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Description
Models of neutron and strange stars are studied within the approximation of a uniform density distribution. A universal algebraic equation, valid for any equation of state, is used to estimate the stellar mass at a given density without resorting to the numerical integration of differential equations. Different equations of state for neutron stars had been used.
Homogeneous strange star models based on the quark bag model equation of state admit simple analytical solutions. The formation of strange stars is examined as a function of the deconfinement boundary (DB), at which quarks become deconfined. Existing experimental data indicate that matter reaches extremely high densities in the vicinity of the DB. This places strong constraints on the maximum mass of strange stars and their existence, when limiting mass of neutron stars is substantially higher and corresponds to significantly lower matter densities.