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Abstract <p>The problem of describing neutron stars with masses greater than two solar masses is closely related to the emergence of hyperons at densities several times higher than normal nuclear (the so-called “hyperon puzzle”). In the Skyrme force approximation, the characteristics of matter of neutron stars before the appearance of hyperons are calculated. The dependence of the density, at which <InlineEquation ID="IEq1"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="11496_2025_9099_Article_IEq1.gif" Format="GIF" Height="14" Rendition="HTML" Resolution="72" Type="Linedraw" Width="13" /> </InlineMediaObject> <EquationSource Format="TEX">\(\Lambda \)</EquationSource> <!--PhysPart2470256Nasakin-m1--> </InlineEquation> and <InlineEquation ID="IEq2"> <InlineMediaObject> <ImageObject Color="BlackWhite" FileRef="11496_2025_9099_Article_IEq2.gif" Format="GIF" Height="14" Rendition="HTML" Resolution="72" Type="Linedraw" Width="12" /> </InlineMediaObject> <EquationSource Format="TEX">\(\Xi \)</EquationSource> <!--PhysPart2470256Nasakin-m2--> </InlineEquation> hyperons appear, on the characteristics of nucleon–nucleon and hyperon interactions is considered.</p>

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Conditions of Hyperon Appearance in Neutron Star Matter

  • 期刊论文

  • 发表日期：

    2025年6月27日

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  • A. I. Nasakin,
  • D. E. Lanskoy,
  • S. A. Mikheev,
  • T. Y. Tretyakova

摘要

Abstract

The problem of describing neutron stars with masses greater than two solar masses is closely related to the emergence of hyperons at densities several times higher than normal nuclear (the so-called “hyperon puzzle”). In the Skyrme force approximation, the characteristics of matter of neutron stars before the appearance of hyperons are calculated. The dependence of the density, at which \(\Lambda \) and \(\Xi \) hyperons appear, on the characteristics of nucleon–nucleon and hyperon interactions is considered.