Stabilizing cloud feedback dramatically expands the habitable zone of tidally locked planets. Dim prospects for transmission spectra of ocean earths around M stars. Clouds will likely prevent the detection of water vapor in JWST transmission spectra of terrestrial exoplanets. III: Simulated observables–the return of the spectrum. The TRAPPIST-1 Habitable Atmosphere Intercomparison (THAI). Impact of clouds and hazes on the simulated JWST transmission spectra of habitable zone planets in the TRAPPIST-1 System. Global Physical Climatology (Elsevier Science, 2015).įauchez, T. Furthermore, cloud streets-long bands of low-level clouds oriented nearly parallel to the direction of the mean boundary-layer winds-appear in the CPM and substantially affect energy balance and surface precipitation at a local level. The CPM produces relatively lower cloud liquid water concentration, smaller cloud coverage, lower cloud albedo and deeper H 2O spectral features than previous general circulation model simulations using empirical convection and cloud parameterizations. We show that the substellar region is covered by deep convective clouds and cloud albedo increases with increasing stellar flux. Here we present CPM simulations in a quasi-global domain with high spatial resolution (4 × 4 km 2 grid) and explicit convection to study the cloud regime of 1:1 tidally locked rocky planets orbiting around low-mass stars. Given the lack of in situ observations, one of the most preferable approaches is to use cloud-resolving or cloud-permitting models (CPM). Determining the behaviour of convection and clouds is one of the biggest challenges in our understanding of exoplanetary climates.
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