The DOI matches its Crossref record; 68 of the 72 references it cites were found in a registry or an index.
The deep wind structure of the giant planets: Results from an anelastic general circulation model
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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 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
In the citing paper
“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]
In the citing paper
“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
In the citing paper
“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
In the citing paper
“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
Citations
Cites
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An Equation of State for Low-Mass Stars and Giant Planets
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The Maximum Intensity of Hurricanes
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Research works printed but not linked: 1
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Items 101–149 of 149
Simulating rotating fluid bodies: When is vorticity generation via density-stratification important?
Evonuk, M., & Samuel, H. (2011) · Earth and Planetary Science Letters · doi:10.1016/j.epsl.2011.11.036 · Cited by 9
“Deep shell differential rotation in rotating fluids has been simulated in 3D (Aurnou and Olson, 2001; Christensen, 2001, 2002; Glatzmaier, 2005; Heimpel et al., 2005; Jones and Kuzanyan, 2009; Kaspi et al., 2009), in the 2D meridional plane (Jones et al.”
BackgroundConstraining Jupiter's internal flows using Juno magnetic and gravity measurements
Galanti, E., Cao, H., & Kaspi, Y. (2017) · Geophysical Research Letters · doi:10.1002/2017gl074903 · Cited by 8
Self-citationInvestigating Barotropic Zonal Flow in Jupiter's Deep Atmosphere Using Juno Gravitational Data
Kulowski, L., Cao, H., Yadav, R. K., & Bloxham, J. (2021) · Journal of Geophysical Research Planets · doi:10.1029/2020je006795 · Cited by 8
Depth Dependent Dynamics Explain the Equatorial Jet Difference Between Jupiter and Saturn
Duer, K., Galanti, E., & Kaspi, Y. (2024) · Geophysical Research Letters · doi:10.1029/2023gl107354 · Cited by 7
“This could explain the absence of midlatitude jets, for example, in deep, convection‐driven, simulations (e.g., Kaspi et al., 2009).”
BackgroundInfluentialSelf-citationSimulation of the Tianwen-4 Mission Contribution to Jupiter Gravity Field Improvement
Afzal, Z., Yan, J., Dirkx, D., Huang, Y. H., Wang, Z., Haider, Z., & Barriot, J. (2025) · The Astrophysical Journal · doi:10.3847/1538-4357/adb1e8 · Cited by 7
“On the equatorial side of these jets, there is an eastward current moving at approximately 100 m s − 1 with respect to the System III reference frame, exhibiting super-rotation close to the equator within 6 ° ( Y. Kaspi et al. 2009 ) .”
Characterizing Jupiter’s interior using machine learning reveals four key structures
Ziv, M., Galanti, E., Howard, S., Guillot, T., & Kaspi, Y. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202452383 · Cited by 7
Self-citationContributions to Jupiter's Gravity Field From Dynamics in the Dynamo Region
Kulowski, L., Cao, H., & Bloxham, J. (2020) · Journal of Geophysical Research Planets · doi:10.1029/2019je006165 · Cited by 7
“These winds may extend thousands of kilometers deep into Jupiter's interior (Busse, 1976; Heimpel et al., 2005; Jones & Kuzanyan, 2009; Kaspi et al., 2009) or be confined to a thin weather layer on top of weaker interior convective flows (Dowling, 1995; Vasavada & Showman, 2005).”
BackgroundConvective differential rotation in stars and planets – II. Observational and numerical tests
Jermyn, A. S., Chitre, S. M., Lesaffre, P., & Tout, C. A. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2576 · Cited by 7
A mascon approach to estimating the depth of Jupiter’s Great Red Spot with Juno gravity measurements
Parisi, M., Folkner, W. M., Galanti, E., Kaspi, Y., Buccino, D., Oudrhiri, K., & Bolton, S. J. (2019) · Planetary and Space Science · doi:10.1016/j.pss.2019.104781 · Cited by 7
“The thermal wind (TW) equation has been widely used in the past to explain Jupiter’s large-scale dynamics (Kaspi et al., 2009; Kaspi et al., 2010) and the gravity field derived from the density anomaly profile has matched with remarkable accuracy the values of the first four odd harmonics of Jupiter’s gravity field (K…”
BackgroundMethodSelf-citationDirect driving of simulated planetary jets by upscale energy transfer
Böning, V. G. A., Wulff, P., Dietrich, W., Wicht, J., & Christensen, U. R. (2022) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202244278 · Cited by 7
Resolving the Latitudinal Short‐Scale Gravity Field of Jupiter Using Slepian Functions
Parisi, M., Galanti, E., Folkner, W. M., Kaspi, Y., & Buccino, D. (2020) · Journal of Geophysical Research Planets · doi:10.1029/2020je006416 · Cited by 6
“…(longitudinal) velocity component, r is the radial direction and θ is the latitude. ucyl is the velocity profile obtained by extending the observed cloud level wind (Tollefson et al., 2017) along the direction of the rotation axis (Kaspi et al., 2009), and RJ is Jupiter's equatorial 1-bar radius.”
