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Simulation of equatorial and high-latitude jets on Jupiter in a deep convection model
Abstract
The bands of Jupiter represent a global system of powerful winds. Broad eastward equatorial jets are flanked by smaller-scale, higher-latitude jets flowing in alternating directions. Jupiter's large thermal emission suggests that the winds are powered from within, but the zonal flow depth is limited by increasing density and electrical conductivity in the molecular hydrogen-helium atmosphere towards the centre of the planet. Two types of planetary flow models have been explored: shallow-layer models reproduce multiple high-latitude jets, but not the equatorial flow system, and deep convection models only reproduce an eastward equatorial jet with two flanking neighbours. Here we present a numerical model of three-dimensional rotating convection in a relatively thin spherical shell that generates both types of jets. The simulated flow is turbulent and quasi-two-dimensional and, as observed for the jovian jets, simulated jet widths follow Rhines' scaling theory. Our findings imply that Jupiter's latitudinal transition in jet width corresponds to a separation between the bottom-bounded flow structures in higher latitudes and the deep equatorial flows.
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“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 [21]
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“we could simulate it for about 0.1 viscous diffusion time (about 1600 rotations), which is similar to earlier highresolution studies [21, 35].”
From Deep rotating convection generates the polar hexagon on Saturn (2020) · cites this paper as [21]
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“Existing models posit as the driver of the flow either the differential radiative heating of the upper atmosphere (e.g., Williams 1979Williams , 2003b) ) or the intrinsic heat fluxes emanating from the deep interior (e.g., Busse 1976;Heimpel et al. 2005;Aurnou et al. 2007;Chan and Mayr 2008;Kaspi et al. 2009).”
From Mechanisms of Jet Formation on the Giant Planets (2010) · cites this paper as Heimpel et al. 2005
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Citations
Cites
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Novi, L., von Hardenberg, J., Hughes, D. W., Provenzale, A., & Spiegel, E. A. (2019) · Physical review. E · doi:10.1103/physreve.99.053116 · Cited by 29
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Self-citationThe Role of Density Stratification in Generating Zonal Flow Structures in a Rotating Fluid
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Wulff, P., Dietrich, W., Christensen, U. R., & Wicht, J. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac3045 · Cited by 25
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BackgroundNon-Oberbeck–Boussinesq zonal flow generation
Held, M., Wiesenberger, M., Kube, R., & Kendl, A. (2018) · Nuclear Fusion · doi:10.1088/1741-4326/aad28e · Cited by 23
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ON THE VARIATION OF ZONAL GRAVITY COEFFICIENTS OF A GIANT PLANET CAUSED BY ITS DEEP ZONAL FLOWS
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“In models with relatively small viscosity (which can be measured by the Ekman number, the ratio of the rotation period to the global viscous timescale), the zonal flows develop persistent multiple jets of alternating sign inside the tangent cylinder (e.g. Heimpel et al. 2005; Gastine et al. 2014).”
BackgroundA Fully Compressible Nonhydrostatic Deep-Atmosphere Equations Solver for MPAS
Skamarock, W. C., Ong, H., & Klemp, J. B. (2020) · Monthly Weather Review · doi:10.1175/mwr-d-20-0286.1 · Cited by 22
The Role of Density Stratification in Generating Zonal Flow Structures in a Rotating FluidPreprint
Evonuk, M. (2013) · Cited by 22
The Global Atmospheric Circulation of Saturn
Showman, A. P., Ingersoll, A. P., Achterberg, R. K., & Kaspi, Y. (2018) · Cambridge University Press eBooks · doi:10.1017/9781316227220.011 · Cited by 21
The Physical Oceanography of Ice-Covered Moons
Soderlund, K. M., Rovira‐Navarro, M., Bars, M. L., Schmidt, B. E., & Gerkema, T. (2023) · Annual Review of Marine Science · doi:10.1146/annurev-marine-040323-101355 · Cited by 25
Takehiro, S., & Sasaki, Y. (2017) · Physics of The Earth and Planetary Interiors · doi:10.1016/j.pepi.2017.03.001 · Cited by 21
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Garcia, F., Chambers, F. R. N., & Watts, A. L. (2020) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/staa2962 · Cited by 20
“…0.9, are presented in a parameter regime – defined by a Taylor number Ta = 1011 and a Prandtl number Pr = 0.01 – similar to those used previous models developed for the understanding of moderate and low-latitude wind jets observed in giant planets (Heimpel & Aurnou 2007; Heimpel et al. 2005, 2015).”
