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A Starspot Model for the RS CVn Stars

Published online by Cambridge University Press:  14 August 2015

Steven N. Shore  and
Douglas S. Hall
Steven N. Shore
Affiliation:
Astronomy Department, Columbia University Astronomy Department, Case Western Reserve University
Douglas S. Hall
Affiliation:
Dyer Observatory, Vanderbilt University

Extract

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We employ a simplified dynamo model to describe the long term photometric spectroscopic behavior of the RS CVn stars. The essential feature of the model is that the stars are in nearly synchronous rotation, with the differential rotation slower and the rotational velocity higher than for a single evolved 1 to 2 solar mass star. The spot groups are formed by eruption of enhanced toroidal fields, which have areas at the photosphere of several tenths of the surface area; the sizes of these regions are shear limited. Estimates of the lifetimes of active regions and of flare energetics are presented. The RS CVn phenomenon is then related to both the evolutionary status and the orbital parameters of the binary system.

Type
VII. The RS Canum Venaticorum Stars
Information
Symposium - International Astronomical Union , Volume 88: Close Binary Stars: Observations and Interpretation , 1980 , pp. 389 - 396
Copyright
Copyright © Reidel 1980 

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