BackgroundSelf-citationChachan, Y., & Stevenson, D. J. (2019) · Icarus · doi:10.1016/j.icarus.2018.12.020 · Cited by 5
“Deviations from the Taylor-Proudman theorem in a fluid with large density variations but no MHD effects arise primarily from latitudinal entropy gradients but also potentially from the Reynolds stress (e.g., Equation 22 of Liu et al., 2008; Kaspi et al., 2009).”
BackgroundThree eras of planetary exploration
Ingersoll, A. P. (2017) · Nature Astronomy · doi:10.1038/s41550-016-0010 · Cited by 5
Galileo probe interpretation indicating a neutrally stable layer in the Jovian troposphere
O’Neill, M. E., Kaspi, Y., & Fletcher, L. N. (2017) · Geophysical Research Letters · doi:10.1002/2017gl073305 · Cited by 5
Self-citationExploring Jupiter's Polar Deformation Lengths with High-resolution Shallow Water Modeling
Hyder, A., Lyra, W., Chanover, N. J., Morales-Juberías, R., & Jackiewicz, J. (2022) · The Planetary Science Journal · doi:10.3847/psj/ac7952 · Cited by 5
“This includes, but is not limited to, full general circulation models of the entire atmosphere (e.g. Williams 1978, 1988; Kaspi et al. 2009), as well as localized process modeling for predictions of storm behavior and evolution to determine the quasi-steady state of such systems (e.g.…”
BackgroundThree-dimensional numerical simulation of convection in giant planets: Effects of solid core size
Cai, T., & Chan, K. L. (2012) · Planetary and Space Science · doi:10.1016/j.pss.2012.07.023 · Cited by 5
From gas to ice giants: A unified mechanism for equatorial jets
Duer, K., Gavriel, N., Galanti, E., Tziperman, E., & Kaspi, Y. (2025) · Science Advances · doi:10.1126/sciadv.ads8899 · Cited by 4
“Studies indicate that the equatorial jets can form in either direction depending on the dominance of Coriolis or buoyancy forces (i.e., Rayleigh number and Ekman number, see Materials and Methods) ( 29, 30, 42 ).”
InfluentialSelf-citationAnalytical Estimation of the Widths of Hadley Cells in the Solar System
Rees, K. N., & Garrett, T. J. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/ab1fde · Cited by 4
“…deep-forcing model, cylindrical Taylor columns drive differential rotation in the deep interior of the planet, which manifest as zonal midlatitude jets that span from the deep interior to the upper cloud level (Ingersoll 1969), reproducing a Hadley cell in equatorial regions (Kaspi et al. 2009).”
BackgroundPoleward translation of vortices due to deep thermal convection on a rotating planet
Afanasyev, Y. D., & Huang, Y. (2019) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091929.2019.1694676 · Cited by 4
Some statistical properties of three-dimensional zonostrophic turbulence
Cabanes, S., Favier, B., & Bars, M. L. (2018) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091929.2018.1467413 · Cited by 3
“…have revived the possibility to generate Jupiter like jets from a 3D convective envelope, extending through the molecular layer between the surface weather layer and the deeper dynamo region (Christensen 2001, Heimpel et al. 2005, Kaspi et al. 2009, Heimpel et al. 2016, Cabanes et al. 2017).”
BackgroundEffects of neutral buoyancy outer boundary condition in models of deep convection in giant planets
Cuff, K., & Heimpel, M. H. (2018) · Physics of The Earth and Planetary Interiors · doi:10.1016/j.pepi.2018.07.001 · Cited by 4
On the energetics of a two-layer baroclinic flow
Jougla, T., & Dritschel, D. G. (2017) · Journal of Fluid Mechanics · doi:10.1017/jfm.2017.79 · Cited by 3
“(Kaspi et al. 2009) studied a 3D non-hydrostatic general circulation model, with a large density variation under the anelastic approximation.”
