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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

References

Ashok, N.M., Bhatt, H.C., Kulkami, P.V., et al. 1984, MNRAS, 211, 471 Google Scholar
Bjorkman, J., Cassinelli, J.P. 1993, ApJ, 409, 429 CrossRefGoogle Scholar
Cassinelli, J.P., Hartmann, L. 1979 ApJ, 212, 488 Google Scholar
Chalabaev, A.A., Maillard, J.P. 1985, ApJ, 294, 640 Google Scholar
Coté, J., Waters, L.B.F.M. 1987, A&A, 176, 93 Google Scholar
Dachs, J., Wamsteker, W. 1982, A&A, 107, 240 Google Scholar
Dachs, J., Hanuschik, R., Kaiser, D., Rohe, D. 1986, A&A, 159, 276 Google Scholar
Dougherty, S.M., Taylor, A.R. 1992, Nature 359, 808 Google Scholar
Dougherty, S.M., Taylor, A.R. 1994, MNRAS, 269 1123 Google Scholar
Dougherty, S.M., Waters, L.B.F.M., Burki, , et al. 1994, A&A, 290, 609 Google Scholar
Gehrz, R.D., Hackwell, J.A., Jones, T.W. 1974, ApJ, 191, 675 CrossRefGoogle Scholar
Hamann, F., Simon, M. 1987, ApJ, 318 356 Google Scholar
Hanuschik, R.W. 1987, A&A, 173, 299 Google Scholar
Hony, S., Waters, L.B.F.M., Zaal, P.A. et al. 2000, A&A, in pressGoogle Scholar
Hummer, D.G., Storey, P.J. 1987, MNRAS, 224, 801 Google Scholar
De Graauw, Th., et al. 1996, A&A, 315, L49 Google Scholar
Kessler, M.F., et al. 1996, A&A, 315, L27 Google Scholar
Lamers, H.J.G.L.M., Najarro, P., Kudritzki, R.P., et al. 1996, A&A, 315, L229 Google Scholar
Lemke, D., et al. 1996 A&A, 315, L64 Google Scholar
Marlborough, J.M., Zijlstra, J.-W., Waters, L.B.F.M. 1997, A&A, 321, 867 Google Scholar
McLean, I.S., Brown, J.D. 1978 A&A, 69, 291 Google Scholar
Millar, C.E., Marlborough, J.M. 1998, ApJ, 494, 715 CrossRefGoogle Scholar
Persson, S.E., McGregor, P.J. 1985, AJ, 90, 1860 CrossRefGoogle Scholar
Quirrenbach, A., Bjorkman, K.S., Bjorkman, , et al. 1997, ApJ, 479, 477 Google Scholar
Rinehart, S.A., Houck, J.R., Smith, J.D. 2000, AJ, in pressGoogle Scholar
Sellgren, K., Smith, R.G. 1992, ApJ, 388, 178 Google Scholar
Slettebak, A. 1982, ApJS, 50, 55 Google Scholar
Stee, Ph., de Araujo, F.X., Vakili, F., Mourard, D., et al. 1995, A&A, 300, 219 Google Scholar
Stee, Ph., Vakili, F., Bonneau, D., Mourard, D. 1998, A&A, 332, 268 Google Scholar
Taylor, A.R., Waters, L.B.F.M., Bjorkman, K.S., Dougherty, S.M. 1990, A&A, 231, 453 Google Scholar
Telting, J., Waters, L.B.F.M., Persi, P., Dunlop, S.R. 1993, A&A, 270, 355 Google Scholar
Waters, L.B.F.M. 1986, A&A, 162, 121 Google Scholar
Waters, L.B.F.M., Coté, J., Lamers, H.J.G.L.M. 1987, A&A, 176, 93 Google Scholar
Waters, L.B.F.M., van der Veen, W.E.C.J., Taylor, A.R., et al. 1991, A&A, 244, 120 Google Scholar
Waters, L.B.F.M., Marlborough, J.M. 1992, A&A, 253, L25 Google Scholar
Wright, A.E., Barlow, M.J. 1975, MNRAS, 170, 41 CrossRefGoogle Scholar
Zaal, P.A., Waters, L.B.F.M., Marlborough, J.M. 1995 A&A, 299, 574 Google Scholar