BackgroundMethodResultInfluentialNumerical simulations of dynamos generated in spherical Couette flows
Guervilly, C., & Cardin, P. (2010) · White Rose Research Online (University of Leeds, The University of Sheffield, University of York) · Cited by 21
Numerical models of zonal flow dynamos: an application to the ice giants
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“Such an azimuthal flow would be expected to exist at the top of the liquid electrolytic envelope if the atmospheric zonal winds extend to great depths in the fluid envelope (Aurnou and Heimpel 2004, Heimpel et al. 2005b, Aurnou et al. 2007, Heimpel and Aurnou 2007).”
BackgroundSelf-citationPlanetary Magnetism as a Parameter in Exoplanet Habitability
McIntyre, S. R. N., Lineweaver, C. H., & Ireland, M. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz667 · Cited by 20
“…Ω, with all three normalized to their corresponding Earth values: F F⊕ = ( ROl ROl⊕ )2 ( D D⊕ )2/3 ( Ω Ω⊕ )7/3 (3) where D = 0.65r0 is the radial extent of the convection cell based on the Heimpel et al. (2005) model for the most efficient dynamo for at least some period of the planet’s lifetime.”
BackgroundExperimental evidence for the boundary zonal flow in rotating Rayleigh–Bénard convection
Wedi, M., Moturi, V. M., Fünfschilling, D., & Weiss, S. (2022) · Journal of Fluid Mechanics · doi:10.1017/jfm.2022.195 · Cited by 20
Constraining the depth of Saturn’s zonal winds by measuring thermal and gravitational signals
Liu, J., Schneider, T., & Fletcher, L. N. (2014) · Icarus · doi:10.1016/j.icarus.2014.05.036 · Cited by 20
Gravitational signature of rotationally distorted Jupiter caused by deep zonal winds
Kong, D., Liao, X., Zhang, K., & Schubert, G. (2013) · Icarus · doi:10.1016/j.icarus.2013.08.016 · Cited by 20
Scaling of Off-Equatorial Jets in Giant Planet Atmospheres
Liu, J., & Schneider, T. (2014) · Journal of the Atmospheric Sciences · doi:10.1175/jas-d-13-0391.1 · Cited by 18
“…in which the energy transfer from eddies to the mean flow extends over great depth (Kaspi et al. 2009), making it necessary to drive the models with very strong energy fluxes if one wants to reproduce the observed scales of eddies and jets in the upper atmosphere (e.g., Heimpel et al. 2005).”
BackgroundA FULLY SELF-CONSISTENT MULTI-LAYERED MODEL OF JUPITER
Kong, D., Zhang, K., & Schubert, G. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/826/2/127 · Cited by 19
“The cases with =H 0.9 and =H 0.95 represent shallow wind models similar to that studied by direct numerical simulations (Heimpel et al. 2005).”
InfluentialDietrich, W., Wulff, P., Wicht, J., & Christensen, U. R. (2021) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stab1566 · Cited by 18
Self-citationLarge-scale-vortex dynamos in planar rotating convection
Guervilly, C., Hughes, D. W., & JONES, C. A. (2017) · Journal of Fluid Mechanics · doi:10.1017/jfm.2017.56 · Cited by 18
“To date, LSVs have not been reported in numerical simulations of rotating convection in spherical geometry; large-scale coherent flows are observed for low Ek and large Re, but these are zonal flows — i.e. axisymmetric and azimuthal jets (e.g. Heimpel et al., 2005; Gastine & Wicht, 2012).”
