  The interaction between equilibrium tides and convection in stellar envelopes
is often considered important for tidal evolution in close binary and
extrasolar planetary systems. Its efficiency for fast tides has however long
been controversial, when the tidal frequency exceeds the turnover frequency of
convective eddies. Recent numerical simulations indicate that convection can
act like an effective viscosity which decays quadratically with tidal frequency
for fast tides, resulting in inefficient dissipation in many applications
involving pre- and main-sequence stars and giant planets. A new idea was
however recently proposed by Terquem (2021), who suggested Reynolds stresses
involving correlations between tidal flow components dominate the interaction
instead of correlations between convective flow components as usually assumed.
They further showed that this can potentially significantly enhance tidal
dissipation for fast tides in many applications. Motivated by the importance of
this problem for tidal dissipation in stars and planets, we directly compute
this new term using analytical arguments and global spherical simulations using
Boussinesq and anelastic hydrodynamic models. We demonstrate that the new term
proposed by Terquem vanishes identically for equilibrium tides interacting with
convection in both Boussinesq and anelastic models; it is therefore unlikely to
contribute to tidal dissipation in stars and planets.
