Other
Scientific paper
Nov 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001mnras.327..881d&link_type=abstract
Monthly Notices of the Royal Astronomical Society, Volume 327, Issue 3, pp. 881-887.
Other
12
Stars: Early-Type, Hertzsprung-Russell (Hr) Diagram, Stars: Oscillations, Stars: Variables: Other
Scientific paper
We carried out a series of linear stability analyses of the radial and low-degree non-radial p modes for stellar models with initial masses of 6-30Msolar. The stellar models were computed by using convective overshoot distance dover=0.10, 0.25 and 0.40HP. Our numerical results show that the β Cephei instability strip forms a horn-shaped region pointing upwards near the main sequence on the Hertzsprung-Russell diagram (HRD). The lower part of the instability strip for the radial modes join the zero-age main-sequence (ZAMS) at M~8.0-10.5Msolar, while the top of the instability strip extends up to M~15.5Msolar. The instability strip for the non-radial modes is even wider. The overall instability strip is dominated by the radial and non-radial fundamental modes. The first overtone (the radial-order index n=1) is also pulsationally unstable. We have shown that the β Cephei stability is almost independent of the overshoot parameter dover used for the stellar models, while it depends critically on the metal abundance. With decreasing metal abundance, the instability region shrinks and eventually disappears for Z<~0.005.
Deng Licai
Xiong Da-Run
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