Stellar model with non-zero strange quark mass ( $$m_s\ne 0$$ m s ≠ 0 ) and Mak–Harko density profile admitting observational results

Abstract

Abstract This article describes the configuration of strange quark stars composed of three flavour quarks in hydrostatic equilibrium considering the energy density profile of Mak and Harko and non-zero strange quark mass ( $$m_s\ne {0}$$ m s ≠ 0 ). A suitable stellar model is proposed assuming equation of state of interior matter as modified MIT equation of state in bag model $$p=\frac{1}{3}(\rho -4B_g)$$ p = 1 3 ( ρ - 4 B g ) , where $$B_g$$ B g is known as bag constant, to predict the viability of strange stars. The interior of such compact stars is mainly composed of quarks and electrons to establish charge neutrality condition. We have checked the various stability windows depending on the energy per baryon for different values of bag constant $$B_g$$ B g and mass of strange quark $$m_s$$ m s . We have studied the effect of non-zero mass of the strange quark ( $$m_s$$ m s ) on the physical properties of the strange star in the context of the modified MIT bag equation of state. We note that the maximum stellar mass decreases with increasing $$m_s$$ m s . The model is suitable for predicting the radius, central density and other properties of compact stars having mass $$\le 2.01M_{\odot }$$ ≤ 2.01 M ⊙ , such as $$4U~1820-30$$ 4 U 1820 - 30 , $$PSR~J1614-2230$$ P S R J 1614 - 2230 etc, which are supposed to be strange stars. The radius of few recently observed compact stars are predicted in our model and they are found to be compatible with the value as predicted from observation. The model is found to be suitable in view of all the necessary criterion along with fulfilment of stability of the stellar configuration as well as stable in view of small radial perturbations.