On the rotational modes of fully convective stars with application to close binary systems

Details On the rotational modes of fully convective stars with application to close binary systems On the rotational modes of fully convective stars with application to close binary systems

Jun 1981

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1981mnras.195..743p&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 195, June 1981, p. 743-753.

Astronomy and Astrophysics

Astrophysics

21

Astrophysics, Binary Stars, Stellar Rotation, Apsides, Circular Orbits, Eigenvalues, Modal Response, Toroids

Scientific paper

The purely rotational toroidal modes are calculated for an n = 1.5 polytrope. There are no g modes in this stellar model, so that in the slowly rotating case, a single low frequency spectrum is expected, which corresponds to the toroidal modes and is free from the complications of interactions with g modes, as well as the usual high frequency p and f mode spectrum. The eigenvalue problem for the toroidal modes for the case of slow uniform rotation is formulated and solved for some of the eigenmodes for m = 2, where m is the usual azimuthal mode number, using a numerical method based on a variational technique applied to the eigenvalue problem. Results are applied to the apsidal motion problem and the circularization problem in close binary systems, with particular reference to the SU UMa subclass of the cataclysmic binaries, in which such modes are liable to be excited if there is a small eccentricity in the system. Possible consequences of resonance between the orbital motion and a pulsation period are evaluated.

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