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Title:
Kappa-mechanism excitation of retrograde mixed modes in rotating B-type stars
Authors:
Townsend, R. H. D.
Affiliation:
AA(Bartol Research Institute, University of Delaware, Newark, DE 19716, USA; Department of Physics & Astronomy, University College London, Gower Street, London WC1E 6BT)
Publication:
Monthly Notices of the Royal Astronomical Society, Volume 364, Issue 2, pp. 573-582. (MNRAS Homepage)
Publication Date:
12/2005
Origin:
MNRAS
MNRAS Keywords:
instabilities, stars: early-type, stars: emission-line, Be, stars: oscillations, stars: rotation, stars: variables: other
DOI:
10.1111/j.1365-2966.2005.09585.x
Bibliographic Code:
2005MNRAS.364..573T

Abstract

I examine the stability of retrograde mixed modes in rotating B-type stars. These modes can be regarded as a hybrid between the Rossby modes that arise from conservation of vorticity, and the Poincaré modes that are gravity waves modified by the Coriolis force. Using a non-adiabatic pulsation code based around the traditional approximation, I find that the modes are unstable in mid- to late-B-type stars, as a result of the same iron-bump opacity mechanism that is usually associated with SPB and β Cep stars. At one-half of the critical rotation rate, the instability for the modes with azimuthal orders m= 1 to 4spans the spectral types B4 to A0. Inertial-frame periods of the unstable modes range from 100 days down to a fraction of a day, while normalized growth rates can reach in excess of 10-5.

I discuss the relevance of these findings to SPB and pulsating Be stars, and to the putative Maia class of variable star. I also outline some of the questions raised by this discovery of a wholly new class of pulsational instability in early-type stars.

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