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Abstract <p>The structure of the magnetic field of HD 37479 corresponds to the structure of a dipole displaced along the axis by a significant value <InlineEquation ID="IEq3"> <EquationSource Format="TEX">\(\Delta a=0.2R_{*}\)</EquationSource> <!--ASPBull2560023Glagolevskij-m3--> </InlineEquation> and across the axis by the value <InlineEquation ID="IEq4"> <EquationSource Format="TEX">\(\Delta a=0.05R_{*}\)</EquationSource> <!--ASPBull2560023Glagolevskij-m4--> </InlineEquation>. As a result, the magnetic field is distributed extremely unevenly over the stellar surface. The maximum values of the average surface magnetic field are equal to <InlineEquation ID="IEq5"> <EquationSource Format="TEX">\(B_{s}=+2591\)</EquationSource> <!--ASPBull2560023Glagolevskij-m5--> </InlineEquation> and <InlineEquation ID="IEq6"> <EquationSource Format="TEX">\(-7486\)</EquationSource> <!--ASPBull2560023Glagolevskij-m6--> </InlineEquation> G. It is in these areas that the maximum wind occurs, and also in approximately these same areas the maximum helium abundance is observed. A cloud of rarefied gas extends along the magnetic equator, in which H<InlineEquation ID="IEq7"> <EquationSource Format="TEX">\(\alpha\)</EquationSource> <!--ASPBull2560023Glagolevskij-m7--> </InlineEquation> emission lines are formed.</p>

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Special Features of the Magnetic Field Structure of the He-r Star HD 37479 \(\boldsymbol{\sigma}\)Ori E

  • 期刊论文

  • 发表日期：

    2025年6月1日

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  • Yu. Yu. Glagolevskij,
  • A. F. Nazarenko

摘要

Abstract

The structure of the magnetic field of HD 37479 corresponds to the structure of a dipole displaced along the axis by a significant value \(\Delta a=0.2R_{*}\) and across the axis by the value \(\Delta a=0.05R_{*}\) . As a result, the magnetic field is distributed extremely unevenly over the stellar surface. The maximum values of the average surface magnetic field are equal to \(B_{s}=+2591\) and \(-7486\) G. It is in these areas that the maximum wind occurs, and also in approximately these same areas the maximum helium abundance is observed. A cloud of rarefied gas extends along the magnetic equator, in which H \(\alpha\) emission lines are formed.