  In close two-body astrophysical systems, such as binary stars or Hot Jupiter
systems, tidal interactions often drive dynamical evolution on secular
timescales. Many host stars and presumably giant gaseous planets feature a
convective envelope. Tidal flows generated therein by the tidal potential of
the companion can be dissipated through viscous friction, leading to the
redistribution and exchange of angular momentum within the convective shell and
with the companion, respectively. In the tightest systems, nonlinear effects
are likely to have a significant impact on the tidal dissipation and trigger
differential rotation in the form of zonal flows, as has been shown in previous
studies. In this context, we investigate how the addition of nonlinearities
affect the tidal flow properties, and energy and angular momentum balances,
using 3D nonlinear simulations of an adiabatic and incompressible convective
shell. In our study, we have chosen a body forcing where the equilibrium tide
(the quasi-hydrostatic tidal flow component) acts via an effective forcing to
excite tidal inertial waves in a spherical shell. Within this set-up, we show
new results for the amplitude of the energy stored in zonal flows, angular
momentum evolution, and its consequences on tidal dissipation in the envelopes
of low-mass stars and giant gaseous planets.