BackgroundHigh‐Latitude Westward Jets in the Earth's Outer Core Due to Small‐Scale Convection
Afanasyev, Y. D. (2018) · Geophysical Research Letters · doi:10.1029/2018gl078550 · Cited by 3
A joint investigation of Saturn’s deep zonal flow via its gravitational field and Ohmic dissipation
Yuan, L., & Kong, D. (2023) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stad2556 · Cited by 3
Observational constraints on the strength and depth of the zonal jets on Saturn
Galanti, E., Durante, D., IESS, L., & Kaspi, Y. (2025) · Nature Communications · doi:10.1038/s41467-025-57790-x · Cited by 3
Self-citationAtmospheric Dynamics of Giants and Icy Planets
Sánchez-Lavega, A., & Heimpel, M. H. (2017) · Springer eBooks · doi:10.1007/978-3-319-30648-3_51-1 · Cited by 2
Dynamics of Baroclinic Multiple Zonal Jets
Berloff, P., & Kamenkovich, I. V. (2019) · Cambridge University Press eBooks · doi:10.1017/9781107358225.019 · Cited by 2
Lee, S., & Kaspi, Y. (2021) · Journal of the Atmospheric Sciences · doi:10.1175/jas-d-20-0342.1 · Cited by 2
Self-citationAtmospheric Dynamics of Giants and Icy Planets
Sánchez-Lavega, A., & Heimpel, M. H. (2018) · Springer eBooks · doi:10.1007/978-3-319-55333-7_51 · Cited by 2
Global climate modelling of Saturn’s atmosphere, Part V: Large-scale vortices
Donnelly, P. T., Spiga, A., Guerlet, S., James, M. K., & Bardet, D. (2024) · Icarus · doi:10.1016/j.icarus.2024.116302 · Cited by 1
“The other is the ‘‘deep-seated’’ dynamo-like model that captures convection through the planet’s molecular envelope (Heimpel et al., 2005; Yano et al., 2005; Kaspi et al., 2009; Heimpel and Gómez Pérez, 2011; Gastine et al., 2014; Heimpel et al., 2016; Cabanes et al., 2017).”
BackgroundSymmetric Instability in a Boussinesq Fluid on a Rotating Planet
Zeng, Y., & Jansen, M. F. (2025) · Journal of Geophysical Research Planets · doi:10.1029/2025je009115 · Cited by 1
“…zonal flow, Equations 6 and 7 yield Equation 9 is similar to the thermal wind balance in a rapidly rotating (geostrophic) fluid (Bire et al., 2022; Kaspi et al., 2009), but here f is modified by the background flow, with the effects of centrifugal force incorporated, thus giving the shear of a…”
Goluskin, D. (2015) · SpringerBriefs in applied sciences and technology · doi:10.1007/978-3-319-23941-5_1 · Cited by 1
Galanti, E., Finocchiaro, S., Kaspi, Y., & IESS, L. (2012) · AGU Fall Meeting Abstracts
Self-citationIs spontaneous generation of baroclinic flows possiblePreprint
Bakas, N. A., & Ioannou, P. J. (2017) · arXiv (Cornell University)
Is spontaneous generation of coherent baroclinic flows possible?Preprint
Bakas, N. A., & Ioannou, P. J. (2017) · arXiv (Cornell University) · doi:10.48550/arxiv.1712.05724
Davighi, J., Kaspi, Y., Galanti, E., & Hubbard, W. B. (2015) · DPS
Self-citationEvidence for Multiple Ferrel-Like Cells on Jupiter
Duer, K., Gavriel, N., Galanti, E., Kaspi, Y., Fletcher, L. N., Guillot, T., Bolton, S. J., Levin, S., Atreya, S. K., Grassi, D., et al. (2022) · doi:10.5194/egusphere-egu22-9155
Self-citationInterior heating drives the formation of clouds on exoplanet gas giantsPreprint
Temel, O., Sert, H., Senel, C. B., Hoolst, T. V., & Karatekin, Ö. (2021) · doi:10.1002/essoar.10509745.1
Numerical Simulations of Magnetic Effects on Zonal Flows in Giant Planets
Xue, S., & Lin, Y. (2024) · Journal of Geophysical Research Planets · doi:10.1029/2023je008280
“…numerical models have been developed to simulate zonal jets driven by rotating convection in thin shells, modeling the hydrodynamics in the molecular envelope (e.g., Aurnou & Olson, 2001; Christensen, 2001; Gastine & Wicht, 2012; Heimpel et al., 2005; Jones & Kuzanyan, 2009; Kaspi et al., 2009).”
