| dc.description.abstract | Flare events are eruptive brightening observed on the surface of late-type stars. The solar-type stars known to have convection layers produce magnetic fields, and those areas exposed to considerable magnetic fluxes are visible as spots on the surface. Some M dwarfs, the later spectral types, the more so, being more convective, are even more prone to such stellar flares, with higher occurrence rates and significantly more energetic during the flares in comparison to the quiescent photometric luminosities.
Here we report the optical flare activity of Wolf 359 (GJ409; CN Leo). This relatively young (< 1 Gyr) red dwarf (M6.5 Ve), being the fifth nearest stellar system (2.4 pc) to the Sun, is known for its frequent optical flares, along with gamma-ray and X-ray bursts. Our data consist of 27 hours spanning seven days in April 2020 of photometric monitoring with two small telescopes in Xinjiang, including a one-meter and one of the TAOS 0.5 m telescopes recently relocated from Lulin Observatory. A total of 13 flares with energies greater than 1029 ergs were detected, including one ”superflare” event (∼ 1031 ergs), implying an average occurrence rate of one flare per two hours. Each flare is parameterized and fitted the decay phase with exponential templates. For the ”superflare” event, which was observed simultaneously by two telescopes, we simulate how do the sampling functions influence the profiles and recover the ”possible truth” of this particular event. We also discuss how the sampling function reshapes the underlying profile, and therefore different energy budgets are derived. | en_US |