What tides and flares do to RS Canum Venaticorum binaries

Details What tides and flares do to RS Canum Venaticorum binaries What tides and flares do to RS Canum Venaticorum binaries

Jun 1979

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1979apj...230..815d&link_type=abstract

Astrophysical Journal, Part 1, vol. 230, June 15, 1979, p. 815-821.

Astronomy and Astrophysics

Astrophysics

47

Eclipsing Binary Stars, Flare Stars, Stellar Mass Ejection, Tides, Angular Momentum, Light Curve, Stellar Magnetic Fields, X Ray Absorption

Scientific paper

The effects that anisotropic mass should have on the orbital and spin states of RS Canum Venaticorum binaries are discussed. In the absence of magnetic fields, orbital period changes reported for several RS Canum Venaticorum systems require dM/dt of about 0.000001 solar masses/yr. Magnetic braking can lower this required rate if the surface magnetic fields are not less than 1000 gauss. However, this requires a method much more powerful than tidal torques to convert spin angular momentum loss to orbital angular momentum loss. This possibility is important when interpreting the complicated light curves of these systems, and may contradict the Hall's 'drifting star spot' hypothesis. In addition, large mass-loss rates may result in significant self-absorption of quiescent soft X-rays observed from several of these binaries.

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