Angular momentum budget in General Circulation Models of superrotating atmospheres: A critical diagnostic

Lebonnois, Sébastien; Covey, Curt; Grossman, Allen; Parish, H. F.; Schubert, G.; Walterscheid, R. L.; Lauritzen, P. H.; Jablonowski, Christiane

doi:10.1029/2012je004223

Cited by 39 publications

(47 citation statements)

References 33 publications

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“…Given our inability to reproduce these winds, it is our conclusion that the CAM 3 model running the finite volume dynamical core in its current form is incapable of reproducing Titan's superrotating winds. This conclusion is supported by the angular momentum analysis of Lebonnois et al (2012b), who compared the angular momentum terms of several GCMs on a modified Earth, Venus, and Titan. They found that the CAM finite volume dynamical core has errors in its angular momentum conservation that affect its ability to reproduce superrotation.…”

Section: Ad Hoc Forcing and Dynamicssupporting

confidence: 51%

“…It reaches equilibrium near a tropospheric superrotation index of 2. It is clear our non-forced model does not exhibit the superrotation in Titan's atmosphere that other Titan GCMs have recently been able to achieve (Newman et al, 2011;Lebonnois et al, 2012b). Other GCMs indicate that Titan's atmosphere may take dozens of Titan years to spin up.…”

Section: Ad Hoc Forcing and Dynamicsmentioning

confidence: 73%

See 1 more Smart Citation

Simulating Titan’s aerosols in a three dimensional general circulation model

Larson¹,

Toon²,

Friedson³

2014

Icarus

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Section: Ad Hoc Forcing and Dynamicssupporting

confidence: 51%

Section: Ad Hoc Forcing and Dynamicsmentioning

confidence: 73%

Simulating Titan’s aerosols in a three dimensional general circulation model

Larson¹,

Toon²,

Friedson³

2014

Icarus

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“…Note that some past studies have found that the CAM finite volume dynamical core failed to capture the upper atmosphere superrotating winds of Titan and Venus (Parish et al 2011;Lebonnois et al 2012;Larson et al 2014). However, here we find no resultant differences in surface climate for slow rotating Earth-like planets using all three dynamical cores available in CAM.…”

Section: Control Simulationsmentioning

confidence: 99%

Habitable Moist Atmospheres on Terrestrial Planets near the Inner Edge of the Habitable Zone around M Dwarfs

Kopparapu

Wolf

Arney

et al. 2017

ApJ

188

269

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Terrestrial planets in the habitable zones (HZs) of low-mass stars and cool dwarfs have received significant scrutiny recently Transit spectroscopy of such planets with JWST represents our best shot at obtaining the spectrum of a habitable planet within the next decade. As these planets are likely tidal-locked, improved 3D numerical simulations of such planetary atmospheres are needed to guide target selection. Here we use a 3-D climate system model, updated with new water-vapor absorption coefficients derived from the HITRAN 2012 database, to study ocean covered planets at the inner edge of the HZ around late-M to mid-K stars (2600K ≤ T ef f ≤ 4500K). Our results indicate that these updated water-vapor coefficients result in significant warming compared to previous studies, so the inner HZ around M-dwarfs is not as close as suggested by earlier work. Assuming synchronously rotating Earth-sized and Earth-massed planets with background 1 bar N 2 atmospheres, we find that planets at the inner -2 -HZ of stars with T ef f > 3000K undergo the classical "moist-greenhouse" (H 2 O mixing ratio > 10 −3 in the stratosphere) at significantly lower surface temperature (∼ 280K) in our 3-D model compared with 1-D climate models (∼ 340K). This implies that some planets around low mass stars can simultaneously undergo water-loss and remain habitable. However, for star with T ef f ≤ 3000K, planets at the inner HZ may directly transition to a runaway state, while bypassing the moist greenhouse water-loss entirely. We analyze transmission spectra of planets in a moist greenhouse regime, and find that there are several prominent H 2 O features, including a broad feature between 5-8 microns, within JWST MIRI instrument range. Thus, relying only upon standard Earth-analog spectra with 24-hour rotation period around M-dwarfs for habitability studies will miss the strong H 2 O features that one would expect to see on synchronously rotating planets around M-dwarf stars, with JWST.

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“…For planetary applications, it will be important to also check the discrete angular momentum budget (Lebonnois et al, 2012;Lauritzen et al, 2014a).…”

Section: Outlook For Dynamicomentioning

confidence: 99%

DYNAMICO-1.0, an icosahedral hydrostatic dynamical core designed for consistency and versatility

Dubos¹,

Dubey

Tort³

et al. 2015

Geosci. Model Dev.

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Abstract. The design of the icosahedral dynamical core DY-NAMICO is presented. DYNAMICO solves the multi-layer rotating shallow-water equations, a compressible variant of the same equivalent to a discretization of the hydrostatic primitive equations in a Lagrangian vertical coordinate, and the primitive equations in a hybrid mass-based vertical coordinate. The common Hamiltonian structure of these sets of equations is exploited to formulate energy-conserving spatial discretizations in a unified way.The horizontal mesh is a quasi-uniform icosahedral C-grid obtained by subdivision of a regular icosahedron. Control volumes for mass, tracers and entropy/potential temperature are the hexagonal cells of the Voronoi mesh to avoid the fast numerical modes of the triangular C-grid. The horizontal discretization is that of Ringler et al. (2010), whose discrete quasi-Hamiltonian structure is identified. The prognostic variables are arranged vertically on a Lorenz grid with all thermodynamical variables collocated with mass. The vertical discretization is obtained from the three-dimensional Hamiltonian formulation. Tracers are transported using a second-order finite-volume scheme with slope limiting for positivity. Explicit Runge-Kutta time integration is used for dynamics, and forward-in-time integration with horizontal/vertical splitting is used for tracers. Most of the model code is common to the three sets of equations solved, making it easier to develop and validate each piece of the model separately.Representative three-dimensional test cases are run and analyzed, showing correctness of the model. The design permits to consider several extensions in the near future, from higher-order transport to more general dynamics, especially deep-atmosphere and non-hydrostatic equations.

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Angular momentum budget in General Circulation Models of superrotating atmospheres: A critical diagnostic

Cited by 39 publications

References 33 publications

Simulating Titan’s aerosols in a three dimensional general circulation model

Simulating Titan’s aerosols in a three dimensional general circulation model

Habitable Moist Atmospheres on Terrestrial Planets near the Inner Edge of the Habitable Zone around M Dwarfs

DYNAMICO-1.0, an icosahedral hydrostatic dynamical core designed for consistency and versatility

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