K and L Band spectroscopy of Be stars.

GRANADA, A.; ARIAS, M. L.; CIDALE, L. S.; MENNICKENT, R.

Paris

Simposio; IAU Symposium 272: Active OB stars: structure, evolution, mass loss, and critical limits; 2010

International Astronomical Union

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.