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Chattopadhyay P., Bhattacharjee D.
   The impact of finite strange quark mass and baryon number density on the stability and maximum mass of strange stars / Chattopadhyay P., Bhattacharjee D. - Текст на англ. языке // Физические интерпретации теории относительности, Международная научная конференция 24-я, Москва, 7 - 10 июля 2025 г. = Physical Interpretations of Relativity Theory (PIRT–2025) : сборник тезисов / МГТУ им. Н. Э. Баумана. - М., 2025. - С. 86-86.

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This study examines the effects of a non-zero strange quark mass and baryon number density on the structural properties, stability, and maximum mass of strange stars. An exact relativistic solution to the Einstein field equations is derived using the Tolman-IV metric potential and a modified MIT bag model equation of state (EoS), where the modified bag parameter depends on the bag constant and the strange quark mass. Here, the bag constant represents the difference between perturbative and non-perturbative vacuum energy. According to CERN's findings, transition from hadronic matter to Quark-Gluon Plasma (QGP) can occur at high densities under favourable conditions. The standard MIT bag model, which assumes a constant bag parameter, cannot adequately describe this transition. Incorporating a finite strange quark mass and employing Wood-Saxon parametrization for the bag parameter, which depends on baryon number density, provides a more realistic EoS capable of addressing this phase transition. As the strange quark mass increases, the EoS becomes softer, influencing the solutions of the TOV equations. For a zero strange quark mass, the maximum mass is 2.01 solar masses having radius of 10.96 Km. For strange quark masses of 50 and 100, these values reduce to 1.99 and 1.96 solar masses and radii of 10.88 Km and 10.69 Km, respectively. Phase transition from hadronic to quark matter occurs at higher density values when the strange quark mass increases (0.482, 0.489 and 0.51 for strange quark masses 0, 50 and 100 respectively). Beyond these values, the energy per baryon drops below 930.4, indicating a complete transition to quark matter and the stability of the system increases. The proposed model satisfies causality, energy, and stability conditions, effectively describing strange star properties.