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Modelling of an Eclipsing RS CVn Binary: V405 And

Published online by Cambridge University Press:  23 April 2012

Krisztián Vida ,
Katalin Oláh  and
Zsolt Kővári
Krisztián Vida
Affiliation:
Konkoly Observatory, Konkoly Thege út 15-17., H-1121 Budapest, Hungary email: vida@konkoly.hu, olah@konkoly.hu, kovari@konkoly.hu
Katalin Oláh
Affiliation:
Konkoly Observatory, Konkoly Thege út 15-17., H-1121 Budapest, Hungary email: vida@konkoly.hu, olah@konkoly.hu, kovari@konkoly.hu
Zsolt Kővári
Affiliation:
Konkoly Observatory, Konkoly Thege út 15-17., H-1121 Budapest, Hungary email: vida@konkoly.hu, olah@konkoly.hu, kovari@konkoly.hu
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Abstract

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V405 And is an ultrafast-rotating (Prot ≈ 0.46 days) eclipsing binary. The system consists of a primary star with radiative core and convective envelope, and a fully convective secondary. Theories have shown that stellar structure can depend on magnetic activity, i.e., magnetically active M-dwarfs should have larger radii. Earlier light curve modelling of V405 And indeed showed this behaviour: we found that the radius of the primary is significantly larger than the theoretically predicted value for inactive main sequence stars (the discrepancy is the largest of all known objects), while the secondary fits well to the mass-radius relation. By modelling our recently obtained light curves, which show significant changes of the spotted surface of the primary, we can find further proof for this phenomenon.

Keywords

stars:activitybinaries: eclipsingstars: fundamental parametersstars: late-typestars: spots
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. 199 - 200
Copyright
Copyright © International Astronomical Union 2012

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