The RS CVn–type Star GT Mus Shows Most Energetic X-Ray Flares Throughout the 2010sRyo Sasaki

This research used MAXI data provided by RIKEN, JAXA, and the MAXI team. This work was supported by NASA through the NICER team and the Astrophysics Explorers Program. It used data and software provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. The authors thank Kazunari Shibata for useful discussions and comments on the cooling process. R.S. acknowledges financial support from the Junior Research Associate Program in RIKEN, JSPS Overseas Challenge Program for Young Researchers and Research Assistant Program in Chuo University. Y.T. acknowledges financial support from JSPS KAKENHI grant No. JP17K05392. W.I. acknowledges support from the Special Postdoctoral Researchers Program in RIKEN and JSPS KAKENHI grant No. JP16K17717. Y.M. gratefully acknowledges funding from the Tanaka Kikinzoku Memorial Foundation. M.S. acknowledges financial support from JSPS KAKENHI grant No. JP16K17672.