Scholarlink

<p>Models of neutron and strange stars are studied within the approximation of a&#xa0;uniform density distribution. A&#xa0;universal algebraic equation, valid for any equation of state, is used to estimate the stellar mass at a&#xa0;given density without resorting to the numerical integration of differential equations. Equations of state for neutron stars include both a&#xa0;degenerate neutron gas and more realistic models, such as those employed by Malone, Johnson and Bethe [<CitationRef CitationID="CR1">1</CitationRef>]. Homogeneous strange star models based on the quark bag model equation of state admit simple analytical solutions. The approximate solutions presented in this work differ from the exact results obtained by numerical integration of the structure equations by no more than <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(\sim 20\%\)</EquationSource> </InlineEquation>.</p><p>The formation of strange stars is examined as a&#xa0;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 disfavors their formation at the final stages of stellar evolution, since the limiting mass of neutron stars is substantially higher and corresponds to significantly lower matter densities.</p>

错误：搜索内容不能为空，请输入英文关键词
错误：关键词超出字数限制，请精简
高级检索

Uniform models of neutron and quark (strange) stars in general relativity

  • 期刊论文

  • 发表日期：

    2026年7月21日

查看全文
  • G. S. Bisnovatyi-Kogan,
  • E. A. Patraman

摘要

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. Equations of state for neutron stars include both a degenerate neutron gas and more realistic models, such as those employed by Malone, Johnson and Bethe [1]. Homogeneous strange star models based on the quark bag model equation of state admit simple analytical solutions. The approximate solutions presented in this work differ from the exact results obtained by numerical integration of the structure equations by no more than \(\sim 20\%\) .

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 disfavors their formation at the final stages of stellar evolution, since the limiting mass of neutron stars is substantially higher and corresponds to significantly lower matter densities.