Strange quark mass (m s ) dependent model of anisotropic strange quark star*

Abstract

Abstract This article presents the configuration of strange quark stars in hydrostatic equilibrium considering the Vaidya-Tikekar metric ansatz. The interior of such stars comprises strange quark matter (henceforth SQM), whose equation of state ( ) is described by the MIT EoS , where B is the difference between perturbative and non-perturbative vacuum. We have included the mass of the strange quark into the EoS and studied its effect on the overall properties of the strange quark star in this work. It is observed that the maximum mass reaches its highest value when . We have evaluated the range of the maximum mass of the strange quark star by solving the TOV equation for necessary for stable strange quark matter at a zero external pressure condition with respect to neutrons. Maximum mass lies within the range of to when B ranges from to and . It is noted that the maximum mass decreases with an increase in . Our model is found suitable for describing the mass of pulsars such as PSR J1614-2230 and Vela X-1 and the secondary objects in the GW170817 event. The model is also useful in predicting the radius of the recently observed pulsars PSR J0030+0451, PSR J0740+6620, and PSR J0952-0607 and the secondary objects in the GW170817 and GW190814 events. Our model is found to be stable with respect to all stability criteria of the stellar configurations and is also stable with respect to small perturbations.