Scholarlink

<p>The present paper is devoted to the variability of the star 19&#xa0;Cep. We analyze line profile variations in spectra of the star obtained with the 1.25‑m telescope of the Crimean station of the Sternberg Astronomical Institute and brightness variations of the star based on TESS data in 2019. Regular components of line profile variations in the Balmer lines and in the He&#xa0;II and C&#xa0;III lines with periods from 12&#xa0;to 108 min were detected. Those are associated with high modes of non-radial pulsations. Components with periods from 1.07 to 6.22 days were registered in the TESS brightness variations of the star. The TESS period <InlineEquation ID="IEq1"> <EquationSource Format="TEX">\(P=4.65\pm 0.43\)</EquationSource> </InlineEquation> days is interpreted as the rotation period of the star. The inclination of the rotation axis of the star <InlineEquation ID="IEq2"> <EquationSource Format="TEX">\(i=23^\circ\pm 2^\circ\)</EquationSource> </InlineEquation> is estimated. Stochastic variations in the brightness of a&#xa0;star, the Fourier amplitude of which can be described by a&#xa0;quasi-Lorentzian curve, are investigated.</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

Spectral and photometric variability of 19 Cep: optical data

  • 期刊论文

  • 发表日期：

    2026年7月9日

查看全文
  • A. F. Kholtygin,
  • N. P. Ikonnikova,
  • D. N. Mokshin,
  • G. M. Karataeva,
  • V. S. Bukharinov,
  • O. A. Tsiopa

摘要

The present paper is devoted to the variability of the star 19 Cep. We analyze line profile variations in spectra of the star obtained with the 1.25‑m telescope of the Crimean station of the Sternberg Astronomical Institute and brightness variations of the star based on TESS data in 2019. Regular components of line profile variations in the Balmer lines and in the He II and C III lines with periods from 12 to 108 min were detected. Those are associated with high modes of non-radial pulsations. Components with periods from 1.07 to 6.22 days were registered in the TESS brightness variations of the star. The TESS period \(P=4.65\pm 0.43\) days is interpreted as the rotation period of the star. The inclination of the rotation axis of the star \(i=23^\circ\pm 2^\circ\) is estimated. Stochastic variations in the brightness of a star, the Fourier amplitude of which can be described by a quasi-Lorentzian curve, are investigated.