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Binary evolution models with rotation
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We discuss the first available binary evolution models which include up-to-date rotational physics for both components, as well as angular momentum accretion and spin-orbit coupling. These models allow a self-consistent computation of the mass transfer efficiency during Roche-lobe overflow phases, and a determination of the transition from quasi-conservative to non-conservative evolution. Applications to massive binary systems lead to predictions for the spin rates of compact objects in binaries, and for the occurrence of gamma-ray bursts from collapsars in binaries. Rotational effects in accreting white dwarfs are found to stabilise the shell burning and decrease the carbon abundance in progenitor models for Chandrasekhar-mass Type Ia supernovae, and to potentially avoid a detonation of the white dwarf within the sub-Chandrasekhar mass scenario.
Forward citations
Cited by 2 Pith papers
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You're Gonna Need a Bigger Core: Calibrating Massive Star Models against Galactic OB-type Stars
Galactic OB-star HR-diagram data imply a constant core overshoot α_ov ≈ 0.33 for 12–40 M_sun, yielding larger helium cores than standard prescriptions.
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Binary stars take what they get: Evidence for Efficient Mass Transfer from Stripped Stars with Rapidly Rotating Companions
Analysis of 16 Be+sdOB binaries shows that most transferred mass is retained by the accretor, with half of the systems requiring efficiencies above 50%.
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