2020/10/31 by Michael T. Roman, Eliza M. -R. Kempton, Eliza M.-R. Kempton +4 · 1 citation
Physics and Astronomy · #Amplitude #Astro and Planetary Science #Astronomy and Astrophysical Research #Hot Jupiter #Jupiter (rocket family) #Observable #Planet #Radiative transfer #Range (aeronautics) #Scale height #Stellar, planetary, and galactic studies #Thermal #astro-ph.EP
paper · pdf · doi:10.3847/1538-4357/abd549
Accepted to ApJ. 34 pages, 16 figures
openalex created_date 2020/10/22 · arxiv created 2020/12/19 · openalex publication_date 2021/02/01 · arxiv updated 2021/02/24 · openalex updated_date 2026/08/05
Abstract Using a general circulation model (GCM), we investigate trends in simulated hot Jupiter atmospheres for a range of irradiation temperatures (1500–4000 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 Jupiter 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 ≈ 3000 K ( T eq ≈ 2100 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 ≈ 2000–3500 K) with clouds confined to the nightside and western limb. If clouds are vertically compact (i.e., on the 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 ≲ 3000 K.