On non-radial oscillations of B-type stars

Details On non-radial oscillations of B-type stars On non-radial oscillations of B-type stars

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.262..213g&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 262, no. 1, p. 213-219.

Statistics

Computation

89

B Stars, Stellar Interiors, Stellar Oscillations, Variable Stars, Hertzsprung-Russell Diagram, Nonstabilized Oscillation, Stellar Evolution, Stellar Models

Scientific paper

The excitation mechanisms behind the slow pulsations - with periods of the order of one day - of OB stars are discussed on the basis of numerical computations. Nonradial, non-adiabatic stability analysis is performed on a set of evolutionary models with masses between 5.2 and 12.1 solar masses. The long-period oscillations in stellar models below the newly recovered Beta Cephei region are found to be excited by the iron bump in the newly available OPAL opacities. For more massive stars exhibiting oscillations with periods of the order of one day, however, another excitation mechanism must be sought.

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