We calculate tidally driven mean flows in a slowly and uniformly rotating massive main sequence star in a binary system .
We treat the tidal potential due to the companion as a small perturbation to the primary star .
We compute tidal responses of the primary as forced linear oscillations , as a function of the tidal forcing frequency \omega _ { tide } = 2 ( \Omega _ { orb } - \Omega ) , where \Omega _ { orb } is the mean orbital angular velocity and \Omega is the angular velocity of rotation of the primary star .
The amplitude of the tidal responses is proportional to the parameter f _ { 0 } \propto ( M _ { 2 } / M ) ( a _ { orb } / R ) ^ { -3 } , where M and M _ { 2 } are the masses of the primary and companion stars , R is the radius of the primary and a _ { orb } is the mean orbital separation between the stars .
For a given f _ { 0 } , the amplitudes depend on \omega _ { tide } and become large when \omega _ { tide } is in resonance with natural frequencies of the star .
Using the tidal responses , we calculate axisymmetric mean flows , assuming that the mean flows are non-oscillatory flows driven via non-linear effects of linear tidal responses .
We find that the \phi -component of the mean flow velocity dominates .
We also find that the amplitudes of the mean flows are large only in the surface layers where non-adiabatic effects are significant and that the amplitudes are confined to the equatorial regions of the star .
Depending on M _ { 2 } / M and a _ { orb } / R , the amplitudes of mean flows at the surface become significant .