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Differential Rotation in Two RS CVn Systems: σ Gem and ζ And

Published online by Cambridge University Press:  23 April 2012

Zsolt Kővári ,
János Bartus ,
Levente Kriskovics ,
Katalin Oláh ,
Krisztián Vida ,
Orsolya Ribárik  and
Klaus G. Strassmeier
Zsolt Kővári
Affiliation:
Konkoly Observatory, Konkoly Thege út 15-17., H-1121 Budapest, Hungary email: [email protected], [email protected], [email protected], [email protected], [email protected]
János Bartus
Affiliation:
Konkoly Observatory, Konkoly Thege út 15-17., H-1121 Budapest, Hungary email: [email protected], [email protected], [email protected], [email protected], [email protected] Leibniz Institute for Astrophysics Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany email: [email protected], [email protected]
Levente Kriskovics
Affiliation:
Konkoly Observatory, Konkoly Thege út 15-17., H-1121 Budapest, Hungary email: [email protected], [email protected], [email protected], [email protected], [email protected]
Katalin Oláh
Affiliation:
Konkoly Observatory, Konkoly Thege út 15-17., H-1121 Budapest, Hungary email: [email protected], [email protected], [email protected], [email protected], [email protected]
Krisztián Vida
Affiliation:
Konkoly Observatory, Konkoly Thege út 15-17., H-1121 Budapest, Hungary email: [email protected], [email protected], [email protected], [email protected], [email protected]
Orsolya Ribárik
Affiliation:
Konkoly Observatory, Konkoly Thege út 15-17., H-1121 Budapest, Hungary email: [email protected], [email protected], [email protected], [email protected], [email protected]
Klaus G. Strassmeier
Affiliation:
Leibniz Institute for Astrophysics Potsdam, An der Sternwarte 16, 14482 Potsdam, Germany email: [email protected], [email protected]
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Abstract

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The differentially rotating convective envelope is an indispensable element of the magnetic dynamo working in RS CVn-systems. Tidal coupling is responsible for maintaining fast rotation, and also the observed high level of magnetic activity. In this work, we compare the physical properties of two well known RS CVn-type binaries, that is the long-period system σ Gem and the ellipsoidal variable ζ And. For the comparison, we use the results obtained from processing time-series Doppler images. We also aim at understanding how differential rotation could be affected by tidal forces in such close binaries.

Keywords

stars: activitystars: imagingstars: individual (σ Gem, ζ And)stars: spotsstars: late-type
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 7 , Symposium S282: From Interacting Binaries to Exoplanets: Essential Modeling Tools , July 2011 , pp. 197 - 198
Copyright
Copyright © International Astronomical Union 2012

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