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Title:
Surface trapping and leakage of low-frequency g modes in rotating early-type stars - II. Global analysis
Authors:
Townsend, R. H. D.
Affiliation:
AA(Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 319, Issue 1, pp. 289-304. (MNRAS Homepage)
Publication Date:
11/2000
Origin:
MNRAS
MNRAS Keywords:
WAVES, STARS: EARLY-TYPE, STARS: EMISSION-LINE, BE, STARS: OSCILLATIONS, STARS: ROTATION
DOI:
10.1046/j.1365-8711.2000.03853.x
Bibliographic Code:
2000MNRAS.319..289T

Abstract

A global analysis of the surface trapping of low-frequency non-radial g modes in rotating early-type stars is undertaken within the Cowling, adiabatic and traditional approximations. The dimensionless pulsation equations governing these modes are reviewed, and the boundary conditions necessary for solution of the equations are considered; in particular, an outer mechanical boundary condition, which does not enforce complete wave trapping at the stellar surface, is derived and discussed in detail. The pulsation equations are solved for a 7-Msolar model star over a range of rotation rates, using a numerical approach. The results of the calculations confirm the findings of the preceding paper in the series: modes with eigenfrequencies below a cut-off cannot be fully trapped within the star, and exhibit leakage in the form of outwardly propagating waves at the surface. The damping rates resulting from leakage are calculated for such `virtual' modes, and found to be appreciably larger than typical growth rates associated with opacity-driven pulsation. Furthermore, it is demonstrated that the surface perturbations generated by virtual modes are significantly changed from those caused by fully trapped modes; the latter result suggests differences in the line-profile variations exhibited by these two types of mode. The findings are discussed in the context of the 53 Per, SPB and pulsating Be classes of variable star. Whilst wave leakage will probably not occur for overstable g modes in the 53 Per and slowly rotating SPB stars, the adoption of the new outer mechanical boundary condition may still affect the pulsational stability of these systems. Wave leakage for overstable modes remains a possibility in Be stars and the more rapidly rotating SPB stars.

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