BackgroundHierarchical Modeling of Solar System Planets with Isca
Thomson, S. I., & Vallis, G. K. (2019) · Atmosphere · doi:10.3390/atmos10120803 · Cited by 18
On the necessary conditions for bursts of convection within the rapidly rotating cylindrical annulus
Teed, R., Jones, C. A., & Hollerbach, R. (2012) · Physics of Fluids · doi:10.1063/1.4711398 · Cited by 17
Non-Oberbeck–Boussinesq zonal flow generation
Held, M., Wiesenberger, M., Kube, R., & Kendl, A. (2018) · Technical University of Denmark, DTU Orbit (Technical University of Denmark, DTU) · Cited by 17
Zonostrophic turbulence in the subsurface oceans of the Jovian and Saturnian moons
Cabanes, S., Gastine, T., & Fournier, A. (2024) · Icarus · doi:10.1016/j.icarus.2024.116047 · Cited by 18
“…the formation of zonal jets has been observed in simulations replicating conditions akin to those found within the Earth’s liquid core (Guervilly and Cardin, 2017) and the deep convective envelope of Jupiter and Saturn (Aurnou and Olson, 2001; Heimpel et al., 2005; Yadav and Bloxham, 2020).”
Quenching of zonal winds in Jupiter’s interior
Christensen, U. R., & Wulff, P. (2024) · Proceedings of the National Academy of Sciences · doi:10.1073/pnas.2402859121 · Cited by 16
Zonal flow reversals in two-dimensional Rayleigh-Bénard convection
Winchester, P., Dallas, V., & Howell, P. D. (2021) · Physical Review Fluids · doi:10.1103/physrevfluids.6.033502 · Cited by 16
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Jupiter’s Red Oval BA: Dynamics, Color, and Relationship to Jovian Climate Change
Marcus, P., Asay‐Davis, X., Wong, M. H., & de Pater, I. (2012) · ASME Journal of Heat and Mass Transfer · doi:10.1115/1.4007666 · Cited by 16
A Global Simulation of the Dynamo, Zonal Jets, and Vortices on Saturn
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“Prior studies (Aurnou & Olson 2001; Christensen 2001; Heimpel et al. 2005; Jones & Kuzanyan 2009; Gastine et al. 2014a; Yadav & Bloxham 2020) investigating the origin of zonal flows in deep spherical shells show that the location of the first westward zonal jet is largely governed by the location…”
BackgroundWeakly non-Boussinesq convection in a gaseous spherical shell
Korre, L., Brummell, N. H., & Garaud, P. (2017) · Physical review. E · doi:10.1103/physreve.96.033104 · Cited by 15
AtmoFlow - Investigation of Atmospheric-Like Fluid Flows Under Microgravity Conditions
Zaussinger, F., Canfield, P., Froitzheim, A., Travnikov, V. V., Haun, P., Meier, M., Meyer, A., Heintzmann, P., Driebe, T. M., & Egbers, C. (2019) · Microgravity Science and Technology · doi:10.1007/s12217-019-09717-7 · Cited by 15
Planetary Core‐Style Rotating Convective Flows in Paraboloidal Laboratory Experiments
Lonner, T. L., Aggarwal, A., & Aurnou, J. M. (2022) · Journal of Geophysical Research Planets · doi:10.1029/2022je007356 · Cited by 17
“The boundary curvature creates Rossby wave-like convective flows that tend to drive energy into coherent zonal (azimuthal) motions (Gastine et al., 2014; Heimpel et al., 2005; Manneville & Olson, 1996).”
BackgroundSelf-citationLinearly forced fluid flow on a rotating sphere
Supekar, R., Heinonen, V., Burns, K. J., & Dunkel, J. (2020) · Journal of Fluid Mechanics · doi:10.1017/jfm.2020.205 · Cited by 14
Galanti, E., & Kaspi, Y. (2017) · Icarus · doi:10.1016/j.icarus.2017.01.004 · Cited by 14
“shown in many studies that strong internal convection can lead to zonally symmetric ows aligned parallel to the axis of rotation (e.g., Aurnou and Olson, 2001; Christensen, 2002; Wicht et al., 2002; Heimpel et al., 2005; Kaspi et al., 2009; Jones and Kuzanyan, 2009; Gastine and Wicht, 2012; Gastine et al., 2013; Chan…”
BackgroundModeling the Interior Dynamics of Gas Planets
Wicht, J., French, M., Stellmach, S., Nettelmann, N., Gastine, T., Duarte, L., & Redmer, R. (2018) · Astrophysics and space science library · doi:10.1007/978-3-319-64292-5_2 · Cited by 13
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Oscillations and Stability of the Jupiter Polar Cyclones
Mura, A., Adriani, A., Bracco, A., Moriconi, M. L., Grassi, D., Plainaki, C., Ingersoll, A. P., Bolton, S. J., Sordini, R., Altieri, F., et al. (2021) · Geophysical Research Letters · doi:10.1029/2021gl094235 · Cited by 14
de Wit, X. M., Boot, W. J. M., Madonia, M., Guzmán, A. J. A., & Kunnen, R. (2023) · Physical Review Fluids · doi:10.1103/physrevfluids.8.073501 · Cited by 13
“Rotating Rayleigh-B´enard convection is the principal source of motion underlying the majority of geophysical and astrophysical flows [1–3].”
