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Summary: Stellar Coronae in the Chandra and XMM-Newton Era
ASP Conference Series, Vol. TBD, 2001
F. Favata & J. Drake
Flare Heating of Stellar Coronae
Vinay Kashyap & Jeremy Drake
SAO, 60 Garden St., Cambridge MA 02138, USA
Marc Audard & Manuel Gudel
PSI, 5232 Villigen PSI, Switzerland
Abstract. We model the emission from the coronae of active stars
FK Aqr, V1054 Oph, AD Leo, and Per as a superposition of numerous
weak
ares whose numbers are distributed as a power-law in energy. We
nd that most of the emission on these stars may be attributed to
aring
activity.
1. Introduction
An open question in the eld of Solar and stellar astrophysics is the source of
heating that causes stellar coronae to reach temperatures of millions of degrees.
One possibility is that the coronae are heated by a large number of small
ares
(see Gudel & Benz 1993; Gudel et al. 1997; Gudel 1997; Audard et al. 1999,
2000).
On the Sun,
ares are distributed with energy as a power-law E with
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