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Paper: Feeding a Disk: The Mechanical Mass Loss of Be Stars from a Numerical Point of View
Volume: 453, Advances in Computational Astrophysics: Methods, Tools, and Outcome
Page: 353
Authors: Ekström, S.; Georgy, C.; Granada, A.; Wyttenbach, A.; Meynet, G.
Abstract: Be stars are supposed to rise from fast rotating stars losing mass in an equatorial disk. As stars evolve on the Main Sequence, they tend to get closer from the critical limit where the gravity is challenged by the centrifugal force. At that moment, a mechanical mass loss allows to lose the excess of angular momentum brought to the surface by internal transport mechanisms. We present the results of a new grid of stellar models in which several models reach the critical limit during their evolution. An estimation of the mass loss rate is obtained and compared with observations of Be stars.
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