Charged compact star in f(R, T) gravity in Tolman–Kuchowicz spacetime

Pramit Rej; Piyali Bhar; Megan Govender

doi:10.1140/epjc/s10052-021-09127-3

2023 Impact factor 4.2

Particles and Fields

Open Access

Eur. Phys. J. C (2021) 81: 316
https://doi.org/10.1140/epjc/s10052-021-09127-3

Regular Article – Theoretical Physics

Charged compact star in f(R, T) gravity in Tolman–Kuchowicz spacetime

Pramit Rej¹^a, Piyali Bhar² and Megan Govender³

¹ Department of Mathematics, Sarat Centenary College, Dhaniakhali, 712 302, Hooghly, West Bengal, India
² Department of Mathematics, Government General Degree College, Singur, 712 409, Hooghly, West Bengal, India
³ Department of Mathematics, Faculty of Applied Sciences, Durban University of Technology, Durban, South Africa

^a pramitrej@gmail.com

Received: 4 March 2021
Accepted: 6 April 2021
Published online: 13 April 2021

Abstract

In this current study, our main focus is on modeling the specific charged compact star SAX J 1808.4-3658 (M = 0.88 $M_{⊙}$ $M_{\odot }$ , R = 8.9 km) within the framework of $f (R, T)$ $f(R,\,T)$ modified gravity theory using the metric potentials proposed by Tolman–Kuchowicz (Tolman in Phys Rev 55:364, 1939; Kuchowicz in Acta Phys Pol 33:541, 1968) and the interior spacetime is matched to the exterior Reissner–Nordström line element at the surface of the star. Tolman–Kuchowicz metric potentials provide a singularity-free solution which satisfies the stability criteria. Here we have used the simplified phenomenological MIT bag model equation of state (EoS) to solve the Einstein–Maxwell field equations where the density profile ( $ρ$ $\rho$ ) is related to the radial pressure ( $p_{r}$ $p_{\mathrm{r}}$ ) as $p_{r} (r) = (ρ - 4 B_{g}) / 3$ $p_{\mathrm{r}}(r) = (\rho - 4B_{\mathrm{g}})/3$ . Furthermore, to derive the values of the unknown constants $a, b, B, C$ $a,\, b,\, B,\, C$ and the bag constant $B_{g}$ $B_{\mathrm{g}}$ , we match our interior spacetime to the exterior Reissner–Nordström line element at the surface of stellar system. In addition, to check the physical validity and stability of our suggested model we evaluate some important properties, such as effective energy density, effective pressures, radial and transverse sound velocities, relativistic adiabatic index, all energy conditions, compactness factor and surface redshift. It is depicted from our current study that all our derived results lie within the physically accepted regime which shows the viability of our present model in the context of $f (R, T)$ $f(R,\,T)$ modified gravity.

© The Author(s) 2021

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