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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 

References

Asplund, M., Grevesse, N., & Sauval, A. J. 2005, in Barnes, T. G. III & Bash, F. N. (eds.), Cosmic Abundances as Records of Stellar Evolution and Nucleosynthesis, Vol. 336 of Astronomical Society of the Pacific Conference Series, p. 25Google Scholar
Badnell, N. R., Bautista, M. A., Butler, K., et al. 2005, MNRAS 360, 458CrossRefGoogle Scholar
Bouabid, M.-P., Dupret, M.-A., Salmon, S., et al. 2013, MNRAS 429, 2500CrossRefGoogle Scholar
Dupret, M.-A. 2002, Non-radial non-adiabatic oscillations of near main sequence variable stars, Vol. 71Google Scholar
Ekström, S., Georgy, C., Granada, A., Wyttenbach, A., & Meynet, G. 2012, in Capuzzo-Dolcetta, R., Limongi, M., & Tornambè, A. (eds.), Advances in Computational Astrophysics: Methods, Tools, and Outcome, Vol. 453 of Astronomical Society of the Pacific Conference Series, p. 353Google Scholar
Granada, A., Ekström, S., Georgy, C., et al. 2012, in Carciofi, A. C. & Rivinius, T. (eds.), Circumstellar Dynamics at High Resolution, Vol. 464 of Astronomical Society of the Pacific Conference Series, p. 117Google Scholar
Ishimatsu, H. & Shibahashi, H. 2013, in Shibahashi, H. & Lynas-Gray, A. E. (eds.), Astronomical Society of the Pacific Conference Series, Vol. 479 of Astronomical Society of the Pacific Conference Series, p. 325Google Scholar
Neiner, C., Mathis, S., Saio, H., & Lee, U. 2013, in Shibahashi, H. & Lynas-Gray, A. E. (eds.), Astronomical Society of the Pacific Conference Series, Vol. 479 of Astronomical Society of the Pacific Conference Series, p. 319Google Scholar
Porter, J. M. & Rivinius, T. 2003, PASP 115, 1153CrossRefGoogle Scholar
Scuflaire, R., Théado, S., Montalbán, J., et al. 2008, Ap&SS 316, 83Google Scholar
Shibahashi, H. 2014, in Guzik, J. A., Chaplin, W. J., Handler, G., & Pigulski, A. (eds.), IAU Symposium, Vol. 301 of IAU Symposium, pp 173–176Google Scholar