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Deciphering the role of clouds is central to our understanding of exoplanetatmospheres, as they have a direct impact on the temperature and pressurestructure, and observational properties of the planet. Super-hot Jupitersoccupy a temperature regime similar to low mass M-dwarfs, where minimal cloudcondensation is expected. However, observations of exoplanets such as WASP-12b(Teq ~ 2500 K) result in a transmission spectrum indicative of a cloudyatmosphere. We re-examine the temperature and pressure space occupied by thesesuper-hot Jupiter atmospheres, to explore the role of the initial Al- andTi-bearing condensates as the main source of cloud material. Due to the hightemperatures a majority of the more common refractory material is not depletedinto deeper layers and would remain in the vapor phase. The lack of depletioninto deeper layers means that these materials with relatively low cloud massescan become significant absorbers in the upper atmosphere. We providecondensation curves for the initial Al- and Ti-bearing condensates that may beused to provide quantitative estimates of the effect of metallicity on cloudmasses, as planets with metal-rich hosts potentially form more opaque cloudsbecause more mass is available for condensation. Increased metallicity alsopushes the point of condensation to hotter, deeper layers in the planetaryatmosphere further increasing the density of the cloud. We suggest that planetsaround metal-rich hosts are more likely to have thick refractory clouds, anddiscuss the implication on the observed spectra of WASP-12b.

High temperature condensate clouds in super-hot Jupiter atmospheres