The Evolution of the Period and Synchronization for Close G-Type MS Binaries
We give some preliminary computations of the variation of the synchronization parameter f = P K /P and the orbital period P K with time for late type close binaries. Angular momentum loss by stellar wind from the components and angular momentum transfer due to the torque exerted by the tidal bulge are both taken into account. The uncertainties introduced by the treatment of the equilibrium tide and the estimation of the angular momentum loss are discussed. It is argued that the expected non-homogeneous rotation of the components has only a negligible effect on the results of the computations
KeywordsOrbital Period Stellar Wind Inertial Moment Close Binary Convective Envelope
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- 3.Linnell,A.P.: 1980, 2nd Cambridge workshop on cool stars, stellar systems and the sun, t.2, eds. M.S.Giampapa, L.Golub p. 65Google Scholar