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A simple model of convection in the Jovian atmosphere
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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 [18]
In the citing paper
“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 Busse 1976
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 Busse 1976
Citations
Cites
Hydrodynamic and Hydromagnetic Stability
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Cited by
Sorted by citations
Items 101–200 of 278
Predictions of thermal and gravitational signals of Jupiter’s deep zonal winds
Liu, J., Schneider, T., & Kaspi, Y. (2013) · Icarus · doi:10.1016/j.icarus.2013.01.025 · Cited by 32
“Because the Rossby number is small and viscous momentum dissipation and thermal diffusion are negligible, convective motions are approximately aligned with surfaces of constant planetary angular momentum, which are cylinders concentric with the planet’s spin axis (Busse 1976; Kaspi et al. 2009).”
InfluentialKaspi, Y., Davighi, J., Galanti, E., & Hubbard, W. B. (2016) · Icarus · doi:10.1016/j.icarus.2016.04.001 · Cited by 30
“…consistent with the observed flows on all four gi- nt planets ( Lian and Showman, 2010; Liu and Schneider, 2010 ). he alternative approach suggests that the observed jets are the urface manifestation of convective columns originating from the ot interiors of the giant planets ( Busse, 1976, 1994 ).”
BackgroundThe effect of differential rotation on Jupiter's low‐degree even gravity moments
Kaspi, Y., Guillot, T., Galanti, E., Miguel, Y., Helled, R., Hubbard, W. B., Militzer, B., Wahl, S. M., Levin, S., Connerney, J. E. P., et al. (2017) · Geophysical Research Letters · doi:10.1002/2017gl073629 · Cited by 31
“If the fluid would have been completely barotropic, this would result in the zonal flow being constant along the direction of the spin axis [e.g., Busse, 1976; Hubbard, 1999].”
BackgroundThree-dimensional convection driven by centrifugal buoyancy
Auer, M., Busse, F. H., & Clever, R. M. (1995) · Journal of Fluid Mechanics · doi:10.1017/s0022112095003934 · Cited by 31
Self-citationGalanti, E., & Kaspi, Y. (2016) · The Astrophysical Journal · doi:10.3847/0004-637x/820/2/91 · Cited by 29
“…lasting debate regarding the depth of the dynamics on the giant planets, and thus shed light on the mechanisms the could be driving the jets (e.g., Busse 1976; Williams 1978; Cho and Polvani 1996; Showman et al. 2006; Scott and Polvani 2007; Kaspi and Flierl 2007; Lian and Showman 2010; Liu and…”
BackgroundKang, C., Meyer, A., Yoshikawa, H. N., & Mutabazi, I. (2019) · Physical Review Fluids · doi:10.1103/physrevfluids.4.043501 · Cited by 29
Catling, D. C. (2015) · Elsevier eBooks · doi:10.1016/b978-0-444-53802-4.00185-8 · Cited by 30
Rotvig, J., & JONES, C. A. (2006) · Journal of Fluid Mechanics · doi:10.1017/s0022112006002254 · Cited by 27
“It remains an open problem whether the zonal flows are confined to a thin layer in the top few hundred kilometres of the planet or extend deep into the interior as suggested by Busse (1976).”
BackgroundJet streams and tracer mixing in the atmospheres of brown dwarfs and isolated young giant planets
Tan, X. (2022) · Monthly Notices of the Royal Astronomical Society · doi:10.1093/mnras/stac344 · Cited by 27
Dynamo Simulations of Jupiter's Magnetic Field: The Role of Stable Stratification and a Dilute Core
Moore, K. M., Barik, A., Stanley, S., Stevenson, D. J., Nettelmann, N., Helled, R., Guillot, T., Militzer, B., & Bolton, S. J. (2022) · Journal of Geophysical Research Planets · doi:10.1029/2022je007479 · Cited by 25
“Historically, fluid dynamical theories of Jupiter's zonal winds have fallen into two main camps—(a) that the winds extend geostrophically deep into the planet along so-called Taylor Columns (Busse, 1976), or (b) that the surface winds could be considered a shallower “weather layer” due to effects such as variable sola…”
BackgroundMarcus, P., & Shetty, S. (2011) · Philosophical Transactions of the Royal Society A Mathematical Physical and Engineering Sciences · doi:10.1098/rsta.2010.0299 · Cited by 25
Convection-driven zonal flows in the major planets
Busse, F. H. (1983) · Pure and Applied Geophysics · doi:10.1007/bf02590147 · Cited by 25
Self-citationSun, Z.-P., & Schubert, G. (1995) · Physics of Fluids · doi:10.1063/1.868716 · Cited by 24
Probing the depth of Jupiter’s Great Red Spot with the Juno gravity experiment
Parisi, M., Galanti, E., Finocchiaro, S., IESS, L., & Kaspi, Y. (2015) · Icarus · doi:10.1016/j.icarus.2015.12.011 · Cited by 23
ON THE VARIATION OF ZONAL GRAVITY COEFFICIENTS OF A GIANT PLANET CAUSED BY ITS DEEP ZONAL FLOWS
Kong, D., Zhang, K., & Schubert, G. (2012) · The Astrophysical Journal · doi:10.1088/0004-637x/748/2/143 · 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
Deep model simulation of polar vortices in gas giant atmospheres
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
“…the jets in a thin atmospherical layer (Liu & Schneider 2010; Morales-Juberı́as et al. 2015; Rostami, Zeitlin & Spiga 2017); or a deep scenario (Busse 1976; Heimpel, Aurnou & Wicht 2005; Heimpel & Aurnou 2007; Heimpel, Gastine & Wicht 2015) in which the jets form quasigeotrophic columns…”
BackgroundBusse, F. H., & Finocchi, F. (1993) · Physics of The Earth and Planetary Interiors · doi:10.1016/0031-9201(93)90069-l · Cited by 21
Self-citationDeep two-dimensional turbulence: An idealized model for atmospheric jets of the giant outer planets
Yano, J., Talagrand, O., & Drossart, P. (2005) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091920412331336398 · Cited by 21
“The second possibility is deep dynamics which extends to the whole fluid–gas layer of the planets and is driven by internal heat sources (e.g. Busse, 1976, 1983, 1994).”
