White-light Superflare and Long-term Activity of the Nearby M7-type Binary EI Cnc Observed with GWAC System

• Published in: The Astrophysical journal Vol. 954; no. 2; pp. 142 - 152
• Main Authors: Li, Hua-Li, Wang, Jing, Xin, Li-Ping, Bai, Jian-Ying, Han, Xu-Hui, Cai, Hong-Bo, Huang, Lei, Lu, Xiao-Meng, Qiu, Yu-Lei, Wu, Chao, Li, Guang-Wei, Deng, Jing-Song, Xu, Da-Wei, Yang, Yuan-Gui, Wang, Xiang-Gao, Liang, En-Wei, Wei, Jian-Yan
• Format: Journal Article
• Language: English
• Published: Philadelphia The American Astronomical Society 01.09.2023; IOP Publishing
• Subjects: Astrophysics; Binary stars; Chemical properties; Extrasolar planets; Frequency distribution; Light curve; Stars; Stellar flares; White light
• ISSN: 0004-637X; 1538-4357
• DOI: 10.3847/1538-4357/ace59b

Abstract Stellar white-light flares are believed to play an essential role in the physical and chemical properties of the atmosphere of the surrounding exoplanets. Here we report an optical monitoring campaign on the nearby flaring system EI Cnc carried out by the Ground-based Wide Angle Camera (GWAC) and its dedicated follow-up telescope. A superflare, coming from the brighter component EI CncA, was detected and observed, in which four components are required to properly model the complex decay light curve. The lower limit of flare energy in the R − band is estimated to be 3.3 × 10 32 erg. A total of 27 flares are additionally detected from the GWAC archive data with a total duration of 290 hr. The inferred cumulative flare frequency distribution follows a quite shallow power-law function with a slope of β = − 0.50 ± 0.03 over the energy range between 10 30 and 10 33 erg, which reinforces the trend that stars cooler than M4 show enhanced superflare activity. The flares identified in EI Cnc enable us to extend the τ – E relationship previously established in the white-light superflares of solar-type stars down to an energy as low as ∼10 30 erg (i.e., by 3 orders): τ ∝ E 0.42±0.02 , which suggests a common flare mechanism for stars with a type from M to solar-like and implies an invariant of B 1/3 υ A in the white-light flares.