We study the stability properties of magnetized strange quark matter and strangelets under a strong magnetic field in the MIT bag model. The free energy per baryon of strange quark matter feels a great influence from ...We study the stability properties of magnetized strange quark matter and strangelets under a strong magnetic field in the MIT bag model. The free energy per baryon of strange quark matter feels a great influence from the magnetic field. At the field strength about 1017 G, the magnetized strange quark matter becomes more stable.Considering the finite size effect, the magnetic influence on strangelets becomes complicated. For a given magnetic field, there exists a critical baryon number, below which the magnetized strangelets have lower energy than the nonmagnetized strangelets. For the field strength of 5 × 1017 G, the critical baryon number is Ac～ 100. Generally, the critical baryon number increases with the decreasing external magnetic field. When the field strength is smaller than1017 G, the critical baryon number goes up to Ac～ 105. The stable radius, electric charge, and quark flavor fractions of magnetized strangelets are shown.展开更多
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 eq...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(hencefor orth EoS)is described by the MIT EoS p=1/3(p-4B),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 57.55<B<91.54 MeV/fm^(3)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 57.55 to 91.54MeV/fm^(3)and ms=0.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.展开更多
We investigated the impact of f(R,L_(m),T)gravity on the internal structure of compact stars,expecting this theory to manifest prominently in the high-density cores of such stars.We considered the algebraic function,f...We investigated the impact of f(R,L_(m),T)gravity on the internal structure of compact stars,expecting this theory to manifest prominently in the high-density cores of such stars.We considered the algebraic function,f(R,L_(m),T)=R+αTL_(m),whereαrepresents the matter-geometry coupling constant.We specifically chose the matter Lagrangian density L_(m)=-ρto explore compact stars with anisotropic pressure.To this end,we employed the MIT bag model as an equation of state.Subsequently,we numerically solved the hydrostatic equilibrium equations to obtain mass-radius relations for quark stars(QSs),examining static stability criteria,adiabatic index,and speed of sound.Finally,we used recent astrophysical data to constrain the coupling parameterα,which may lead to either larger or smaller masses for QSs,compared to their counterparts in general relativity.展开更多
基金Supported by the National Natural Science Foundation of China under Grant Nos.11475110 and 11005071the Shanxi Provincial Natural Science Foundation under Grant No.2011011001-1
文摘We study the stability properties of magnetized strange quark matter and strangelets under a strong magnetic field in the MIT bag model. The free energy per baryon of strange quark matter feels a great influence from the magnetic field. At the field strength about 1017 G, the magnetized strange quark matter becomes more stable.Considering the finite size effect, the magnetic influence on strangelets becomes complicated. For a given magnetic field, there exists a critical baryon number, below which the magnetized strangelets have lower energy than the nonmagnetized strangelets. For the field strength of 5 × 1017 G, the critical baryon number is Ac～ 100. Generally, the critical baryon number increases with the decreasing external magnetic field. When the field strength is smaller than1017 G, the critical baryon number goes up to Ac～ 105. The stable radius, electric charge, and quark flavor fractions of magnetized strangelets are shown.
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)。
文摘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(hencefor orth EoS)is described by the MIT EoS p=1/3(p-4B),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 57.55<B<91.54 MeV/fm^(3)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 57.55 to 91.54MeV/fm^(3)and ms=0.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.
基金Supported by Walailak University under the New Researcher Development scheme(WU67268)A.Pradhan expresses gratitude to the IUCCA in Pune,India,for offering facilities under associateship programs.In addition,İzzet Sakallıthanks TÜBİTAK,ANKOS,and SCOAP3 for their contributions.Takol Tangphati andİzzet Sakallıalso appreciate COST Actions CA21106 and CA22113 for their networking support。
文摘We investigated the impact of f(R,L_(m),T)gravity on the internal structure of compact stars,expecting this theory to manifest prominently in the high-density cores of such stars.We considered the algebraic function,f(R,L_(m),T)=R+αTL_(m),whereαrepresents the matter-geometry coupling constant.We specifically chose the matter Lagrangian density L_(m)=-ρto explore compact stars with anisotropic pressure.To this end,we employed the MIT bag model as an equation of state.Subsequently,we numerically solved the hydrostatic equilibrium equations to obtain mass-radius relations for quark stars(QSs),examining static stability criteria,adiabatic index,and speed of sound.Finally,we used recent astrophysical data to constrain the coupling parameterα,which may lead to either larger or smaller masses for QSs,compared to their counterparts in general relativity.
