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Polarimetric Observations of Active Cool Binaries

Published online by Cambridge University Press:  12 April 2016

R.H. Koch ,
N.M. Elias ,
B.D. Holenstein ,
V. Piirola ,
F. Scaltriti  and
G.V. Coyne
R.H. Koch
Affiliation:
University of Pennsylvania, Philadelphia, U.S.A.
N.M. Elias
Affiliation:
University of Pennsylvania, Philadelphia, U.S.A.
B.D. Holenstein
Affiliation:
University of Pennsylvania, Philadelphia, U.S.A.
V. Piirola
Affiliation:
Observatory and Astrophysics Laboratory, Helsinki, Finland
F. Scaltriti
Affiliation:
Osservatorio Astronomico di Torino, Pino Torinese, Italia
G.V. Coyne
Affiliation:
Vatican Observatory, Città del Vaticano

Extract

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For a sample of RS CVn binaries Busso and collaborators (Busso et al., 1987, 1988; Busso and Scaltriti, 1990) compared the observed energy distribution from the UV to the near-IR (and to IRAS bandpasses for some objects) with those calculated from the known radii and spectral types of the stellar components. About 25% of the sample gave evidence of an IR excess up to 0.7 mag, generally starting from the I-band. The excess is significantly larger than observational error. These same authors ascribe the excess to a thin dust shell surrounding the binary. Using the “dirty silicates” model by Jones and Merrill (1976) they find for the shell a temperature range of 1500 K to 2000 K, an optical depth of about 0.01 at 10 micrometers in the shell, and a distance of the shell from the stars to be typically about 100 times the radius of the larger star.

Type
Part IV Stellar activity
Information
International Astronomical Union Colloquium , Volume 130: The Sun and Cool Stars: activity, magnetism, dynamos , 1991 , pp. 427 - 429
Copyright
Copyright © Springer-Verlag 1991

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