  Recent observations of Jupiter have suggested the existence of global
oscillatory modes at millihertz frequencies, yet the source mechanism
responsible for driving these modes is still unknown. However, the energies
necessary to produce observable surface oscillations have been predicted. Here
we investigate if moist convection in Jupiter's upper atmosphere can be
responsible for driving the global oscillations and what moist convective
energy requirements are necessary to achieve these theoretical mode energies
and surface amplitudes. We begin by creating a one-dimensional moist convective
cloud model and find that the available kinetic energy of the rising cloud
column falls below theoretical estimates of oscillations energies. That is,
mode excitation cannot occur with a single storm eruption. We then explore
stochastic excitation scenarios of the oscillations by moist convective storms.
We find that mode energies and amplitudes can reach theoretical estimates if
the storm energy available to the modes is more than just kinetic. In order for
the modes to be excited, we find that they require $5 \times 10^{27}$ to
10$^{28}$ erg per day. However, even for a large storm eruption each day, the
available kinetic energy from the storms falls two orders of magnitude short of
the required driving energy. Although our models may oversimplify the true
complexity of the coupling between Jovian storms and global oscillations, our
findings reveal that enough thermal energy is associated with moist convection
to drive the modes, should it be available to them.

Earth and Planetary Astrophysics