The Effects of Age and Metallicity on Be Circumstellar Disk Formation

Details The Effects of Age and Metallicity on Be Circumstellar Disk Formation The Effects of Age and Metallicity on Be Circumstellar Disk Formation

Mar 2007

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2007aspc..361..527w&link_type=abstract

Active OB-Stars: Laboratories for Stellar and Circumstellar Physics, ASP Conference Series, Vol. 361, Proceedings of the confere

Physics

Scientific paper

We present the latest results of our investigation into the possible role evolutionary age and/or metallicity play in the development of the Be phenomenon. We observe an enhancement in the fractional Be content of early-type stars in clusters of age 10-25 Myr, suggesting that the Be phenomenon becomes more prevalent with evolutionary age; furthermore, we find that the fractional content of early-type Be stars in clusters of age 10-25 Myr is enhanced in low metallicity environments, confirming the results of earlier studies. Our results also offer clear evidence to refute the suggestion of tet{fab00} that the Be phenomenon develops exclusively in the second half of a B star's main sequence lifetime, i.e. no earlier than 10 Myr.

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