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The Ice Giants Uranus and Neptune have hydrogen-based atmospheres withseveral constituents that condense in their cold upper atmospheres. A smallnumber of bright cloud systems observed in both planets are good candidates formoist convective storms, but their observed properties (size, temporal scalesand cycles of activity) differ from moist convective storms in the Gas Giants.These clouds and storms are possibly due to methane condensation andobservations also suggest deeper clouds of hydrogen sulfide (H$_2$S) at depthsof a few bars. Even deeper, thermochemical models predict clouds of ammoniahydrosulfide (NH$_4$SH) and water at pressures of tens to hundreds of bars,forming extended deep weather layers. Because of hydrogen's small molecularweight and the high abundance of volatiles, their condensation imposes astrongly stabilizing vertical gradient of molecular weight larger than theequivalent one in Jupiter and Saturn. The resulting inhibition of verticalmotions should lead to a moist convective regime that differs significantlyfrom the one occurring on nitrogen-based atmospheres like those of Earth orTitan. As a consequence, the thermal structure of the deep atmospheres ofUranus and Neptune is not well understood. Similar processes might occur at thedeep water cloud of Jupiter in Saturn, but the Ice Giants offer the possibilityto study these physical aspects in the upper methane cloud layer. A combinationof orbital and in situ data will be required to understand convection and itsrole in atmospheric dynamics in the Ice Giants, and by extension, in hydrogenatmospheres including Jupiter, Saturn and giant exoplanets.

philosophical transactions - royal society. mathematical, physical and engineering sciences/philosophical transactions - royal society. mathematical, physical and engineering sciences

Convective storms and atmospheric vertical structure in Uranus and Neptune