BackgroundWulff, P., Christensen, U. R., Dietrich, W., & Wicht, J. (2024) · Journal of Geophysical Research Planets · doi:10.1029/2023je008042 · Cited by 13
“A strong prograde jet flanked by two retrograde jets in the equatorial region, outside the tangent cylinder, were already reproduced in hydrodynamic simulations (Christensen, 2002; Gastine et al., 2014; Heimpel et al., 2005).”
BackgroundSelf-citationAsymptotic scaling relations for rotating spherical convection with strong zonal flows
Nicoski, J. A., O'Connor, A. R., & Calkins, M. A. (2024) · Journal of Fluid Mechanics · doi:10.1017/jfm.2024.78 · Cited by 13
“The number of zonal jets that appear can be related to the Rhines length scale (Rhines 1975; Heimpel et al. 2005; Gastine et al. 2014).”
BackgroundThe turbulent dynamics of Jupiter’s and Saturn’s weather layers: order out of chaos?
Read, P. L., Young, R. M. B., & Kennedy, D. (2020) · Geoscience Letters · doi:10.1186/s40562-020-00159-3 · Cited by 12
Morin, V. M., & Dormy, E. (2006) · Physics of Fluids · doi:10.1063/1.2215605 · Cited by 13
A dynamo driven by zonal jets at the upper surface: Applications to giant planets
Guervilly, C., Cardin, P., & Schaeffer, N. (2011) · Icarus · doi:10.1016/j.icarus.2011.11.014 · Cited by 13
“In the non-magnetic deep convection models (Heimpel et al., 2005; Jones and Kuzanyan, 2009), zonal motions extend geostrophically throughout the electrically insulating molecular hydrogen layer down to the bottom of the model.”
BackgroundMethodThe Dynamics of Jupiter's and Saturn's Weather Layers: A Synthesis After Cassini and Juno
Read, P. L. (2023) · Annual Review of Fluid Mechanics · doi:10.1146/annurev-fluid-121021-040058 · Cited by 12
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Klahr, H. H., Pfeil, T., & Schreiber, A. W. (2018) · Springer eBooks · doi:10.1007/978-3-319-30648-3_138-1 · Cited by 12
Numerical Dynamo Simulations: From Basic Concepts to Realistic Models
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Self-citationTakehiro, S., Yamada, M., & Hayashi, Y. (2007) · Journal of the Atmospheric Sciences · doi:10.1175/2006jas2154.1 · Cited by 12
“Some of the studies have sought their generation and maintenance mechanism in deep convective motion (e.g., Busse 1983; Heimpel et al. 2005), while others have extensively discussed the dynamical properties of two-dimensional fluid motions in a surface thin layer under the influence of rotation and stratification in r…”
BackgroundKaspi, Y. (2008) · doi:10.1575/1912/2492 · Cited by 12
“Previous attempts to model this system fall into two general categories: convection models with deep geometry that are limited to Boussinesq dynamics (e.g. Zhang and Schubert, 1997; Aurnou and Olson, 2001; Christensen, 2002; Heimpel et al., 2005), or spherical shell atmospheric type models which lack or parametrize th…”
BackgroundMethodCONVECTIVE BURSTS AND THE COUPLING OF SATURN'S EQUATORIAL STORMS AND INTERIOR ROTATION
Heimpel, M. H., & Aurnou, J. M. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/746/1/51 · Cited by 11
“He fluid that envelops the metallic interior (e.g., Jones & Kuzanyan 2009; Kaspi et al. 2009; Heimpel et al. 2005; Yano et al. 2003; Busse 1976; cf. Schneider & Liu 2009; Lian & Showman 2008; Showman et al. 2006).”
