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K- and L-band spectroscopy of Be stars

Published online by Cambridge University Press:  12 July 2011

Anahí Granada
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina Instituto de Astrofísica La Plata, CCT La Plata-CONICET-UNLP, Argentina Observatoire de Genève. Université de Genève, Suisse email: [email protected]
María L. Arias
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina Instituto de Astrofísica La Plata, CCT La Plata-CONICET-UNLP, Argentina
Lydia S. Cidale
Affiliation:
Facultad de Ciencias Astronómicas y Geofísicas, Universidad Nacional de La Plata, Argentina Instituto de Astrofísica La Plata, CCT La Plata-CONICET-UNLP, Argentina
Ronald E. Mennickent
Affiliation:
Departamento de Astronomía, Universidad de Concepción, Chile
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Abstract

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We describe the behaviour of IR hydrogen emission lines of a sample of Be stars and discuss the physical properties of the circumstellar envelopes of Be stars classified in Groups I and II (Mennickent et al. 2009). We find that while Humphreys and Pfund lines of Group I stars form in an optically thick envelope/disk, Group II stars show Pfund lines that form in an optically thick medium and Humphreys lines originating in optically thinner regions. The transition between Groups I and II could be understood in terms of the evolution of the circumstellar disk of the star and might bring clues on the mechanism originating the Be phenomenon.

Type
Contributed Papers
Copyright
Copyright © International Astronomical Union 2011

References

Granada, A., Arias, M. L. & Cidale, L. S. 2010, AJ, 139, 1983CrossRefGoogle Scholar
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Lenorzer, A., Vandenbussche, B., Morris, P., de Koter, A. et al. 2002b, A&A, 384, 473Google Scholar
Mennickent, R. E., Sabogal, B., Granada, A., & Cidale, L. 2009, PASP, 121, 125CrossRefGoogle Scholar