Interaction of eddies and mean zonal flow on Jupiter as inferred from Voyager 1 and 2 images.
Abstract
Voyager 1 and 2 narrow‐angle frames were used to obtain displacements of features at resolutions of 130 km over time intervals of 1 Jovian rotation. The zonal velocity ū was constant to 1.5% during the 4 months between the Voyager 1 and 2 encounters. The latitudes of the zonal jet maxima (extrema of ū) are the same as inferred from earth‐based observations extending over the past 80 years. The curvature of the velocity profile d²ū/dy² varies with latitudinal coordinate y in the range from −3β to +2β, where β is the planetary vorticity gradient. The barotropic stability criterion is violated at about 10 latitudes between ±60°. The eddy momentum flux variation with latitude is positively correlated with dū/dy for both Voyager 1 and 2 data. The rate of conversion of eddy kinetic energy into zonal mean kinetic energy is in the range 1.5–3.0 Wm −2 , for a layer 2.5 bar deep. The time constant for resupply of zonal mean kinetic energy by eddies is in the range 2–4 months, less than the interval between Voyager encounters. The rate of energy conversion is more than 10% of the total infrared heat flux for Jupiter, in contrast with earth where it is only 0.1% of the infrared heat flux. This hundred‐fold difference suggests that the thermomechanical energy cycles are very different on the two planets.
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Eddy angular momentum fluxes inferred from tracking cloud features in Jupiter's and Saturn's upper tropospheres indicate that the mean conversion rate from eddy to mean-flow kinetic energy is of order 10^-5 W m^-3.
“But the eddy angular momentum fluxes inferred from tracking cloud features in Jupiter's and Saturn's upper tropospheres indicate that the mean conversion rate from eddy to mean-flow kinetic energy is of order 10 25 W m 23 (Ingersoll et al. 1981;Salyk et al. 2006;Del Genio et al. 2007).”
From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Ingersoll et al. 1981
Such angular momentum transport from retrograde into prograde jets has indeed been observed on Jupiter and Saturn.
“Such angular momentum transport from retrograde into prograde jets has indeed been observed on Jupiter and Saturn (Ingersoll et al. 1981;Salyk et al. 2006;Del Genio et al. 2007).”
From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Ingersoll et al. 1981
This angular momentum transport has a baroclinic structure and, in the Jupiter and Saturn simulations, is in structure and magnitude consistent with observations.
“It has a baroclinic structure and, in the Jupiter and Saturn simulations, is in structure and magnitude consistent with observations (cf.Ingersoll et al. 1981;Salyk et al. 2006;Del Genio et al. 2007).”
From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Ingersoll et al. 1981
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- Authors
- Ingersoll, A. P., Beebe, R. F., Mitchell, J. L., Garneau, G. W., Yagi, G. M., & Müller, J.
- Venue
- Journal of Geophysical Research: Space Physics
- Publisher
- American Geophysical Union (AGU)
- Published
- 1981-09-30
- Volume
- 86
- Issue
- A10
- Pages
- 8733-8743
- ISSN
- 0148-0227 (ISSN-L)
- OpenAlex
- W2168895689
- Cited by
- 193
- References
- 11
- Citations by year
- 2026: 1 · 2025: 3 · 2024: 7 · 2023: 2 · 2022: 3 · 2021: 3 · 2020: 6 · 2018: 8 · 2017: 5 · 2016: 1 · 2015: 1 · 2014: 3 · 2013: 3 · 2012: 4
- FWCI
- 15.36
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- Journal of Geophysical Research Atmospheres (publishedVersion)
- CaltechAUTHORS (California Institute of Technology) (submittedVersion)
- Topics
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Astro and Planetary Science
- Physical Sciences › Engineering › Computational Mechanics › Fluid Dynamics and Turbulent Flows
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Ionosphere and magnetosphere dynamics
- Keywords
- Jupiter, zonal jets, eddy-mean flow interaction, eddy momentum flux, atmospheric dynamics
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