All the modelling in PROTEUS is done under the assumption that the planet can be globally-averaged into a single 1D column. However, we could extend this by simulating multiple columns around the planet's equator, with a description of heat transport between them. This has been done before with models of exoplanet atmospheres, but never for a magma ocean model.
This would allow us to capture day-night differences on tidally locked planets, including the potential for nightside clouds, and also could allow comparison with phase curve observations.
All the modelling in PROTEUS is done under the assumption that the planet can be globally-averaged into a single 1D column. However, we could extend this by simulating multiple columns around the planet's equator, with a description of heat transport between them. This has been done before with models of exoplanet atmospheres, but never for a magma ocean model.
This would allow us to capture day-night differences on tidally locked planets, including the potential for nightside clouds, and also could allow comparison with phase curve observations.