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Summary: The Twelfth Cool Stars, Stellar Systems and the Sun
University of Colorado, Electronic publication, 2002
A. Brown, T. R. Ayres, G. M. Harper, eds.
A Study of the Coronal Plasma in RS CVn binary systems
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 bright RS CVn binaries in its Calibration and Guaranteed Time
programs. We present results from ongoing investigations in the context
of a systematic study of coronal emission from RS CVns. We concen-
trate in this paper on coronal abundances and investigate the abundance
pattern in RS CVn binaries as a function of activity and average temper-
ature. A transition from an Inverse First Ionization Potential (FIP) e ect
towards an absence of a clear trend (no FIP) is found in intermediately
active RS CVn systems. This scheme corresponds 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
The RS CVn binary system class is loosely de ned as consisting of a chromo-
spherically active evolved star orbiting within a few days around a main-sequence
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