The DOI matches its Crossref record; 66 of the 69 references it cites were found in a registry or an index.
Atmospheric Dynamics of the Outer Planets
Abstract
Despite major differences in the solar and internal energy inputs, the atmospheres of the four Jovian planets all exhibit latitudinal banding and high-speed jet streams. Neptune and Saturn are the windiest planets, Jupiter is the most active, and Uranus is a tipped-over version of the others. Large oval storm systems exhibit complicated time-dependent behavior that can be simulated in numerical models and laboratory experiments. The largest storm system, the Great Red Spot of Jupiter, has survived for more than 300 years in a chaotic shear zone where smaller structures appear and dissipate every few days. Future space missions will add to our understanding of small-scale processes, chemical composition, and vertical structure. Theoretical hypotheses about the interiors provide input for fluid dynamical models that reproduce many observed features of the winds, temperatures, and cloud patterns. In one set of models the winds are confined to the thin layer where clouds form. In other models, the winds extend deep into the planetary fluid interiors. Hypotheses will be tested further as observations and theories become more exact and detailed comparisons are made.
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In the citing paper
“In the Uranus and Neptune simulations, the equator-to-pole brightness temperature contrasts are 8 and 2 K, respectively, consistent with observations (Ingersoll 1990).”
From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Ingersoll 1990
In the citing paper
“In the Saturn simulation, the equator-topole brightness temperature contrast is 7 K, consistent with observations (Ingersoll 1990;Fletcher et al. 2007).”
From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Ingersoll 1990
In the citing paper
“In the Jupiter simulation, the equator-to-pole contrast in the brightness temperature of thermal radiation is 10 K, which is similar to, albeit larger than, the observed brightness temperature contrast or the observed temperature contrast near the emission level (Ingersoll et al. 1976;Ingersoll 1990;Ingersoll et al. 2004;Simon-Miller et al. 2006).”
From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Ingersoll 1990
In the citing paper
“Variations in brightness temperature gradients off the equator may be weaker in the Jupiter and Saturn simulations than they are in observations, at least at some wavelengths(Ingersoll 1990; Ingersoll et al. 2004).”
From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Ingersoll 1990
In the citing paper
“The thermal optical depths t l0 at pressure p 0 are chosen such that the observed thermal emission levels (e.g., Ingersoll 1990) of the giant planets approximately correspond to t l 5 1.”
From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Ingersoll 1990
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Research works printed but not linked: 12
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Cited by
Sorted by citations
Schou, J., Antia, H. M., Basu, S., Bogart, R. S., Bush, R. I., Chitre, S. M., Christensen-Dalsgaard, J., Mauro, M. P. D., Dziembowski, W. A., Eff‐Darwich, A., et al. (1998) · The Astrophysical Journal · doi:10.1086/306146 · Cited by 998
Porco, C., West, R., Squyres, S., McEwen, A., Thomas, P., Murray, C., Delgenio, A., Ingersoll, A., Johnson, T., Neukum, G., et al. (2004) · Space Science Reviews · doi:10.1007/s11214-004-1456-7 · Cited by 402
“By creating movies of the Saturn atmosphere in motion, we can observe the life cycle of vortices as they merge, split, or oscillate (Ingersoll, 1990; Polvani et al., 1990; Li et al., 2004; see movies of the Jupiter atmosphere at http://ciclops.org).”
MethodJovian atmospheric dynamics: an update after Galileo and Cassini
Vasavada, A. R., & Showman, A. P. (2005) · Reports on Progress in Physics · doi:10.1088/0034-4885/68/8/r06 · Cited by 329
TRANSPORT BY COHERENT BAROTROPIC VORTICES
Provenzale, A. (1999) · Annual Review of Fluid Mechanics · doi:10.1146/annurev.fluid.31.1.55 · Cited by 325
“as the Great Red Spot on Jupiter (e.g. Ingersoll 1990, Dowling 1995), dark and bright star spots where rotation and magnetic fields both play a role (Dowling & Spiegel 1990), and perhaps vortex spots on astrophysical disks (Abramowicz et al 1991, Bracco et al 1998).”
BackgroundSimulation of equatorial and high-latitude jets on Jupiter in a deep convection model
Heimpel, M., Aurnou, J., & Wicht, J. (2005) · Nature · doi:10.1038/nature04208 · Cited by 291
Metadata
- Authors
- Ingersoll, A. P.
- Affiliations
- California Institute of Technology (US)
- Corresponding author
- Ingersoll, Andrew P.
- ORCID
- Ingersoll, Andrew P.
- Venue
- Science
- Published
- 1990-04-20
- Volume
- 248
- Issue
- 4953
- Pages
- 308-315
- ISSN
- 0036-8075 (ISSN-L)
- 1095-9203
- OpenAlex
- W2101776268
- Cited by
- 199
- References
- 69
- Citations by year
- 2026: 1 · 2025: 4 · 2024: 6 · 2023: 3 · 2022: 6 · 2021: 5 · 2020: 8 · 2019: 6 · 2018: 10 · 2017: 9 · 2016: 3 · 2015: 3 · 2014: 7 · 2013: 6 · 2012: 2
- FWCI
- 10.40
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- Science (publishedVersion)
- PubMed (publishedVersion)
- CaltechAUTHORS (California Institute of Technology) (submittedVersion)
- Topics
- Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › 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
- Jovian planets, planetary atmospheres, atmospheric dynamics, jet stream, Great Red Spot, Jupiter, Saturn, Uranus, Neptune, cloud formation, planetary interiors, fluid dynamical model, space missions
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