Astronomy and Astrophysics – Astronomy
Scientific paper
Aug 2001
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001apj...557..311l&link_type=abstract
The Astrophysical Journal, Volume 557, Issue 1, pp. 311-319.
Astronomy and Astrophysics
Astronomy
15
Instabilities, Stars: Oscillations, Stars: Rotation
Scientific paper
Low-frequency g-modes excited by the opacity bump mechanism in main-sequence stars with the masses M~4 Msolar are believed to be responsible for the periodic variability observed in slowly pulsating B (SPB) stars. We calculate fully nonadiabatic g-modes with a low-degree l in an SPB star model to examine the pulsational stability by taking into account the effects of the Coriolis force and assuming a uniform rotation. We find that the slow rotation of the star contributes to the excitation of the high radial order retrograde g-modes with low l. This contribution to the excitation is most significant for the g-modes with l=1. At rapid rotation, many g-modes with low l in the model are found to be pulsationally unstable even in the inertial regime in which |ω|<2Ω, where ω denotes the oscillation frequency observed in the corotating frame and Ω is the angular rotation frequency. As the rotation rate increases, mode coupling caused by the Coriolis force between g-modes with different values of l becomes influential on the pulsational stability. We find that some of the g-modes in the inertial regime are stabilized by mode coupling at rapid rotation and that this stabilization effect is most significant for the retrograde g-modes with l>|m|.
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