Kelvin-Helmholtz instabilities and their application to B-type variables

Details Kelvin-Helmholtz instabilities and their application to B-type variables Kelvin-Helmholtz instabilities and their application to B-type variables

Dec 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.197.1139a&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 197, Dec. 1981, p. 1139-1152. Research supported by the Yamada Science

Astronomy and Astrophysics

Astronomy

22

B Stars, Kelvin-Helmholtz Instability, Stellar Rotation, Variable Stars, Boussinesq Approximation, Flow Equations, Magnetohydrodynamic Flow, Periodic Variations, Stellar Envelopes, Stellar Evolution, Stellar Structure

Scientific paper

A Kelvin-Helmholtz instability, formed from the differential rotation in the narrow region between the core and envelope, is proposed as a promising mechanism responsible for the excitation of pulsations in B-type variables (53 Per variables and Beta Cep stars), in which the unstable inertia wave resulting from this instability resonates with an eigenmode of the nonradial oscillation of the whole star. The degeneracy of the two frequencies is found to be expected at any evolutionary stage of a star. The equations for a Kelvin-Helmholtz instability have been formulated for the stellar case, and in the cylindrical configuration limit, the necessary condition for instability and characteristics of the instability have been discussed. The back reaction of the excited modes on the differential rotation is discussed in these stars, and it is pointed out that the differential rotation can be significantly affected by this effect in a short time.

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