Fast optical flares from M dwarfs detected by a one-second-cadence survey with Tomo-e Gozen
Kobayashi, Naoto; Takita, Satoshi; Arimatsu, Ko; Kawana, Kojiro; Doi, Mamoru; Kawahara, Hajime; Ohsawa, Ryou; Sako, Shigeyuki; Tajiri, Tomoyuki; Aizawa, Masataka; Kashiyama, Kazumi; Shigeyama, Toshikazu; Kasuga, Toshihiro; Okumura, Shin-ichiro; Arima, Noriaki; Kondo, Sohei; Mori, Yuki; Hartwig, Tilman; Naokawa, Fumihiro; Jiang, Hanchun; Fujisawa, Kotaro
China, Japan
Abstract
We report on a one-second-cadence wide-field survey for M-dwarf flares using the Tomo-e Gozen camera mounted on the Kiso Schmidt telescope. We detect 22 flares from M3-M5 dwarfs with a rise time of 5 s ≲ trise ≲ 100 s and an amplitude of 0.5 ≲ ΔF/F⋆ ≲ 20. The flare light-curves mostly show steeper rises and shallower decays than those obtained from the Kepler one-minute cadence data and tend to have flat peak structures. Assuming a blackbody spectrum with a temperature of 9000-15000 K, the peak luminosities and energies are estimated to be 1029 erg s-1 ≲ Lpeak ≲ 1031 erg s-1 and 1031 erg ≲ Eflare ≲ 1034 erg, which constitutes the bright end of fast optical flares for M dwarfs. We confirm that more than $90\%$ of the host stars of the detected flares are magnetically active based on their Hα-emission-line intensities obtained by LAMOST. An estimated occurrence rate of detected flares is ~0.7 per day per active star, indicating they are common in magnetically active M dwarfs. We argue that the flare light-curves can be explained by the chromospheric compression model: the rise time is broadly consistent with the Alfvén transit time of a magnetic loop with a length scale of lloop ~ 104 km and a field strength of 1000 gauss, while the decay time is likely determined by the radiative cooling of the compressed chromosphere down near to the photosphere with a temperature of ≳ 10000 K. These flares from M dwarfs could be a major contamination source for a future search of fast optical transients of unknown types.