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

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dc.creatorAudard, M.
dc.creatorGuedel, M.
dc.creatorSres, A.
dc.creatorMewe, R.
dc.creatorRaassen, A. J. J.
dc.creatorBehar, E.
dc.creatorFoley, C. R.
dc.creatorvan der Meer, R. L. J.
dc.date2001-09-17
dc.date.accessioned2026-07-07T02:00:00Z
dc.date.available2026-07-07T02:00:00Z
dc.descriptionXMM-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.
dc.descriptionto appear in 35th ESLAB Symposium "Stellar Coronae in the Chandra and XMM-Newton Era", eds. F. Favata & J.J. Drake (San Francisco: ASP), in press
dc.identifierhttps://arxiv.org/abs/astro-ph/0109264
dc.identifierhttp://arxiv.org/abs/astro-ph/0109264
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/3336
dc.subjectAstrophysics
dc.titleA Study of the Coronal Plasma in RS CVn binary systems: HR 1099 and co
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