text: 63,157,1316752822193606656,1149734612693745666,Emily Rauscher,"🗣 New paper alert! <LINK> In this work, led by Michael Roman, we present a grid of 3D models of hot Jupiters with clouds (temperature dependent and with radiative feedback) across a wide range of irradiation temperature, for different assumed cloud properties. <LINK> In order of decreasing irradiation temperate, clouds form successively on: the night, the cool western terminator, the eastern terminator, and even across the dayside! For planets cooler than irradiation temperatures of about 3000 K (Teq ~ 2100 K) clouds influence observable properties, like phase curves (both thermal and reflected)! Sometimes clouds even produce temperature inversions! Also see a lovely complementary paper by @V_Parmentier that is also on arXiv today! (Sorry this thread isn’t snazzier... my kindergartener needs help with his class work and is crying in my lap right now)",http://arxiv.org/abs/2010.06936,"Using a general circulation model (GCM), we investigate trends in simulated hot Jupiter atmospheres for a range of irradiation temperatures (1,500 - 4,000 K), surface gravities (10 and 40 m s-2), and cloud conditions. Our models include simplified temperature-dependent clouds with radiative feedback and show how different cloud compositions, vertical thicknesses, and opacities shape hot Jupiters atmospheres by potentially increasing planetary albedos, decreasing photospheric pressures and nightside temperatures, and in some cases producing strong dayside thermal inversions. With decreasing irradiation, clouds progressively form on the nightside and cooler western limb followed by the eastern limb and central dayside. We find that clouds significantly modify the radiative transport and affect the observable properties of planets colder than T_irr ~ 3,000~K (T_eq~2,100 K) depending on the clouds' vertical extent. The precise strength of expected effects depends on the assumed parameters, but trends in predicted phase curves emerge from an ensemble of simulations. Clouds lead to larger phase curve amplitudes and smaller phase curve offsets at IR wavelengths, compared to cloud-free models. At optical wavelengths, we predict mostly westward phase curve offsets at intermediate temperatures (T_irr ~ 2,000 - 3,500 K) with clouds confined to the nightside and western limb. If clouds are vertically compact (i.e. on order of a pressure scale height in thickness), their distributions and effects become more complicated as different condensates form at different heights -- some too deep to significantly affect the observable atmosphere. Our results have implications for interpreting the diversity of phase curve observations of planets with T_irr <~3,000~K. ","Clouds in Three-Dimensional Models of Hot Jupiters Over a Wide Range of