B[e] Stars with Warm Dust: Revealing the Nature of Unclassified B[e] Stars and Expanding the Family

Details B[e] Stars with Warm Dust: Revealing the Nature of Unclassified B[e] Stars and Expanding the Family B[e] Stars with Warm Dust: Revealing the Nature of Unclassified B[e] Stars and Expanding the Family

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aspc..355..315m&link_type=abstract

Stars with the B[e] Phenomenon. ASP Conference Series, Vol. 355, Proceedings of the Conference Held 10-16 July, 2005, at the Isl

Astronomy and Astrophysics

Astronomy

2

Scientific paper

Until recently, unclassified B[e] stars represented half of the entire B[e] group. Our study of these objects with strong emission-line spectra and IRAS fluxes, decreasing toward longer wavelengths, resulted in a suggestion that they currently form dust in their envelopes. The objects have been tentatively called B[e] stars with warm dust (B[e]WD). Their luminosity range (˜3 orders of magnitude) is much larger compared to previous suggestions that dust formation occurs only near very luminous hot stars. A significant fraction of B[e]WD are recognized or suspected binaries. The group has been expanded with both previously detected hot emission-line stars with IR fluxes, typical for confirmed B[e]WD, and new candidates, found in recent all-sky surveys. Currently the number of B[e]WD members and candidates is ˜60 with an opportunity to find more in existing stellar catalogs. Main observational and physical properties of B[e]WD and their envelopes are summarized. Our results on newly found group members are presented.
Partially based on observations obtained at the Canada-France-Hawaii Telescope (CFHT).

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