Recent ( 2011 ) results from the Nice Observatory indicate the existence of global seismic modes on Jupiter in the frequency range between 0.7 and 1.5mHz with amplitudes of tens of cm/s .
Currently , the driving force behind these modes is a mystery ; the measured amplitudes are many orders of magnitude larger than anticipated based on theory analogous to helioseismology ( that is , turbulent convection as a source of stochastic excitation ) .
One of the most promising hypotheses is that these modes are driven by Jovian storms .
This work constructs a framework to analytically model the expected equilibrium normal mode amplitudes arising from convective columns in storms .
We also place rough constraints on Jupiter ’ s seismic modal quality factor .
Using this model , neither meteor strikes , turbulent convection , nor water storms can feasibly excite the order of magnitude of observed amplitudes .
Next we speculate about the potential role of rock storms deeper in Jupiter ’ s atmosphere , because the rock storms ’ expected energy scales make them promising candidates to be the chief source of excitation for Jovian seismic modes , based on simple scaling arguments .
We also suggest some general trends in the expected partition of energy between different frequency modes .
Finally we supply some commentary on potential applications to gravity , Juno , Cassini and Saturn , and future missions to Uranus and Neptune .