Non-radial oscillations of rotating stars and their relevance to the short-period oscillations of cataclysmic variables

Details Non-radial oscillations of rotating stars and their relevance to the short-period oscillations of cataclysmic variables Non-radial oscillations of rotating stars and their relevance to the short-period oscillations of cataclysmic variables

Feb 1978

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1978mnras.182..423p&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 182, Feb. 1978, p. 423-442. Research supported by the IBM Corp.

Statistics

Applications

233

Coherent Radiation, Stellar Rotation, Variable Stars, White Dwarf Stars, Binary Stars, Gravitational Effects, Kelvin-Helmholtz Instability, Stellar Envelopes, Stellar Mass Accretion, Tides

Scientific paper

The standard analysis of nonradial oscillations in particular g modes of a slowly rotating or nonrotating white dwarf is briefly reviewed. A theory of nonradial low-frequency modes of a rotating white dwarf is developed, existing theories are summarized, and the standard g-mode hypothesis is critically evaluated. It is argued that this hypothesis is untenable in its present form mainly because of difficulties in accounting for the size and variation of observed periods. Some modifications are suggested, but it is shown that estimated accretion rates for binary systems containing white dwarfs invalidate the slow-rotation hypothesis on which the previous g-mode theory is based. Nonradial oscillations of rotating white dwarfs are found to be capable of accounting for the observed oscillations in dwarf novae. Applications of the results to rotating stars, Beta Cephei stars, and effects of tidal interaction in binary systems are discussed.

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