Simulating the cloudy atmospheres of HD 209458 b and HD 189733 b with the 3D Met Office Unified Model

摘要: To understand and compare the 3D atmospheric structure of HD 209458 b 189733 b, focusing on formation distribution cloud particles, as well their feedback dynamics thermal profile. We couple Met Office Unified Model (UM), including detailed treatments radiative transfer dynamics, to a kinetic scheme. The resulting model self--consistently solves for condensation seeds, surface growth evaporation, gravitational settling advection, via absorption and, crucially, scattering. Fluxes directly obtained from UM are used produce synthetic SEDs phase curves. Our simulations show extensive in both planets, however, cooler temperatures result higher particle number densities. Sub-micron particles suspended by vertical flows leading upper-atmosphere cover. A combination meridional advection efficient high latitude regions, enhanced coverage latitudes > 30 degrees leads zonally banded all our simulations. bands extend around entire planet(s), temperatures, even day side, remain below temperature silicates oxides. Therefore, simulated optical curve shows no `offset', contrast observations. Efficient scattering results an cooling up 250K, advection-driven fluctuating opacity causes temporal variability emission. inclusion this fundamental cloud-atmosphere significant differences with approaches neglecting these physical elements suggests note caution interpretations such scattering, merits further study.