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Highly Energetic Physical Processes and Mechanisms for Emission from Astrophysical Plasmas
 

Summary: Highly Energetic Physical Processes and
Mechanisms for Emission from Astrophysical Plasmas
IAU Symposium, Vol. 195, 1999
P. C. H. Martens and S. Tsuruta, eds.
Active Late-Type Stellar Coronae: Hints for Flare Heating?
M. Audard 1;2 , M. Gudel 1;2 , J. J. Drake 3 , V. Kashyap 3 , & E. F. Guinan 4
Abstract. The Extreme Ultraviolet Explorer data archive has been used
to study are energy distributions and infer the role of ares in coronal
heating. We have constructed are number distributions as a function of
observed EUV and X-ray emitted thermal energy. We nd cumulative
are distributions of the form N(> E) / E +1 with  1:5 2:6. We
present results in the context of spectral type classi cation.
1. Introduction
To explain coronal temperatures (1 30 MK), it has been proposed that ares
play a crucial role (e.g. Parker 1988). Flares have been found to be distributed in
energy according to a power law, i.e., dN=dE / E , with around 2. Hudson
(1991) argued that, if > 2 for solar micro ares, an extrapolation to lower
energies may provide the energy necessary to heat the whole corona. We have
initiated a project in which we analyze data from the EUVE archive to study
coronal heating on active late-type stars. Audard et al. (1999) found indices

  

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

 

Collections: Physics