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Leaky-wave-induced disks around Be stars: a pulsational analysis on their formation

Published online by Cambridge University Press:  23 January 2015

Melanie Godart ,
Hiromoto Shibahashi  and
Marc-Antoine Dupret
Melanie Godart
Affiliation:
Dept. of Astronomy, The University of Tokyo, Japan email: [email protected]
Hiromoto Shibahashi
Affiliation:
Dept. of Astronomy, The University of Tokyo, Japan email: [email protected]
Marc-Antoine Dupret
Affiliation:
Dept. of Astrophysics, Geophysics and Oceanography, University of Liège, Belgium
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Abstract

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Be stars are B-type stars near the main sequence which undergo episodic mass loss events detected by emission lines, whose line shape and intensity vary with a timescale of the order of decades. Spectroscopic observations show a large rotation velocity such that one of the prevailing scenarios for the formation of the equatorial disk consists in an increasing equatorial rotation velocity to the break-up limit where gravity is challenged by the centrifugal force. We investigate here a new scenario recently suggested by Ishimatsu & Shibahashi (2013), in which the transport of angular momentum through the photosphere would be achieved by leaky waves, keeping the rotation velocity still below the break-up limit.

Keywords

stars: emission-lineBeoscillationsrotation
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 215 - 217
Copyright
Copyright © International Astronomical Union 2015 

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