The RS CVn–type Star GT Mus Shows Most Energetic X-Ray Flares Throughout the 2010sRyo Sasaki
2021
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.
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