Since we are likely modelling tidally locked planets, it might make sense to include/parameterise heat redistribution.
The method of Koll 2022 is relatively simple to implement since we just scale the downward flux at TOA. The scaling is set by P_surf, T_eq, and LW optical thickness.
Since we are likely modelling tidally locked planets, it might make sense to include/parameterise heat redistribution.
The method of Koll 2022 is relatively simple to implement since we just scale the downward flux at TOA. The scaling is set by P_surf, T_eq, and LW optical thickness.
See the paper here: 10.3847/1538-4357/ac3b48.