Impact of non-zero strange quark mass (<i>m</i> _<i>s</i> ≠ 0) on the properties of strange stars in <i>f</i>(<i>R</i>, <i>T</i>) gravity admitting observational results

Abstract In this article we propose a new class of isotropic strange star using Buchdahl-I metric ansatz in the context of MIT bag model equation of state considering of non-zero strange quark mass ( m s ) in the framework of modified f ( R , T ) theory of gravity. The barotropic form of MIT bag model equation of state and a specific class of f ( R , T ) model, viz. , f ( R , T ) = R + 2 α c T where α c is termed as the gravity-matter coupling constant, produces a tractable set of solutions of Einstein field equations. From the obtained permissible range of numerical value of the coupling constant ( α c ), we have considered a range of α c from -2.0 to 2.0. Maximum mass and radius in this model is evaluated by numerically solving the TOV equations. Interestingly, the increment of m s and α c results in a softer equation of state which leads to the decrease in the maximum mass and radius while negative value of α c leads to a stiffer equation of state thereby increasing the maximum mass and radius in the present model. For physical application, we consider EXO 1745-248 and study the effects of m s and α c on its radius. Using the formalism, we have analysed the characteristic properties of EXO 1745-248. Apart from that, we have predicted the radii of a wide range of strange star candidates in the context of f ( R , T ) gravity and the obtained results agree well with the observed results. We note that the proposed model satisfies all the necessary energy conditions and stability criteria to emerge as a viable stellar configuration.