  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.
