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Abstract <p>The polar V379 Vir is a well-known magnetic cataclysmic variable with a brown dwarf donor. Despite numerous studies of this system across various spectral ranges, a detailed investigation of the orbital variability of its optical spectra has not been carried out. In this work, we present an analysis of spectroscopic observations of V379 Vir obtained with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences. The orbital variability of the H<InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(\alpha\)</EquationSource> <!--ASPBull2560069Suslikov-m1--> </InlineEquation> emission indicates that the line is most likely formed in the accretion stream near the Lagrangian point <InlineEquation ID="IEq2"> <EquationSource Format="TEX">\(L_{1}\)</EquationSource> <!--ASPBull2560069Suslikov-m2--> </InlineEquation>, rather than on the donor’s surface, as previously assumed. The analysis of the rotational variability of the Zeeman splitting of hydrogen lines reveals a complex magnetic field topology of the white dwarf, which differs from a simple dipole configuration.</p>

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Phase-Resolved Spectroscopy of the Polar V379 Vir with a Brown Dwarf

  • 期刊论文

  • 发表日期：

    2026年3月1日

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  • M. V. Suslikov,
  • A. I. Kolbin,
  • N. V. Borisov

摘要

Abstract

The polar V379 Vir is a well-known magnetic cataclysmic variable with a brown dwarf donor. Despite numerous studies of this system across various spectral ranges, a detailed investigation of the orbital variability of its optical spectra has not been carried out. In this work, we present an analysis of spectroscopic observations of V379 Vir obtained with the 6-m telescope of the Special Astrophysical Observatory of the Russian Academy of Sciences. The orbital variability of the H \(\alpha\) emission indicates that the line is most likely formed in the accretion stream near the Lagrangian point \(L_{1}\) , rather than on the donor’s surface, as previously assumed. The analysis of the rotational variability of the Zeeman splitting of hydrogen lines reveals a complex magnetic field topology of the white dwarf, which differs from a simple dipole configuration.