K- and L-band spectroscopy of Be stars

Details K- and L-band spectroscopy of Be stars K- and L-band spectroscopy of Be stars

Jul 2011

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011iaus..272..392g&link_type=abstract

Active OB stars: structure, evolution, mass loss, and critical limits, Proceedings of the International Astronomical Union, IAU

Astronomy and Astrophysics

Astronomy

Stars: Emission-Line, Be, Circumstellar Matter

Scientific paper

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.

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