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K- and L-band spectroscopy of Be stars

Published online by Cambridge University Press:  12 July 2011

Anahí Granada ,
María L. Arias ,
Lydia S. Cidale  and
Ronald E. Mennickent
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: granada@fcaglp.unlp.edu.ar
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.

Keywords

stars: emission-lineBecircumstellar matter

References

Granada, A., Arias, M. L. & Cidale, L. S. 2010, AJ, 139, 1983CrossRefGoogle Scholar
Lenorzer, A., de Koter, A. & Waters, L. B. F. M. 2002a, A&A, 386, L5Google Scholar
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