The opacity mechanism in B-type stars. I - Unstable modes in Beta Cephei star models

Details The opacity mechanism in B-type stars. I - Unstable modes in Beta Cephei star models The opacity mechanism in B-type stars. I - Unstable modes in Beta Cephei star models

May 1993

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993mnras.262..204d&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 262, no. 1, p. 204-212.

Astronomy and Astrophysics

Astronomy

134

B Stars, Main Sequence Stars, Metallicity, Nonstabilized Oscillation, Stellar Oscillations, Supergiant Stars, Opacity, Stellar Evolution, Stellar Models

Scientific paper

A stability survey for models of 7- to 16-solar-mass stars in the main-sequence (MS) and early post-MS evolutionary phases is presented on the basis of an improved version of the OPAL capacities, with the metal abundance parameter Z having values of 0.02 and 0.03. For most of the Beta Cep objects, a value of Z = 0.02 suffices to account for the pulsational instability. The fundamental radial mode, p1, is unstable in all sequences of stellar models considered, except the one with M = 7 solar masses and Z = 0.02. Instability of the overtones, up to p3 for Z = 0.03, appears with mass increase. Nonradial modes of low degrees are unstable in a wider frequency range encompassing low-order g-modes. All of these modes may be associated with the Beta Cep phenomenon. For higher spherical harmonic degrees, there is a domain of high-order g-mode instability. Excitation of such modes may be responsible for long-period variability of line profiles observed in some B-type stars.

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