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• W2496863071 abstract "The actual characteristic average surface angular velocity ratio of the Be phenomenon may be higher than Ω/Ω c = 0.8 ± 0.1 derived from v sin i values not corrected from gravity darkening effects. Late Be Stars need not only higher values of Ω/Ω c , but also larger main sequence age ratios τ/τ MS than early Be Stars to display the Be phenomenon. Galactic field Be Stars appear at any MS phase, but their frequency is higher for τ/τ MS ≳ 0.5. Be Stars are probably neat differential rotators, i.e. they rotate with energy ratios kinetic/|gravitational| larger than withstood by critical rigid rotators. Initial formation conditions must favor the existence of fast rotators, while only a small fraction of them could be accounted for by mass transfer in close binary systems. Bn stars could perhaps represent a pre-Be phase." @default.
• W2496863071 created "2016-08-23" @default.
• W2496863071 creator A5049438697 @default.
• W2496863071 date "2004-01-01" @default.
• W2496863071 modified "2023-10-17" @default.
• W2496863071 title "Rotation and Properties of Be Stars" @default.
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• W2496863071 doi "https://doi.org/10.1017/s0074180900195269" @default.
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