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Cited by 149Astro and Planetary ScienceStellar, planetary, and galactic studiesFluid Dynamics and Turbulent Flows

The deep wind structure of the giant planets: Results from an anelastic general circulation model

Kaspi, Yohai, Flierl, Glenn R., Showman, Adam P.·2009·Icarus
DOI 10.1016/j.icarus.2009.03.026
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Crossref · 10.1016/j.icarus.2009.03.026

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  • The absence of momentum injection by eddies might be caused by injection of energy at smaller scales not resolvable by the measurements or might reinforce the idea that the jets are deeply rooted structures driven by internal convection, making them insensitive at tropospheric level to the seasonal cycle.

    “The absence of momentum injection by eddies might be caused by injection of energy at smaller scales not resolvable by the measurements or might reinforce the idea that the jets are in fact deeply rooted structures driven by the internal convection [ Aurnou and Olson, 2001; Kaspi et al. 2009] making them insensitive at tropospheric level to the seasonal cycle”

    From Dynamics of Saturn's polar regions (2015) · cites this paper as Kaspi et al. 2009

  • Alternating jets on gas giant planets are either shallow, existing above about 10 bars, or deep, extending to tens of thousands of bars.

    “on one hand, the alternating jets on gas giant planets are 'shallow', existing above 10 bars or so [15-17]; on the other hand, zonal jets are 'deep', extending to tens of thousands of bars [18-22].”

    From Deep rotating convection generates the polar hexagon on Saturn (2020) · cites this paper as [22]

  • The meridional eddy fluxes of angular momentum per unit volume in deep-flow models have a barotropic structure, extending roughly along cylinders concentric with the planet's spin axis over the entire depth of the fluid, typically to pressures of order 10^6 bar.

    “Their meridional eddy fluxes of angular momentum per unit volume (taking density variations into account) have a barotropic structure: they extend roughly along cylinders concentric with the planet's spin axis over the entire depth of the fluid, typically to pressures of order 10 6 bar (e.g., Kaspi et al. 2009, their Fig.10).”

    From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Kaspi et al. 2009

  • Under conditions of small convective Rossby number and negligible viscous momentum dissipation and thermal diffusion, convective plumes are columns aligned with M_V surfaces because rapid rotation inhibits motion perpendicular to M_V surfaces in the absence of viscous or other stresses.

    “Under these circumstances, convective plumes are columns aligned with M V surfaces because, as above, rapid rotation inhibits motion perpendicular to M V surfaces in the absence of viscous or other stresses (e.g., Busse 1976Busse , 1978;;Kaspi et al. 2009;Jones et al. 2009).”

    From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Kaspi et al. 2009

  • If entropy deviations from an isentropic reference state are not small so that the anelastic approximation cannot be made, the thermal wind balance becomes more complicated.

    “If entropy deviations from an isentropic reference state are not small so that the anelastic approximation cannot be made, the thermal wind balance (13) becomes more complicated(Kaspi et al. 2009).”

    From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Kaspi et al. 2009

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Authors
Kaspi, Y., Flierl, G. R., & Showman, A. P.
Affiliations
  • Massachusetts Institute of Technology (US)
  • University of Arizona (US)
Corresponding author
Kaspi, Yohai
ORCID
Venue
Icarus
Publisher
Elsevier BV
Published
2009-08
Volume
202
Issue
2
Pages
525-542
ISSN
0019-1035 (ISSN-L)
DOI
10.1016/j.icarus.2009.03.026
OpenAlex
W2087943296
Cited by
149
References
72
Citations by year
2026: 5 · 2025: 5 · 2024: 9 · 2023: 7 · 2022: 6 · 2021: 8 · 2020: 15 · 2019: 13 · 2018: 9 · 2017: 16 · 2016: 6 · 2015: 11 · 2014: 10 · 2013: 9 · 2012: 8
FWCI
3.36
Type
journal article
Language
en
Open access
closed
Licence
www.elsevier.com/tdm/userlicense/1.0/ (tdm)
Locations
  • Icarus (publishedVersion)
  • CaltechAUTHORS (California Institute of Technology) (submittedVersion)
Topics
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
  • Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
  • Physical Sciences › Engineering › Computational Mechanics › Fluid Dynamics and Turbulent Flows
Keywords
giant planet atmospheres, baroclinic vorticity, compressibility effects, vertical shear, thermal wind relation, equatorial superrotation, poleward heat transport, Rayleigh number, Jupiter, Saturn

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