BackgroundSelf-citationRossby Waves and Jets in Two-Dimensional Decaying Turbulence on a Rotating Sphere
Hayashi, Y., Nishizawa, S., Takehiro, S., Yamada, M., Ishioka, K., & Yoden, S. (2007) · Journal of the Atmospheric Sciences · doi:10.1175/2007jas2209.1 · Cited by 11
“Heimpel et al. (2005) shows that, in addition to the westward flow around the equator, a banded structure of zonal flows caused by the (cid:2) effect appears in the mid-and high latitudes inside of the tangent cylinder.”
BackgroundGas Giant Simulations of Eddy‐Driven Jets Accompanied by Deep Meridional Circulation
Duer, K., Galanti, E., & Kaspi, Y. (2023) · AGU Advances · doi:10.1029/2023av000908 · Cited by 10
“Deep, convection-driven, 3D simulations can produce alternating jets, but the meridional circulation and the eddy momentum fluxes are rarely addressed and analyzed in such setups (e.g., Aurnou & Olson, 2001; Christensen, 2001; Christensen, 2002; Heimpel et al., 2005, 2016, 2022).”
BackgroundGlobal climate modeling of the Jupiter troposphere and effect of dry and moist convection on jets
Boissinot, A., Spiga, A., Guerlet, S., Cabanes, S., & Bardet, D. (2024) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202245220 · Cited by 10
Thermal boundary layer structure in convection with and without rotation
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“Thermally driven flows are important in many industrial and natural settings including metal production [1], planetary atmospheres [2], solar and stellar bodies [3], and Earth’s liquid metal outer core [4].”
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Critical Prandtl Number for Heat Transfer Enhancement in Rotating Convection
Anas, M., & Joshi, P. (2024) · Physical Review Letters · doi:10.1103/physrevlett.132.034001 · Cited by 9
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Temperature fluctuations and heat transport in partitioned supergravitational thermal turbulence
Wang, D., Liu, J., Lai, R., & Sun, C. (2024) · Acta Mechanica Sinica · doi:10.1007/s10409-023-23405-x · Cited by 8
Multiple heat transport maxima in confined-rotating Rayleigh–Bénard convection
Hartmann, R. A., Verzicco, R., Kranenbarg, L. K., Lohse, D., & Stevens, R. J. A. M. (2022) · Journal of Fluid Mechanics · doi:10.1017/jfm.2021.1031 · Cited by 8
Investigating 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
“Since then, three-dimensional numerical simulations of convection in spherical shells have found that the flow organizes itself into broad and deep zonal jets whose axes are approximately parallel to the rotation axis (Christensen, 2001; Aurnou & Olson, 2001; Heimpel et al., 2005; Jones & Kuzanyan, 2009; Gastine et al…”
BackgroundInfluentialTransport and instability in driven two-dimensional magnetohydrodynamic flows
Durston, S., & Gilbert, A. D. (2016) · Journal of Fluid Mechanics · doi:10.1017/jfm.2016.361 · Cited by 7
Polar waves and chaotic flows in thin rotating spherical shells
Garcia, F., Chambers, F. R. N., & Watts, A. L. (2019) · Physical Review Fluids · doi:10.1103/physrevfluids.4.074802 · 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
“The model can also successfully reproduce benchmark results from other MHD models (e.g., MagIC, Calypso) for Jupiter‐like gaseous planets (Christensen, 2001; Heimpel et al., 2005, 2016; Jones et al., 2011).”
ResultReversal and amplification of zonal flows by boundary enforced thermal wind
Dietrich, W., Gastine, T., & Wicht, J. (2016) · Icarus · doi:10.1016/j.icarus.2016.09.013 · Cited by 7
“Reynolds stress is sometimes described as a cascade from smaller to larger scales that stops at the Rhines scale where convective eddies start to feel the Coriolis force (Heimpel et al., 2005; Gastine et al., 2014a).”
