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The RS Canum Venaticorum Stars

Published online by Cambridge University Press:  07 August 2017

Marcello Rodonò
Marcello Rodonò*
Affiliation:
Istituto di Astronomia, Università degli Studi, and Osservatorio Astrofisico, I-95125 Catania, Italy

Abstract

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The picture emerging from recent studies of RS CVn-type systems indicates the presence of very active stars showing typical solar-like activity phenomena, such as spots and flares, and possibly mutual interactions. The binary nature of RS CVns is certainly important in enforcing high stellar rotation rates, but the actual clue to the understanding of the intrinsic variability of the component stars resides in their internal structure, where the appropriate physical conditions are met for the generation and intensification of strong magnetic fields, as prescribed by the αω-dynamo models. The most significant results have been derived from multi-wavelength, coordinated observations and long-term monitoring programs.

Recent highlights include: a) the mapping of compact atmospheric structures at various temperature regimes by light curve modelling and spectral (Doppler) imaging techniques; b) clear evidence of long-term activity cycles on RS CVn and other types of interacting binaries; c) the detection and measurement of surface magnetic fields, as derived from the differential Zeeman splitting of spectral lines.

These results clearly demonstrate that the study of RS CVn stars can play a very fundamental role in the understanding of basic stellar physics, as well as in interpreting the characteristic variability of interacting binaries.

Type
Invited Papers
Information
Symposium - International Astronomical Union , Volume 151: Evolutionary Processes in Interacting Binary Stars , 1992 , pp. 71 - 82
Copyright
Copyright © Kluwer 1992 

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