Atmospheric Dynamics of Giants and Icy Planets
Sánchez-Lavega, A., & Heimpel, M. H. (2024) · Springer eBooks · doi:10.1007/978-3-319-30648-3_51-2
Dynamics of Jupiter’s equatorial zone: Instability analysis and a mechanism for Y-shaped structures
Rostami, M., Fallah, B., & Fazel-Rastgar, F. (2024) · Icarus (New York, N.Y. 1962) · doi:10.1016/j.icarus.2024.116414
“…depth (despite possible enhancement in the outermost layers, as measured by the Galileo probe), largely due to the fluid’s compressibility (Kaspi et al., 2009), increasing atmospheric density, and potential effects of Ohmic dissipation at these depths, where electrical conductivity begins…”
Jupiter gravity field model estimation based on precision orbit determination of Juno spacecraft
Sun, S., Yan, J., Gao, W., Liu, S., Cao, J., & Barriot, J. (2025) · Zhongguo kexue. Wulixue Lixue Tianwenxue · doi:10.1360/sspma-2025-0013
Peter, T.-J., Michel, V., Suttmeier, F. T., & Wicht, J. (2026) · Inverse Problems · doi:10.1088/1361-6420/ae5553
“Early models of the Jovian atmosphere used the Euler equation in a non-rotating coordinate system as a starting point [6], but today the Euler equation in a rotating reference frame is often used [13, 15, 31, 35].”
InfluentialA Possible Mechanism to Explain the Prograde Equatorial Jet of a Jupiter-like Gaseous Giant
Lian, Y., Duan, P., & Kong, D. (2026) · The Astrophysical Journal Letters · doi:10.3847/2041-8213/ae518c
“In addition, it should be noted that our findings are not inconsistent with the deep atmospheric model, which predicts barotropic fluid columns aligned with the rotation axis, as per the Taylor–Proudman theorem ( K. Zhang & F. Busse 1987; Y. Kaspi et al. 2009 ) .”
Zeng, Y., Kang, W., Flierl, G. R., & Vallis, G. K. (2026) · The Planetary Science Journal · doi:10.3847/psj/ae6da7 · Cited by 1
“…& P. L. Olson 2001; U. R. Christensen 2001, 2002; J.-I. Yano et al. 2005; M. Heimpel et al. 2005; M. Heimpel & J. Aurnou 2007; J. Aurnou et al. 2007; Y. Kaspi et al. 2009; C. A. Jones & K. M. Kuzanyan 2009; K. Soderlund et al. 2013; T. Gastine et al. 2013a,b, 2014; R. K. Yadav et al. 2020, 2022 .”
Self-citationJuno Microwave Radiometer Observations Reveal a Warmer Polar Atmosphere on Jupiter
Hu, J., Li, C., Atreya, S. K., Fletcher, L. N., Galanti, E., Guillot, T., Kaspi, Y., Li, L., Lian, Y., Mura, A., et al. (2026) · The Astrophysical Journal · doi:10.3847/1538-4357/ae6ef5
“If air parcels move freely from depth to the upper layers, their trajectories tend to align with the rotation axis, imprinting angular-momentum structures onto the visible atmosphere (M. Heimpel et al. 2005; Y. Kaspi et al. 2009, 2023).”
Self-citationThe Dynamics of the Atmosphere of Saturn
Sánchez-Lavega, A. (2026) · doi:10.1093/9780197851500.003.0342
Metadata
- Authors
- Kaspi, Y., Flierl, G. R., & Showman, A. P.
- Affiliations
- Massachusetts Institute of Technology (US)
- University of Arizona (US)
- Corresponding author
- Kaspi, Yohai
- Venue
- Icarus
- Publisher
- Elsevier BV
- Published
- 2009-08
- Volume
- 202
- Issue
- 2
- Pages
- 525-542
- ISSN
- 0019-1035 (ISSN-L)
- 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
- Locations
- Icarus (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
- 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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