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Abstract <p>Models of strange stars in general relativity are considered in the case of a uniform density distribution. This approximation allows us to find the approximate mass of a star of a given density without resorting to the integration of differential equations. Uniform-density models of strange stars with the MIT bag model equation of state have a simple analytical solution. In the area of maximum mass, they differ from the exact solutions obtained by numerical integration of differential equations by no more than ~20%. The issues of the formation of strange stars are discussed depending on the deconfinement boundary (DB), where quarks become free. The available experimental results indicate a high density of matter in the DB region. This greatly limits the limiting mass of strange stars, and prevents their formation at the end of stellar evolution due to the fact that the limiting mass of neutron stars is several times greater, and corresponds to a much lower density of matter.</p>

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Strange Stars in a Uniform Density Approximation

  • 期刊论文

  • 发表日期：

    2026年1月1日

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  • G. S. Bisnovatyi-Kogan,
  • E. A. Patraman

摘要

Abstract

Models of strange stars in general relativity are considered in the case of a uniform density distribution. This approximation allows us to find the approximate mass of a star of a given density without resorting to the integration of differential equations. Uniform-density models of strange stars with the MIT bag model equation of state have a simple analytical solution. In the area of maximum mass, they differ from the exact solutions obtained by numerical integration of differential equations by no more than ~20%. The issues of the formation of strange stars are discussed depending on the deconfinement boundary (DB), where quarks become free. The available experimental results indicate a high density of matter in the DB region. This greatly limits the limiting mass of strange stars, and prevents their formation at the end of stellar evolution due to the fact that the limiting mass of neutron stars is several times greater, and corresponds to a much lower density of matter.