Jovian atmospheric dynamics: an update after Galileo and Cassini

By Ashwin R. Vasavada, A. Showman. 2005

346 citations recorded by the source corpus.

Subfields: Astronomy and Astrophysics, Molecular Biology

View Paper: https://www.semanticscholar.org/paper/0fbe08b9430f9c915a4fdfdcd9b6e4754626b66e

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Citations in the corpus

On the arrest of inverse energy cascade and the rhines scale (2006, background): “Rhines scale plays a prominent role in many theories of large-scale atmospheric and oceanic circulation (see, e.g., James and Gray (1986); Vallis and Maltrud (1993); Held and Larichev (1996); Held (1999); Lapeyre and Held (2003); Schneider (2004); LaCasce and Pedlosky (2004); Vallis (2006)) as well ”
The deep wind structure of the giant planets: Results from an anelastic general circulation model (2009, background): “have been two essentially decoupled approaches treating the formation of the zonal winds on the giant planets (see Vasavada and Showman, 2005, for a review).”
ATMOSPHERIC CIRCULATION OF HOT JUPITERS: COUPLED RADIATIVE-DYNAMICAL GENERAL CIRCULATION MODEL SIMULATIONS OF HD 189733b and HD 209458b (2008, neutral): “For flows driven primarily by creation of turbulence at small scales, turbulence theory predicts that jet widths in latitude scale as∼ π(U/β)1/2, where U is a mean wind speed (Rhines 1975; Vasavada & Showman 2005).”
JUpiter ICy moons Explorer (JUICE): An ESA mission to orbit Ganymede and to characterise the Jupiter system (2013, background): “Jupiter’s vertical atmospheric structure is governed by a delicate balance between solar, chemical and internal energy sources, and its layers are coupled by poorly-understood dynamical processes that transport energy, momentum and material (Vasavada and Showman, 2005).”
Constraints on Deep-seated Zonal Winds Inside Jupiter and Saturn (2007, background): “These considerations suggest that strong zonal winds are confined to shallow, stably stratified layers, with equatorial jets being the possible exception.”
Atmospheric Circulation of Hot Jupiters: Three-dimensional Circulation Models of HD 209458b and HD 189733b with Simplified Forcing (2008, neutral): “…implicit in such simpliﬁed models also allow the model dynamics to be relatively easily understood; a comparison of such re-sults with 3D models and observations can lend important insights into which dynamical processes cause which outcomes (Vasavada & Showman 2005; Showman et al. 2007).”
AB INITIO SIMULATIONS FOR MATERIAL PROPERTIES ALONG THE JUPITER ADIABAT (2012, background): “…Stanley & Glatzmaier 2010; Schubert & Soderlund 2011), basic properties, such as the observed flow patterns in the atmosphere (Heimpel et al. 2005; Vasavada & Showman 2005; Kaspi et al. 2009; Gastine & Wicht 2012), still await explanations that are consistent with planetary structure and dynamo…”
Rotating convective turbulence in Earth and planetary cores (2015, background): “However, unlike in Cartesian boxes where LSVs grow to the size of the computational domain, in planetary cores their growth should halt approximately at the Rhines scale, denoted as ‘turb, where boundary curvature effects act to truncate the inverse energy cascade (e.g., Vasavada and Showman, 2005).”