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A Study of the Coronal Plasma in RS CVn binary systems: HR 1099 and co

M. Audard·M. Guedel·A. Sres·R. Mewe·A. J. J. Raassen·E. Behar·C. R. Foley·R. L. J. van der Meer
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Abstract

XMM-Newton has been performing comprehensive studies of X-ray luminous RS CVn binary systems 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 concentrate here on coronal abundances and investigate the abundance pattern in RS CVn binaries as a function of activity and average temperature. We find a transition from an Inverse First Ionization Potential (FIP) effect towards an absence of a clear trend (no FIP) in intermediately active RS CVn systems. This scheme fits well into the long-term evolution from an IFIP to a FIP effect found in solar analogs. We further study variations in the elemental abundances during a large flare.

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M. Audard, M. Guedel, A. Sres, R. Mewe, A. J. J. Raassen, E. Behar, C. R. Foley, R. L. J. van der Meer. 2001-09-17. A Study of the Coronal Plasma in RS CVn binary systems: HR 1099 and co. https://arxiv.org/abs/astro-ph/0109264

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