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ARE CORONAE OF MAGNETICALLY ACTIVE STARS HEATED BY FLARES? II. EXTREME ULTRAVIOLET AND X-RAY FLARE STATISTICS AND THE
 

Summary: ARE CORONAE OF MAGNETICALLY ACTIVE STARS HEATED BY FLARES? II.
EXTREME ULTRAVIOLET AND X-RAY FLARE STATISTICS AND THE
DIFFERENTIAL EMISSION MEASURE DISTRIBUTION
Manuel Gu¨del and Marc Audard1
Paul Scherrer Institut, Wu¨renlingen and Villigen, CH-5232 Villigen PSI, Switzerland;
guedel@astro.phys.ethz.ch, audard@astro.columbia.edu
Vinay L. Kashyap and Jeremy J. Drake
Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138;
vkashyap@cfa.harvard.edu, jdrake@cfa.hardvard.edu
and
Edward F. Guinan
Department of Astronomy and Astrophysics, Villanova University, Villanova, PA 19085;
edward.guinan@villanova.edu
Received 2002 July 30; accepted 2002 September 6
ABSTRACT
We investigate the EUV and X-ray flare rate distribution in radiated energy of the late-type active star AD
Leo. Occurrence rates of solar flares have previously been found to be distributed in energy according to a
power law, dN=dE / EŔ, with a power-law index in the range 1.5­2.6. If ! 2, then an extrapolation of
the flare distribution to low flare energies may be sufficient to heat the complete observable X-ray/EUV
corona. We have obtained long observations of AD Leo with the EUVE and BeppoSAX satellites. Numerous

  

Source: Audard, Marc - INTEGRAL Science Data Centre & Observatory of Geneva, Université de Genčve

 

Collections: Physics