The possibility of non-synchronism of convective secondaries in close binary stars

Details The possibility of non-synchronism of convective secondaries in close binary stars The possibility of non-synchronism of convective secondaries in close binary stars

Aug 1983

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1983mnras.204..433c&link_type=abstract

Monthly Notices of the Royal Astronomical Society (ISSN 0035-8711), vol. 204, Aug. 1983, p. 433-447. Research supported by the S

Astronomy and Astrophysics

Astronomy

42

Binary Stars, Mass Transfer, Stellar Rotation, Synchronism, Tides, Velocity Distribution, Viscosity

Scientific paper

The authors calculate the non-synchronous velocity field of a low mass convective secondary in a close binary system, taking rotation into account. They find that, contrary to previous belief, the velocity tends to zero as the L1 point is approached. They also find that the use of tidal lobes is inappropriate when the secondary is asynchronous. They consider the action of a turbulent viscosity on the velocity field and find that, when convection is inefficient, synchronization times can approach the lifetime of the system.

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