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Summary: Stellar Coronae in the Chandra and XMM-Newton Era
ASP Conference Series, Vol. TBD, 2001
F. Favata & J. J. Drake
A Study of the Coronal Plasma in RS CVn binary
systems: HR 1099 and co.
M. Audard 1 , M. Gudel 1 , A. Sres 1;2 , R. Mewe 3 , A. J. J. Raassen 3;4 , E.
Behar 5 , C. R. Foley 6 , R. L. J. van der Meer 3
Abstract. XMM-Newton has been performing comprehensive studies
of X-ray luminous RS CVn binary systems in its calibration and guar-
anteed time programs. We present results from ongoing investigations in
the context of a systematic study of coronal emission from RS CVns. We
concentrate here on coronal abundances and investigate the abundance
pattern in RS CVn binaries as a function of activity and average tem-
perature. We nd a transition from an Inverse First Ionization Potential
(FIP) e ect towards an absence of a clear trend (no FIP) in intermedi-
ately active RS CVn systems. This scheme ts well into the long-term
evolution from an IFIP to a FIP e ect found in solar analogs. We further
study variations in the elemental abundances during a large
are.
1. Introduction
RS CVn binary systems generally consist of a chromospherically active evolved
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