Strange quark mass(ms)dependent model of anisotropic strange quark star

作     者：A.Hakim K.B.Goswami P.K.Chattopadhyay 

作者机构：Department of PhysicsCoochbehar Panchanan BarmaUniversityVivekananda StreetDistrict:Coochbehar736101West BengalIndia 

出 版 物：《中国物理C:英文版》 (Chinese Physics C)

年 卷 期：2023年第47卷第9期

页      面：145-161页

核心收录：

学科分类：07[理学] 070202[理学-粒子物理与原子核物理] 0702[理学-物理学] 

基　　金：A fellowship has been provided to A.Hakim by Government of West Bengal(G.O.No.52-Edn(B)/5B-15/2017 dated June 7,2017,read with 65-Edn(B)/5-15/2017 dated July 11,2017) to K.B.Goswami by Council of Scientific and Industrial Research,India(vide no.09/1219(0004)/2019-EMR-I) 

主　　题：Einstein field equation strange star strange quark mass MIT bag model 

摘      要：This article presents the configuration of strange quark stars in hydrostatic equilibrium considering the Vaidya-Tikekar metric *** interior of such stars comprises strange quark matter(henceforth SQM),whose equation of state(hencefor orth EoS)is described by the MIT EoS p=1/3(p-4B),where B is the difference between perturbative and non-perturbative *** 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 *** is observed that the maximum mass reaches its highest value *** have evaluated the range of the maximum mass of the strange quark star by solving the TOV equation for 57.55B91.54 MeV/fm^(3)necessary for stable strange quark matter at a zero external pressure condition with respect to *** mass lies within the range of to when B ranges from 57.55 to 91.54MeV/fm^(3)and ms=*** is noted that the maximum mass decreases with an increase *** 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 *** 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 *** 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.