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Paper: The Effects of Age and Metallicity on Be Circumstellar Disk Formation
Volume: 361, Active OB-Stars: Laboratories For Stellar and Circumstellar Physics
Page: 527
Authors: Wisniewski, J.P.; Bjorkman, K.S.; Magalhaes, A.M.; Bjorkman, J.E.
Abstract: 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 Fabregat & Torrejon (2000) 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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