Role of finite value of strange quark mass (ms≠0) and baryon number density (n) on the structure of strange stars

This study investigates the influence of non-zero strange quark mass $\left(m_s\right)$ and baryon number density $\left(n\right)$ on the properties, and maximum mass of strange stars. An exact relativistic solution of Einstein field equations is obtained using Tolman-IV potential and modified MIT bag model equation of state, $p_r=\frac{1}{3}(\rho -4B^{\prime })$, where $B^{\prime }$ depends on bag constant $B$, $m_s$, and $n$. In line with CERN’s findings, the transition from hadronic matter to quark–gluon plasma at high densities requires a more dynamic EoS. Unlike the standard MIT bag model with fixed $B$, the present approach employs Woods–Saxon parametrisation for $B\left(n\right)$, improving the description of phase transitions. Solutions of TOV equations indicate that for $m_s=0$, the maximum mass reaches $2.01M_{\odot }$ with a radius of 10.96 Km at $n=0.66f{m}^{-3}$. Increasing $m_s$ reduces these values. Notably, a correlation exists between $n$ and $m_s$, where the hadron–quark transition occurs at higher densities with increasing $m_s$. Stability analysis suggests that a chosen $n(=0.578f{m}^{-3})$ with $B\left(n\right)=70MeV/f{m}^3$ satisfies causality, energy, and stability criteria, making the model physically viable.