Description of the NCAR Community Climate Model (CCM2)

Hack, James J.; Boville, A.; Briegleb, P.; Kiehl, Tim-Rasmus; Williamson, L.

doi:10.5065/d6qz27xv

Cited by 56 publications

(1 citation statement)

References 23 publications

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“…Cloud fraction and the associated optical properties are evaluated via a diagnostic method. The diagnosis is a generalization of the scheme introduced by Slingo (1987), with variations described in Hack et al (1993), Kiehl et al (1998), andKristjánsson (1998). The model has 26 vertical levels from the surface to the middle stratosphere (≈3 hPa) at the horizontal resolution of T42, which is 2.8 • in latitude by 2.8 • in longitude.…”

Section: D Gcm Simulationsmentioning

confidence: 99%

Idealized 2D Cloud-Resolving Simulations for Tidally Locked Habitable Planets

Song,

Yang,

Luo

et al. 2021

Preprint

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Cloud is critical for planetary climate and habitability, but it is also one of the most challenging parts of studying planets in and beyond the solar system. Previous simulations using global general circulation models (GCMs) found that for 1:1 tidally locked (i.e., synchronously rotating) terrestrial planets with oceans, strong convergence and convection produce optically thick clouds over the substellar area. One obvious weakness of these studies is that clouds are parameterized based on the knowledge on Earth, and whether it is applicable to exoplanetary environment is unknown. Here we use a cloud-resolving model (CRM) with high resolution (2 km) in a two-dimensional (2D) configuration to simulate the clouds and circulation on tidally locked aqua-planets. We confirm that the substellar area is covered by deep convective clouds, the nightside is dominated by low-level stratus clouds, and these two are linked by a global-scale overturning circulation. We further find that a uniform warming of the surface causes the width of convection and clouds to decrease, but a decrease of day-night surface temperature contrast or an increase of longwave radiative cooling rate causes the width of convection and clouds to increase. These relationships can be roughly interpreted based on some simple thermodynamic theories. Comparing the results between CRM and GCM, we find that the results are broadly similar although there are many significant differences. Future work is required to use 3D CRM(s) with realistic radiative transfer and with the Coriolis force to examine the clouds and climate of tidally locked planets.

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Section: D Gcm Simulationsmentioning

confidence: 99%