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The Coronae of RS CVn Systems

Published online by Cambridge University Press:  14 August 2015

Frederick M. Walter ,
Philip A. Charles  and
Stuart Bowyer
Frederick M. Walter
Affiliation:
Space Sciences Laboratory University of California, Berkeley 94720
Philip A. Charles
Affiliation:
Space Sciences Laboratory University of California, Berkeley 94720
Stuart Bowyer
Affiliation:
Space Sciences Laboratory University of California, Berkeley 94720

Extract

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RS CVn systems [1] are close binaries consisting of two late-type stars, one of which has evolved to the base of the giant branch. In most cases, the systems appear to be the product of normal stellar evolutionary processes [2,3]. These systems have attracted much recent attention because they exhibit greatly exaggerated stellar activity in the form of strong chromospheric emission [1]. There is evidence that a large fraction of the surface is covered by dark spots [4]. They also exhibit radio emission [5,6], and quiescent and flaring soft X-ray emission [7-12]. If these stars are undergoing normal evolution, why then are they so peculiar?

Type
VII. The RS Canum Venaticorum Stars
Information
Symposium - International Astronomical Union , Volume 88: Close Binary Stars: Observations and Interpretation , 1980 , pp. 397 - 402
Copyright
Copyright © Reidel 1980 

References

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