  Jupiter's atmosphere comprises several dynamical regimes: the equatorial
eastward flows and surrounding retrograde jets; the midlatitudes, with the
eddy-driven, alternating jet-streams and meridional circulation cells; and the
jet-free turbulent polar region. Despite intensive research conducted on each
of these dynamical regimes over the past decades, they remain only partially
understood. Saturn's atmosphere also encompasses similar distinguishable
regimes, but observational evidence for midlatitude deep meridional cells is
lacking. Models offer a variety of explanations for each of these regions, but
only a few are capable of simulating more than one of the regimes at once. This
study presents new numerical simulations using a 3D deep anelastic model that
can reproduce the equatorial flows as well as the midlatitudinal pattern of the
mostly barotropic, alternating eddy-driven jets and the meridional circulation
cells accompanying them. These simulations are consistent with recent Juno
mission gravity and microwave data. We find that the vertical eddy momentum
fluxes are as important as the meridional eddy momentum fluxes, which drive the
midlatitudinal circulation on Earth. In addition, we discuss the parameters
controlling the number of midlatitudinal jets/cells, their extent, strength,
and location. We identify the strong relationship between meridional
circulation and the zonal jets in a deep convection setup, and analyze the
mechanism responsible for their generation and maintenance. The analysis
presented here provides another step in the ongoing pursuit of understanding
the deep atmospheres of gas giants.
