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The Initial Mass Function of Be Stars
Published online by Cambridge University Press: 26 May 2016
Abstract
Allowing for systematic differences in the counting of Be Stars due to their overluminosity, changes produced by their fast rotation on spectral types and time spent in the main sequence, a difference between the IMF (Be) and IMF(B) appears, which indicates that the appearance of the Be phenomenon may relay on differences in the initial star formation conditions.
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- Session 1 Observations of Rotating Stars
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- Copyright © Astronomical Society of the Pacific 2004