Mixing coefficients as a function of enclosed mass fraction for a 5 M_⊙ main-sequence star at solar metallicity, with an initial rotation rate set to 20 percent of the critical surface rotation rate. Shown are contributions from convection, convective overshoot, and rotationally- induced hydrodynamical instabilities, namely: Eddington–Sweet circulation (ES), Solberg–Høiland instability (SH), Goldreich–Schubert–Fricke instability (GSF), dynamical shear instability (DSI), and secular shear instability (SSI).