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• W2129783387 startingPage "835" @default.
• W2129783387 abstract "The model of anisotropic loss of the mass and angular momentum is constructed and the non-conservative evolution of the binary system is investigated in this paper. The joint effects of the centrifugal force and tidal force cause the configurations of two components to become triaxial ellipsoids. The high-order disturbing potential, which includes the rotational and tidal distortions, is applied to describe the local gravity in a close binary system. The |$g_{rm eff}$|(⁠|$theta$|⁠, |$varphi$|⁠)-effect dominates the mass-loss distribution in the massive O-type star. Both the |$g_{rm eff}$|(⁠|$theta$|⁠, |$varphi$|⁠)-effect and the |$kappa$|-effect have an important influence on the equatorial ejection, and the Roche lobe overflow and the H-shell burning occur earlier in the rotational models. The rotation and tide can intensify the mass loss before mass overflow, and the rate of stellar wind goes down, resulting from a decrease of the luminosity in the subsequent stages. The high-order disturbing potential and other associated physical factors may significantly affect the Roche lobe and might be possible to drive the non-conservative mass transfer process when the stars approach the break-up rotation. Rotation and tide can allow the primary to shift towards the blue side of the HR diagram and modify the thermal relaxation time-scale in the slow phase of the mass transfer in Case A. The star attempts to attain thermal equilibrium and displays a slightly cyclical expansion and contraction. When stellar wind was taken into consideration in the model, the secondary star accreted less mass than the model without stellar wind." @default.
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• W2129783387 date "2011-08-25" @default.
• W2129783387 modified "2023-10-16" @default.
• W2129783387 title "Wind Anisotropy and Angular Momentum Loss in a Massive Rotating Binary System" @default.
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• W2129783387 doi "https://doi.org/10.1093/pasj/63.4.835" @default.
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