BackgroundSelf-citationZhang, K., Kong, D., & Schubert, G. (2017) · Annual Review of Earth and Planetary Sciences · doi:10.1146/annurev-earth-063016-020305 · Cited by 7
Kong, D., Zhang, K., & Schubert, G. (2019) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stz2019 · Cited by 7
Contributions 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).”
BackgroundThe Compressional Beta Effect: Analytical Solution, Numerical Benchmark, and Data Analysis
Ong, H., & Roundy, P. E. (2020) · Journal of the Atmospheric Sciences · doi:10.1175/jas-d-20-0124.1 · Cited by 9
“Research about effects of NCTs on wave propagation began with a focus on the interior of stars and giant planets, and the following two important effects have been identified: topographic beta-effect (e.g., Busse 1994; Gerkema et al. 2008; Heimpel et al. 2005; Yano 1998) and compressional beta-effect (e.”
BackgroundFive Years of Observations of the Circumpolar Cyclones of Jupiter
Mura, A., Scarica, P., Grassi, D., Adriani, A., Bracco, A., Piccioni, G., Sindoni, G., Moriconi, M. L., Plainaki, C., Ingersoll, A. P., et al. (2022) · Journal of Geophysical Research Planets · doi:10.1029/2022je007241 · Cited by 7
“They classify these models into two broad classes: “deep” (i.e., Cai et al., 2021; Garcia et al., 2020; Heimpel et al., 2005, 2016) and “shallow” (i.e., Gavriel & Kaspi, 2021; Li et al., 2020; Reinaud, 2019; Reinaud & Dritschel, 2019).”
Wang, Q., Goluskin, D., & Lohse, D. (2023) · Journal of Fluid Mechanics · doi:10.1017/jfm.2023.875 · Cited by 7
EQUATORIAL ZONAL JETS AND JUPITER's GRAVITY
Kong, D., Liao, X., Zhang, K., & Schubert, G. (2014) · The Astrophysical Journal Letters · doi:10.1088/2041-8205/791/2/l24 · Cited by 7
“…winds are powered by internal heat via thermal convection, but they are confined within the planet’s outermost thin shell, about 10% of Jupiter’s radius (Heimpel et al. 2005), because the effect of magnetic braking by the Jovian magnetic field limits their depth of penetration (Liu et al. 2008).”
Dynamo Models for Planets Other Than Earth
Stanley, S., & Glatzmaier, G. A. (2009) · Space sciences series of ISSI · doi:10.1007/978-1-4419-5901-0_19 · Cited by 8
Interaction of Magnetic Field and Flow in the Outer Shells of Giant Planets
Liu, J. (2006) · CaltechTHESIS (California Institute of Technology) · doi:10.7907/4pvm-0g30 · Cited by 7
The onset of zonal modes in two-dimensional Rayleigh–Bénard convection
Winchester, P., Howell, P. D., & Dallas, V. (2022) · Journal of Fluid Mechanics · doi:10.1017/jfm.2022.185 · Cited by 7
“Large-scale zonal flow in buoyancy-driven convection has been found in the atmosphere of Jupiter (Heimpel, Aurnou & Wicht 2005; Kaspi et al. 2018; Kong, Zhang & Schubert 2018), the Earth’s oceans (Maximenko, Bang & Sasaki 2005; Nadiga 2006; Richards et al. 2006), nuclear fusion devices (Diamond et al. 2005; Fujisawa 2…”
BackgroundEffects of rough surfaces on annular centrifugal Rayleigh–Bénard convection
Xu, F., Zhong, J., Su, J., Zhao, B., He, Y., Sun, C., & Wang, J. (2024) · International Journal of Heat and Mass Transfer · doi:10.1016/j.ijheatmasstransfer.2024.125929 · Cited by 6
Huang, M., & He, X. (2022) · Journal of Turbulence · doi:10.1080/14685248.2022.2128360 · Cited by 6
“The zonal flow can also be observed in the atmosphere of Jupiter [19, 20], and in the toroidal plasmas [21].”
