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Progress and problems in massive star pulsation theory

Published online by Cambridge University Press:  27 October 2016

Hideyuki Saio ,
Cyril Georgy  and
Georges Meynet
Hideyuki Saio
Affiliation:
Astronomical Institute, Graduate School of Science, Tohoku University, Sendai 980-8578, Japan email: saio@astr.tohoku.ac.jp
Cyril Georgy
Affiliation:
Astrophysics, Lennard-Jones Laboratories, EPSAM, Keele University, Staffordshire ST5 5BG, UK email: c.georgy@keele.ac.uk
Georges Meynet
Affiliation:
Geneva Observatory, University of Geneva, Maillettes 51, CH-1290 Versoix, Switzerland email: Georges.Meynet@unige.ch
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Abstract

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Massive stars pulsate in various modes; radial and nonradial p-modes, g-modes, and strange modes including oscillatory convective (non-adiabatic g−) modes. Those modes are responsible for the light and velocity variations of β Cephei stars, slowly pulsating B (SPB) stars, and α Cyg variables. The instability mechanisms for these pulsations are discussed. We also discuss the relation between the evolution of massive stars and the excitation of strange modes, which are considered responsible for the pulsation in most of the α Cyg variables. The surface He and CNO abundances of hotter α Cyg variables seem to indicate that the Ledoux criterion of convection is better than the Schwarzschild criterion, although the latter is extensively used in stellar evolution computations.

Keywords

massive starspulsationinstabilitymixing
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 11 , General Assembly A29B: Astronomy in Focus , August 2015 , pp. 573 - 580
Copyright
Copyright © International Astronomical Union 2016 

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