A Search for Be Stars in Open Clusters

Details A Search for Be Stars in Open Clusters A Search for Be Stars in Open Clusters

Nov 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005aspc..337..270m&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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Be stars are a class of B stars with circumstellar disks that cause Balmer and other line emission. There are three possible reasons for the rapid rotation of Be stars: they may have been born as rapid rotators, spun up by binary mass transfer, or spun up during the main-sequence evolution of B stars. To test the various formation scenarios, we are conducting a photometric survey of 57 young open clusters (of which 20 are discussed here) to determine their fraction of Be stars relative to B stars as a function of cluster age. Low metallicity and/or high cluster density may also favor Be star formation, and we investigate these possibilities as well.

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