Circumstellar Disk Systems in the LMC, SMC, and Milky Way Galaxy

Details Circumstellar Disk Systems in the LMC, SMC, and Milky Way Galaxy Circumstellar Disk Systems in the LMC, SMC, and Milky Way Galaxy

Nov 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..337..333w&link_type=abstract

The Nature and Evolution of Disks Around Hot Stars, ASP Conference Series, Vol. 337, Proceedings of a meeting held 7-9 July 2004

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Scientific paper

Classical Be stars are rapidly rotating near main-sequence B-type stars which have gaseous circumstellar disks. Our understanding of these stars is incomplete, especially as regards two fundamental questions: 1) Is the Be phenomenon an evolutionary effect? and 2) What role does metallicity play in the formation of Be circumstellar disks? Initial attempts to address these questions have used 2-color diagram photometric techniques to determine the frequency of candidate Be stars in clusters of various ages and metallicities. These techniques classify all B type objects with excess Hα emission as classical Be stars, without accounting for the likelihood that other B-type stars, such as post main-sequence B[e] stars, YSOs, and B-supergiants, may also exhibit Hα emission and therefore contaminate the sample. We discuss our efforts to quantify the reliability of 2-color diagrams to identify classical Be stars.

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