Superrotation of Venus' atmosphere analyzed with a full general circulation model

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The Atmospheric Dynamics of Venus (2017, methodology): “The results broadly confirm those obtained by Lebonnois et al. (2010a, 2010b) in forming a reasonably realistic super-rotation at the cloud level, driven by a combination of thermal tides and planetary waves, but only weak zonal winds in the deep atmosphere.”
NCAR Release of CAM‐SE in CESM2.0: A Reformulation of the Spectral Element Dynamical Core in Dry‐Mass Vertical Coordinates With Comprehensive Treatment of Condensates and Energy (2018, background): “Similarly for axial angular momentum (AAM) which is an important conserved quantity of the continuous equations of motion (e.g., Lebonnois et al., 2010).”
3D modelling of the early Martian Climate under a denser CO2 atmosphere: Temperatures and CO2 ice clouds. (2012, methodology): “In analogy with Earth and Venus, even after taking into account the differences in size, it can be estimated that the initial inventory of volatiles on Mars included at least several bars of atmospheric gases, mostly CO2 (see Haberle et al. 1998).”
Exploring the faint young Sun problem and the possible climates of the Archean Earth with a 3‐D GCM (2013, unknown): “ing a nite dierence dynamical core on an Arakawa C grid. This dynamical core has been in a variety of atmospheres such as the present Earth [Hourdin et al., 2006], Mars [Forget et al., 1999], Venus [Lebonnois et al., 2010], and Titan [Lebonnois et al., 2012; Charnay and Lebonnois, 2012]. In this pap”