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Stellar Coronae in the Chandra and XMM-Newton Era ASP Conference Series, Vol. TBD, 2001
 

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

  

Source: Audard, Marc - INTEGRAL Science Data Centre & Observatory of Geneva, Université de Genève
Guedel, Manuel - Institut für Astronomie, Universität Wien

 

Collections: Physics