BackgroundDirect 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
Self-citationBoundary layer control of rotating convection
King, E. M., Stellmach, S., Noir, J., Hansen, U., & Aurnou, J. M. (2009) · Cited by 6
Self-citationNumerical Dynamo Simulations: From Basic Concepts to Realistic Models
Wicht, J., Stellmach, S., & Harder, H. (2010) · Springer eBooks · doi:10.1007/978-3-642-01546-5_16 · Cited by 6
Self-citationTowards enhanced performance in fusion plasmas via turbulence suppression by MeV ionsPreprint
Mazzi, S., Garcia, J., Zarzoso, D., Kazakov, Y. O., Ongena, J., Nocente, M., Dreval, M., Štancar, Ž., Szepesi, G. L., Eriksson, J., et al. (2020) · arXiv (Cornell University) · doi:10.48550/arxiv.2010.07977 · Cited by 6
“, the famous belts of Jupiter [20].”
Qin, S., Kong, D., Zhang, K., Schubert, G., & Huang, Y. H. (2020) · The Astrophysical Journal · doi:10.3847/1538-4357/ab6a9a · Cited by 5
Li, W., & Kong, D. (2022) · Physical Review Fluids · doi:10.1103/physrevfluids.7.103502 · Cited by 5
Jupiter's occultation radii: Implications for its internal dynamics
Helled, R. (2011) · Geophysical Research Letters · doi:10.1029/2011gl047107 · Cited by 5
The effect of the equatorially symmetric zonal winds of Saturn on its gravitational field
Kong, D., Zhang, K., Schubert, G., & Anderson, J. D. (2018) · Research in Astronomy and Astrophysics · doi:10.1088/1674-4527/18/4/39 · Cited by 5
Saturn’s Magnetic Field and Dynamo
Christensen, U. R., Cao, H., Dougherty, M. K., & Khurana, K. K. (2018) · Cambridge University Press eBooks · doi:10.1017/9781316227220.004 · Cited by 5
The spontaneous breaking of axisymmetry in shallow rotating flows
Antar, G. Y., Lalti, A., & Habchi, C. (2019) · Physics of Fluids · doi:10.1063/1.5098367 · Cited by 5
Three-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
Metadata
- Authors
- Heimpel, M., Aurnou, J., & Wicht, J.
- Affiliations
- University of Alberta (CA)
- University of California, Los Angeles (US)
- Max Planck Society (DE)
- Corresponding author
- Heimpel, Moritz
- Venue
- Nature
- Published
- 2005-11
- Volume
- 438
- Issue
- 7065
- Pages
- 193-196
- ISSN
- 0028-0836 (ISSN-L)
- 1476-4687
- OpenAlex
- W1984695169
- Cited by
- 291
- References
- 30
- Citations by year
- 2026: 7 · 2025: 7 · 2024: 20 · 2023: 9 · 2022: 17 · 2021: 11 · 2020: 27 · 2019: 11 · 2018: 38 · 2017: 14 · 2016: 9 · 2015: 12 · 2014: 12 · 2013: 13 · 2012: 9
- FWCI
- 6.59
- Type
- journal article
- Language
- en
- Open access
- closed
- Licence
- www.springer.com/tdm (tdm)
- Locations
- Nature (publishedVersion)
- PubMed (publishedVersion)
- RePEc: Research Papers in Economics (submittedVersion)
- Max Planck Institute for Plasma Physics (submittedVersion)
- eScholarship (California Digital Library) (submittedVersion)
- Max Planck Digital Library (submittedVersion)
- MPG.PuRe (Max Planck Society) (submittedVersion)
- Funders
- Western Canada Research Grid
- Deutsche Forschungsgemeinschaft
- Natural Sciences and Engineering Research Council of Canada
- Topics
- Physical Sciences › Earth and Planetary Sciences › Space and Planetary Science › Astro and Planetary Science
- Physical Sciences › Engineering › Computational Mechanics › Fluid Dynamics and Turbulent Flows
- Physical Sciences › Physics and Astronomy › Astronomy and Astrophysics › Stellar, planetary, and galactic studies
- Keywords
- Jupiter, equatorial jet, zonal wind, atmospheric bands, deep convection, rotating convection, spherical shell, turbulent flow, three-dimensional numerical model
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