X-ray/Hα scaling relationships in stellar flares

DOI PDF 被引用文献4件 参考文献36件
  • Hiroki Kawai
    Department of Physics, Chuo University , 1-13-27 Kasuga, Bunkyo-ku, Tokyo 112-8551 , Japan
  • Yohko Tsuboi
    Department of Physics, Chuo University , 1-13-27 Kasuga, Bunkyo-ku, Tokyo 112-8551 , Japan
  • Wataru B Iwakiri
    Department of Physics, Chuo University , 1-13-27 Kasuga, Bunkyo-ku, Tokyo 112-8551 , Japan
  • Yoshitomo Maeda
    Institute of Space and Astronautical Science, Japan Aerospace Exploration Agency , 3-1-1 Yoshinodai, Chuo-ku, Sagamihara, Kanagawa 252-5258 , Japan
  • Satoru Katsuda
    Graduate School of Science and Engineering, Saitama University , 255 Shimo-Okubo, Sakura-ku, Saitama, Saitama 338-8570 , Japan
  • Ryo Sasaki
    Department of Physics, Chuo University , 1-13-27 Kasuga, Bunkyo-ku, Tokyo 112-8551 , Japan
  • Junya Kohara
    Department of Physics, Chuo University , 1-13-27 Kasuga, Bunkyo-ku, Tokyo 112-8551 , Japan

書誌事項

公開日
2022-03-21
資源種別
journal article
権利情報
  • https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model
DOI
  • 10.1093/pasj/psac008
公開者
Oxford University Press (OUP)

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説明

<jats:title>Abstract</jats:title> <jats:p>We report on the results of our simultaneous observations of three large stellar flares with soft X-rays (SXRs) and an Hα emission line from two binary systems of RS CVn type. The energies released in the X-ray and Hα emissions during the flares were 1036–1038 and 1035–1037 erg, respectively. This renders the set of the observations as the first successful simultaneous X-ray/Hα observations of the stellar flares with energies above 1035 erg; although the coverage of the Hα observations was limited, with $\sim\! 10\%$ of the e-folding time in the decay phase of the flares, that of the SXR ones was complete. Combining the obtained physical parameters and those in literature for solar and stellar flares, we obtained a good proportional relation between the emitted energies of X-ray and Hα emissions for a flare energy range of 1029–1038 erg. The ratio of the Hα-line to bolometric X-ray emissions was ∼0.1, where the latter was estimated by converting the observed SXR emission to that in the 0.1–100 keV band according to the best-fitting thin thermal model. We also found that the e-folding times of the SXR and Hα light curves in the decaying phase of a flare are in agreement for a time range of 1–104 s. Even very large stellar flares with energies of six orders of magnitude larger than the most energetic solar flares follow the same scaling relationships with solar and much less energetic stellar flares. This fact suggests that their physical parameters can be estimated on the basis of the known physics of solar and stellar flares.</jats:p>

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