Volume 443, Number 2, November IV 2005
|Page(s)||557 - 570|
|Section||Stellar structure and evolution|
|Published online||04 November 2005|
Unstable quasi g-modes in rotating main-sequence stars
Astronomical Institute “Anton Pannekoek”, University of Amsterdam, Kruislaan 403, 1098 SJ Amsterdam, The Netherlands e-mail: email@example.com
Accepted: 18 June 2005
This paper studies the oscillatory stability of uniformly rotating main-sequence stars of mass 3-8 by solving the linearized non-adiabatic, non-radial oscillation equations with a forcing term and searching for resonant response to a complex forcing frequency. By using the traditional approximation, the solution of the forced oscillation equations becomes separable, whereby the energy equation is made separable by approximation. It is found that the κ-mechanism in rotating B-stars can destabilize not only gravity- or pressure modes, but also a branch of low frequency retrograde (in corotating frame) oscillations in between the retrograde g-modes and toroidal r-modes. These unstable quasi-g (or “q-modes”) hardly exhibit rotational confinement to the equatorial regions of the star, while the oscillations are always prograde in the observer's frame, all in contrast to g-modes. The unstable q-modes occur in a few narrow period bands (defined by their azimuthal index m) and seem to fit the oscillation spectra observed in SPB stars rather well. The unstable q-mode oscillation spectrum of a very rapidly rotating 8 star appears similar to that of the well-studied Be-star μ Cen. The unstable q-modes thus seem far better for explaining the observed oscillation spectra in SPB-stars and Be-stars than do normal g-modes.
Key words: stars: rotation / stars: oscillations
© ESO, 2005
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