Near-Infrared Excess of Classical Be Stars

Details Near-Infrared Excess of Classical Be Stars Near-Infrared Excess of Classical Be Stars

Aug 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aspc..404..302l&link_type=abstract

The Eighth Pacific Rim Conference on Stellar Astrophysics: A Tribute to Kam-Ching Leung ASP Conference Series, Vol. 404, proceed

Astronomy and Astrophysics

Astrophysics

1

Scientific paper

Classical Be stars can attribute their IR excess to free-free emission from ionized gas. Those with exceptionally large IR excess (J-H, and H-K both greater than 0.6 mag), however, must be accounted for by thermal emission from circumstellar dust which is condensed out in the flattened, expanding envelope as these fast-rotating stars evolve to the giant phase.

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