Activity-driven structure variations as a cause of period changes in RS Canis Venaticorum-like systems

Details Activity-driven structure variations as a cause of period changes in RS Canis Venaticorum-like systems Activity-driven structure variations as a cause of period changes in RS Canis Venaticorum-like systems

Aug 1985

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1985apj...295l..39v&link_type=abstract

Astrophysical Journal, Part 2 - Letters to the Editor (ISSN 0004-637X), vol. 295, Aug. 15, 1985, p. L39-L42.

Astronomy and Astrophysics

Astrophysics

28

Binary Stars, Magnetic Stars, Stellar Activity, Stellar Rotation, Convection, Mass Transfer, Periodic Variations, Stellar Orbits, Stellar Structure

Scientific paper

Magnetic activity cycles of a convective star in a close binary system may lead to orbit period changes through tidal spin-orbit coupling. An increase in the mean magnetic field throughout the convection zone provides an additional pressure support and increases the star's moment of inertia. In order for the system to conserve angular momentum instantaneously, the convective star must reduce its rotation rate. When this happens, the system is no longer synchronous; in particular, the equilibrium tide now suffers a phase lag. A tidal torque must act, transferring angular momentum from the star's rotation to the orbit, lengthening the period. When the field decays, these events reverse and the period shortens. Observed period changes in RS CVn-like systems are of the order delta p/p = 10 to the -6th, implying variations in the mean field strength at the base of the convection zone of approximately 1000 G over time scales of 10-30 yr. It is predicted that the strength of magnetic activity indicators will track orbital period changes in a given system: the period will be largest during the active portion of the magnetic cycle and smallest during the quiescent part.

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