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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

References

Brown, J.C., McLean, I.S., and Emslie, A.G.: 1978, Astron. Astrophys. 68, 413 Google Scholar
Busso, M., Scaltriti, F., Persi, P., Robberto, M., and Silvestro, G.: 1987, Astron. Astrophys. 183, 83 Google Scholar
Busso, M., Scaltriti, F., Persi, P., Ferrari-Toniolo, M., and Origlia, L.: 1988, Mon. Not. R. astr. Soc. 234, 445 Google Scholar
Busso, M., and Scaltriti, F.: 1990, in preparation.Google Scholar
Jones, T.W., and Merrill, K.M.: 1976, Astrophys. J. 209, 509.Google Scholar
Koch, R.H., Hrivnak, B.J., Bradstreet, D.H., Blitzstein, W., Pfeiffer, R.J., and Perry, P.M.: 1985, Astrophys. J. 288, 731 Google Scholar
Korhonen, T., Piirola, V., and Reiz, A.: 1984, The ESO Messenger, December 1984Google Scholar
Liu, Xuefu and Tan, Huisong: 1987, Acta Astr. Sinica 28, 139.Google Scholar
Pfeiffer, R.J.: 1979, Astrophys. J. 232, 181.Google Scholar
Piirola, V.: 1973, Astron. Astrophys. 27, 383.Google Scholar
Piirola, V.: 1988, in Polarized Radiation of Circumstellar Origin, eds. Coyne, G.V. et al., Univ. of Arizona Press, p. 735.Google Scholar
Popper, D.M., and Ulrich, R.K.: 1977, Astrophys. J. Letters 212, L131.Google Scholar
Scaltriti, F., Piirola, V., Cellino, A., Anderlucci, E., Corcione, L., Massone, G., Racioppi, F.: 1989, Mem. S.A.It. 60, 243.Google Scholar
Weiler, E.J., Owen, F.N., Bopp, B.W., Schmitz, M., Hall, D.S., Fraquelli, D.A., Piirola, V., Ryle, M., and Gibson, D.M.: 1978, Astrophys. J. 225, 919.Google Scholar