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ISO Observations of Be Stars

Published online by Cambridge University Press:  12 April 2016

L.B.F.M. Waters ,
N.R. Trams ,
S. Hony ,
A. de Koter ,
P.W. Morris ,
P.A. Zaal ,
J.M. Marlborough ,
C.E. Millar  and
B. Vandenbussche
L.B.F.M. Waters
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3001 Heverlee, Belgium
N.R. Trams
Affiliation:
Integral Science Operations Centre, ESTEC, P.O. Box 299, 2200 AG Noordwijk, The Netherlands
S. Hony
Affiliation:
Astronomical Institute, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands
A. de Koter
Affiliation:
Integral Science Operations Centre, ESTEC, P.O. Box 299, 2200 AG Noordwijk, The Netherlands
P.W. Morris
Affiliation:
Integral Science Operations Centre, ESTEC, P.O. Box 299, 2200 AG Noordwijk, The Netherlands
P.A. Zaal
Affiliation:
Integral Science Operations Centre, ESTEC, P.O. Box 299, 2200 AG Noordwijk, The Netherlands
J.M. Marlborough
Affiliation:
Department of Physics and Astronomy, University of Western Ontario, London, Ontario N6A 3K7, Canada
C.E. Millar
Affiliation:
Astronomical Institute, University of Amsterdam, Kruislaan 403, NL-1098 SJ Amsterdam, The Netherlands
B. Vandenbussche
Affiliation:
Instituut voor Sterrenkunde, Katholieke Universiteit Leuven, Celestijnenlaan 200B, B-3001 Heverlee, Belgium

Abstract

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We discuss the infrared spectral energy distribution of Be stars, focusing on new results obtained with the Infrared Space Observatory. The 60-160 μm flux of some Be stars is higher than expected, which may be due to cold dust or an outer disk component with enhanced densities. The infrared spectrum of Be stars is dominated by numerous HI recombination lines, whose line strengths show a complex behaviour. The electron temperature in the disk of ϒ Cas was found to be about 9500 K, and evidence for an elevated temperature near the upper part of the disk is presented. Be stars may be recognized from their infrared spectrum on the basis of HI line flux ratios.

Type
2. New Missions
Information
International Astronomical Union Colloquium , Volume 175: The Be Phenomenon in Early-Type Stars , 2000 , pp. 145 - 155
Copyright
Copyright © Astronomical Society of the Pacific 2000

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