  We present a computationally efficient 1-D seasonal radiative model, with
convective adjustment, of Jupiter's atmosphere. Our model takes into account
radiative forcings from the main hydrocarbons (methane, ethane, acetylene),
ammonia, collision-induced absorption, four cloud and haze layers (including a
UV-absorbing "polar" stratospheric haze) and an internal heat flux. We detail
sensitivity studies of the equilibrium temperature profile to several
parameters. We discuss the expected seasonal, vertical and meridional thermal
structure and compare it to that derived from Cassini and ground-based thermal
infrared observations. We find that the equilibrium temperature in the 5-30
mbar pressure range is very sensitive to the chosen stratospheric haze optical
properties, sizes and number of monomers. The polar haze can significantly warm
the lower stratosphere (10-30 mbar) by up to 20K at latitudes 45-60{\deg}. At
pressures lower than 3 mbar, our modeled temperatures systematically
underestimate the observed ones by 5K. This might suggest that other processes,
such as dynamical heating by wave breaking or by eddies, or a coupling with
thermospheric circulation, play an important role. In the troposphere, we can
only match the observed lack of meridional gradient of temperature by varying
the internal heat flux with latitude. We then exploit knowledge of heating and
cooling rates to diagnose the residual-mean circulation in Jupiter's
stratosphere, under the assumption that the eddy heat flux convergence term is
negligible. In the lower stratosphere (5-30 mbar), the residual-mean
circulation strongly depends on the assumed properties of the stratospheric
haze. Our main conclusion is that it is crucial to improve our knowledge on the
radiative forcing terms to increase our confidence in the estimated
circulation. By extension, this will also be crucial for future 3D GCM studies.
