What tides and flares do to RS Canum Venaticorum binaries

Abstract

view Abstract Citations (55) References (25) Co-Reads Similar Papers Volume Content Graphics Metrics Export Citation NASA/ADS What tides and flares do to RS Canum Venaticorum binaries. Decampli, W. M. ; Baliunas, S. L. Abstract 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. Publication: The Astrophysical Journal Pub Date: June 1979 DOI: 10.1086/157140 Bibcode: 1979ApJ...230..815D Keywords: Eclipsing Binary Stars; Flare Stars; Stellar Mass Ejection; Tides; Angular Momentum; Light Curve; Stellar Magnetic Fields; X Ray Absorption; Astrophysics; Mass Loss:RS CVn Stars; Period Changes:RS CVn Stars; RS CVn Stars:Stellar Flares full text sources ADS | data products SIMBAD (7)