Year: 2024
Type: article
Abstract: This work revisits a modified version of the hydrostatic equilibrium equation in the presence of pressure anisotropy based on General Relativity with an extra dimension. We examine the structural features of quark stars in various dimensions by solving the Tolman–Oppenheimer–Volkoff (TOV) equation numerically using the interacting quark EoS. From our result, the compact star model with isotropic pressure can be obtained as $$\alpha $$ α approaches zero. The energy-dependent maximum mass and its associated radius, as well as the other characteristics like pressure, energy density, stability, etc., of the quark star, are obtained using the numerical solution. Through our detailed study, we have demonstrated that the conclusions we obtained here are consistent with observable evidence in four-dimensional spacetime. In four dimensions, for different values of $$\alpha $$ α , our obtained results can predict the mass of the compact stars PSR J0740+6620, PSR J1614-2230, Vela X-1, 4U 1608-52, 4U 1820-30, Cen X-3, and EXO 1785-248.
Source: The European Physical Journal C
Authors: Krishna Pada Das, Piyali Bhar, Ujjal Debnath
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: diamond
OpenAlex ID: W4402927234