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We calculate tidally driven mean flows in a slowly and uniformly rotatingmassive main sequence star in a binary system. We treat the tidal potential dueto the companion as a small perturbation to the primary star. We compute tidalresponses of the primary as forced linear oscillations, as a function of thetidal forcing frequency $\omega_{\rm tide}=2(\Omega_{\rm orb}-\Omega)$, where$\Omega_{\rm orb}$ is the mean orbital angular velocity and $\Omega$ is theangular velocity of rotation of the primary star. The amplitude of the tidalresponses is proportional to the parameter $f_0\propto (M_2/M)(a_{\rmorb}/R)^{-3}$, where $M$ and $M_2$ are the masses of the primary and companionstars, $R$ is the radius of the primary and $a_{\rm orb}$ is the mean orbitalseparation between the stars. For a given $f_0$, the amplitudes depend on$\omega_{\rm tide}$ and become large when $\omega_{\rm tide}$ is in resonancewith natural frequencies of the star. Using the tidal responses, we calculateaxisymmetric mean flows, assuming that the mean flows are non-oscillatory flowsdriven via non-linear effects of linear tidal responses. We find that the$\phi$-component of the mean flow velocity dominates. We also find that theamplitudes of the mean flows are large only in the surface layers wherenon-adiabatic effects are significant and that the amplitudes are confined tothe equatorial regions of the star. Depending on $M_2/M$ and $a_{\rm orb}/R$,the amplitudes of mean flows at the surface become significant.

Tidally driven mean flows in slowly and uniformly rotating massive main sequence stars