Time-resolved spectroscopy and photometry of M dwarf flare star YZ Canis Minoris with OISTER and TESS: Blue asymmetry in the Hα line during the non-white light flare. (2nd November 2020)

• Record Type: Journal Article
• Authors: Maehara, Hiroyuki; Notsu, Yuta; Namekata, Kousuke; Honda, Satoshi; Kowalski, Adam F; Katoh, Noriyuki; Ohshima, Tomohito; Iida, Kota; Oeda, Motoki; Murata, Katsuhiro L; Yamanaka, Masayuki; Takagi, Kengo; Sasada, Mahito; Akitaya, Hiroshi; Ikuta, Kai; Okamoto, Soshi; Nogami, Daisaku; Shibata, Kazunari
• Is Part Of: Publications of the Astronomical Society of Japan. Volume 73:Number 1(2021)
• Page Start: 44
• Page End: 65
• Publication Date: 2020-11-02
• Subjects: stars: activity -- stars: flare -- stars: rotation; Astronomy -- Periodicals; 520.5
• DOI: 10.1093/pasj/psaa098
• Languages: English
• ISSNs: 0004-6264

Abstract

Abstract: In this paper, we present the results from spectroscopic and photometric observations of the M-type flare star YZ CMi in the framework of the Optical and Infrared Synergetic Telescopes for Education and Research (OISTER) collaborations during the Transiting Exoplanet Survey Satellite (TESS) observation period. We detected 145 white-light flares from the TESS light-curve and four Hα flares from the OISTER observations performed between 2019 January 16 and 18. Among them, three Hα flares were associated with white-light flares. However, one of them did not show clear brightening in the continuum; during this flare, the Hα line exhibited blue asymmetry which lasted for ∼60 min. The line-of-sight velocity of the blueshifted component is in the range from −80 to −100 km s −1 . This suggests that there can be upward flows of chromospheric cool plasma even without detectable red/near-infrared (NIR) continuum brightening. By assuming that the blue asymmetry in the Hα line was caused by a prominence eruption on YZ CMi, we estimated the mass and kinetic energy of the upward-moving material to be 10 16 –10 18 g and 10 29.5 –10 31.5 erg, respectively. The estimated mass is comparable to expectations from the empirical relation between the flare X-ray energy and mass of upward-moving material for stellar flares and solar coronal mass ejections (CMEs). In contrast, the estimated kinetic energy for the non-white-light flare on YZ CMi is roughly two orders of magnitude smaller than that expected from the relation between flare X-ray energy and kinetic energy for solar CMEs. This could be understood by the difference in the velocity between CMEs and prominence eruptions.