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Turbulent convection is thought to act as an effective viscosity ($\nu_E$) indamping tidal flows in stars and giant planets. However, the efficiency of thismechanism has long been debated, particularly in the regime of fast tides, whenthe tidal frequency ($\omega$) exceeds the turnover frequency of the dominantconvective eddies ($\omega_c$). We present the results of hydrodynamicalsimulations to study the interaction between tidal flows and convection in asmall patch of a convection zone. These simulations build upon our prior workby simulating more turbulent convection in larger horizontal boxes, and here weexplore a wider range of parameters. We obtain several new results: 1) $\nu_E$is frequency-dependent, scaling as $\omega^{-0.5}$ when $\omega/\omega_c\lesssim 1$, and appears to attain its maximum constant value only for verysmall frequencies ($\omega/\omega_c \lesssim 10^{-2}$). Thisfrequency-reduction for low frequency tidal forcing has never been observedpreviously. 2) The frequency-dependence of $\nu_E$ appears to follow the samescaling as the frequency spectrum of the energy (or Reynolds stress) for lowand intermediate frequencies. 3) For high frequencies ($\omega/\omega_c\gtrsim1-5$), $\nu_E\propto \omega^{-2}$. 4) The energetically-dominant convectivemodes always appear to contribute the most to $\nu_E$, rather than the resonanteddies in a Kolmogorov cascade. These results have important implications fortidal dissipation in convection zones of stars and planets, and indicate thatthe classical tidal theory of the equilibrium tide in stars and giant planetsshould be revisited. We briefly touch upon the implications for planetaryorbital decay around evolving stars.

Convective turbulent viscosity acting on equilibrium tidal flows: new frequency scaling of the effective viscosity