where T is the trace of the energy-momentum tensor.…”