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The atmospheres of ultra-hot Jupiters have been characterized in detailthrough recent phase curve and low- and high-resolution emission andtransmission spectroscopic observations. Previous numerical studies haveanalyzed the effect of the localized recombination of hydrogen on theatmospheric dynamics and heat transport of ultra-hot Jupiters, finding thathydrogen dissociation and recombination lead to a reduction in the day-to-nightcontrasts of ultra-hot Jupiters relative to previous expectations. In thiswork, we add to previous efforts by also considering the localized condensationof clouds in the atmospheres of ultra-hot Jupiters, their resulting transportby the atmospheric circulation, and the radiative feedback of clouds on theatmospheric dynamics. To do so, we include radiatively active cloud tracersinto the existing MITgcm framework for simulating the atmospheric dynamics ofultra-hot Jupiters. We take cloud condensate properties appropriate for thehigh-temperature condensate corundum from CARMA cloud microphysics models. Weconduct a suite of GCM simulations with varying cloud microphysical andradiative properties, and we find that partial cloud coverage is a ubiquitousoutcome of our simulations. This patchy cloud distribution is inherently set byatmospheric dynamics in addition to equilibrium cloud condensation, and causesa cloud greenhouse effect that warms the atmosphere below the cloud deck.Nightside clouds are further sequestered at depth due to a dynamically inducedhigh-altitude thermal inversion. We post-process our GCMs with the Monte Carloradiative transfer code gCMCRT and find that the patchy clouds on ultra-hotJupiters do not significantly impact transmission spectra but can affect theirphase-dependent emission spectra.

Patchy nightside clouds on ultra-hot Jupiters: General Circulation Model simulations with radiatively active cloud tracers