Stellar stability in close binary systems

Details Stellar stability in close binary systems Stellar stability in close binary systems

Aug 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975mnras.172..339p&link_type=abstract

Monthly Notices of the Royal Astronomical Society, vol. 172, Aug. 1975, p. 339-357. Research supported by the Science Research

Astronomy and Astrophysics

Astronomy

51

Astronomical Models, Binary Stars, Dynamic Stability, Roche Limit, Stellar Structure, Adiabatic Conditions, Convective Flow, Orbital Mechanics, Stellar Atmospheres

Scientific paper

The linear adiabatic stability of stars in close binary systems is discussed. Both spherical and Roche geometries are considered. Two destabilizing influences are shown to exist. These are related to previously discussed instability mechanisms. Examination of the stability of models nearly filling the critical equipotential shows that the boundary condition used by Bath (1972) is the most appropriate one to use in the spherical case. Detailed Roche models are constructed, and their stability properties determined. It is concluded that dynamical instabilities may be important in dwarf novae, slow novae, and the binary symbiotic stars.

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