The stability of massive main-sequence stars

Details The stability of massive main-sequence stars The stability of massive main-sequence stars

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.262...85g&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 262, no. 1, p. 85-92.

Astronomy and Astrophysics

Astronomy

42

Dynamic Stability, Main Sequence Stars, Stellar Interiors, Stellar Oscillations, Boundary Conditions, Critical Mass, Eigenvectors, Nonadiabatic Conditions, Stellar Models

Scientific paper

The stability of massive main-sequence stars with respect to radial perturbations is re-examined using recently provided opacity tables. Three types of instability are identified: (1) dynamical instabilities associated with the occurrence of strange modes; (2) instability of the first overtone caused by the kappa-mechanism; and (3) instability of the fundamental mode due to a mixture of the kappa- and epsilon-mechanisms. Critical masses as a function of metallicity are determined for the various instabilities. With respect to both range and strength, instabilities driven by the kappa- and epsilon-mechanisms are negligible when compared with strange-mode instabilities.

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