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Cool Stars in the EUV: Spectral and Structural Variability

Published online by Cambridge University Press:  12 April 2016

Alexander Brown*
Affiliation:
Center for Astrophysics and Space Astronomy, University of Colorado, Campus Box 389, Boulder, CO 80309-0389, USA

Abstract

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EUV observations of RS CVn binaries and M dwarf flare stars are used to illustrate the variability of coronal emission seen in EUVE spectra and photometry. The EUVE emission line spectra show that the quiescent coronae of active stars are extremely hot (≥10 million K) and flares, which are even hotter, are common. Spectral sequences showing the evolution of flare temperature and density are presented. Very high coronal electron densities (log Ne ~ 13) have been detected during M dwarf flares. EUVE data for the RS CVn binary HR1099 are compared with those from simultaneous observations in other spectral regions, including X-ray (ASCA), ultraviolet (IUE), and radio (VLA, AT) data. These combined data show that the peak coronal temperature is above the sensitivity of EUVE and that the time of maximum flare brightness is spectral region dependent.

Type
III. Coronae of Cool Stars
Copyright
Copyright © Kluwer 1996

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