  Turbulent friction in convective regions in stars and planets is one of the
key physical mechanisms that drive the dissipation of the kinetic energy of
tidal flows in their interiors and the evolution of their systems. This
friction acts both on the equilibrium/non-wave like tide and on tidal inertial
waves in these layers. It is thus necessary to obtain a robust prescription for
this friction. In the current state-of-the-art, it is modeled by a turbulent
eddy-viscosity coefficient, based on mixing-length theory, applied on
velocities of tides. However, none of the current prescriptions take into
account the action of rotation that can strongly affects turbulent convection.
Therefore, we use theoretical scaling laws for convective velocities and
characteristic lengthscales in rotating stars and planets that have been
recently confirmed by 3-D high-resolution nonlinear Cartesian numerical
simulations to derive a new prescription. A corresponding local model of tidal
waves is used to understand the consequences for the linear tidal dissipation.
Finally, new grids of rotating stellar models and published values of planetary
convective Rossby numbers are used to discuss astrophysical consequences. The
action of rotation on convection deeply modifies the turbulent friction applied
on tides. In the regime of rapid rotation (with a convective Rossby number
below 0.25), the eddy-viscosity may be decreased by several ordres of
magnitude. It may lead to a loss of efficiency of the viscous dissipation of
the equilibrium tide and to a more efficient complex and resonant dissipation
of tidal inertial waves in the bulk of convective regions. Therefore, it is
necessary to have a completely coupled treatment of the tidal/rotational
evolution of star-planet systems and multiple stars with a coherent treatment
of the variations of tidal flows and of their dissipation as a function of
rotation.
