Optical and X-ray observations of stellar flares on an active M dwarf AD Leonis with the Seimei Telescope, SCAT, NICER, and OISTER. (9th July 2020)

• Record Type: Journal Article
• Authors: Namekata, Kosuke; Maehara, Hiroyuki; Sasaki, Ryo; Kawai, Hiroki; Notsu, Yuta; Kowalski, Adam F; Allred, Joel C; Iwakiri, Wataru; Tsuboi, Yohko; Murata, Katsuhiro L; Niwano, Masafumi; Shiraishi, Kazuki; Adachi, Ryo; Iida, Kota; Oeda, Motoki; Honda, Satoshi; Tozuka, Miyako; Katoh, Noriyuki; Onozato, Hiroki; Okamoto, Soshi; Isogai, Keisuke; Kimura, Mariko; Kojiguchi, Naoto; Wakamatsu, Yasuyuki; Tampo, Yusuke; Nogami, Daisaku; Shibata, Kazunari
• Is Part Of: Publications of the Astronomical Society of Japan. Volume 72:Number 4(2020:Aug.)
• Publication Date: 2020-07-09
• Subjects: stars: activity -- stars: coronae -- stars: flare -- stars: magnetic fields -- starspots; Astronomy -- Periodicals; 520.5
• DOI: 10.1093/pasj/psaa051
• Languages: English
• ISSNs: 0004-6264

Abstract

Abstract: We report on multi-wavelength monitoring observations of an M-dwarf flare star AD Leonis with the Seimei Telescope (6150–7930 Å), SCAT (Spectroscopic Chuo-university Astronomical Telescope; 3700–7500 Å), and NICER (Neutron Star Interior Composition Explorer; 0.2–12.0 keV), with the collaboration of the OISTER (Optical and Infrared Synergetic Telescopes for Education and Research) program. Twelve flares are detected in total, including ten Hα, four X-ray, and four optical-continuum flares; one of them is a superflare with a total energy of ∼2.0 × 10 33 erg. We found that: (1) during the superflare, the Hα emission line full width at 1/8 maximum dramatically increases to 14 Å from 8 Å in the low-resolution spectra ( R ∼ 2000) accompanied by large white-light flares, (2) some weak Hα/X-ray flares are not accompanied by white-light emissions, and (3) the non-flaring emissions show clear rotational modulations in X-ray and Hα intensity in the same phase. To understand these observational features, one-dimensional hydrodynamic flare simulations are performed using the RADYN code. We find the simulated Hα line profiles with hard and high-energy non-thermal electron beams to be consistent with the initial phase line profiles of the superflares, while those with a softer and/or weak-energy beam are consistent with those in decay phases, indicating the changes in the energy fluxes injected to the lower atmosphere. Also, we find that the relation between the optical continuum and Hα intensity is nonlinear, which can be one cause of the non-white-light flares. The flare energy budget exhibits diversity in the observations and models, and more observations of stellar flares are necessary for constraining the occurrence of various emission line phenomena in stellar flares.