BackgroundRetrieval of a Wind Profile from the Galileo Probe Telemetry Signal
Pollack, J. B., Atkinson, D. H., SEIFF, A., & Anderson, J. D. (1992) · Springer eBooks · doi:10.1007/978-94-011-2512-3_6 · Cited by 21
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
“…and their associated heat transport are predominantly confined to surfaces of constant angular momentum per unit mass, which are approximately cylinders concentric with the planet’s spin axis (Busse, 1976, 1994; Christensen, 2001; Heimpel et al., 2005; Aurnou et al., 2008; Kaspi et al., 2009).”
BackgroundGravitational 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
Constraints on the Latitudinal Profile of Jupiter's Deep Jets
Galanti, E., Kaspi, Y., Duer, K., Fletcher, L. N., Ingersoll, A. P., Li, C., Orton, G. S., Guillot, T., Levin, S., & Bolton, S. J. (2021) · Geophysical Research Letters · doi:10.1029/2021gl092912 · Cited by 20
“…has been assumed to be projected into the planet interior along the direction parallel to the spin axis of Jupiter, based on theoretical arguments (Busse, 1970, 1976) and 3D simulations of the flow in a Jovian-like planet (e.g., Busse, 1994; Christensen, 2001; Heimpel et al., 2016; Kaspi…”
BackgroundDynamical Consequences of Orthohydrogen-Parahydrogen Disequilibrium on Jupiter and Saturn
Gierasch, P. J. (1983) · Science · doi:10.1126/science.219.4586.847 · Cited by 20
The Range of Jupiter's Flow Structures That Fit the Juno Asymmetric Gravity Measurements
Duer, K., Galanti, E., & Kaspi, Y. (2020) · Journal of Geophysical Research Planets · doi:10.1029/2019je006292 · Cited by 19
“Taking a hierarchal approach, with an increasing level of complexity, we first use the observed cloud-level wind as an upper boundary condition for the flow field and assume the same profile continues inward in a direction parallel to the spin axis, due to angular momentum considerations (Busse, 1976; Kaspi et al., 20…”
MethodOn 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
Condie, S. A., & Rhines, P. B. (1994) · Journal of Fluid Mechanics · doi:10.1017/s002211209400296x · Cited by 17
Saturn meteorology: A diagnostic assessment of thin-layer configurations for the zonal flow
Allison, M., & Stone, P. H. (1983) · Icarus · doi:10.1016/0019-1035(83)90199-9 · Cited by 17
Atmospheric waves and dynamics beneath Jupiter’s clouds from radio wavelength observations
Cosentino, R., Butler, B. J., Sault, R. J., Morales-Juberías, R., Simon, A. A., & de Pater, I. (2017) · Icarus · doi:10.1016/j.icarus.2017.01.006 · Cited by 16
Characteristic zonal winds and long-lived vortices in the atmospheres of the outer planets
Beebe, R. F. (1994) · Chaos An Interdisciplinary Journal of Nonlinear Science · doi:10.1063/1.165998 · Cited by 16
The upscale turbulent cascade Shear layers, cyclones and gas giant bands
Peltier, W. R., & Stuhne, G. R. (2002) · International geophysics/International geophysics series · doi:10.1016/s0074-6142(02)80156-5 · Cited by 16
A Global Simulation of the Dynamo, Zonal Jets, and Vortices on Saturn
Yadav, R. K., Cao, H., & Bloxham, J. (2022) · The Astrophysical Journal · doi:10.3847/1538-4357/ac9d94 · Cited by 15
“This idea was put forth by Busse (1976) and has been extensively explored in many numerical simulation studies (e.g., Aurnou & Olson 2001; Christensen 2001; Heimpel et al. 2005; Jones & Kuzanyan 2009; Kaspi et al. 2009; Gastine et al. 2014a; Yadav & Bloxham 2020).”
BackgroundTakehiro, S., & Lister, J. R. (2002) · Geophysical Research Letters · doi:10.1029/2002gl015450 · Cited by 15
Galanti, E., & Kaspi, Y. (2017) · Icarus · doi:10.1016/j.icarus.2017.01.004 · Cited by 14
“howman, 2010; Liu and Schneider, 2010). The second approach assumes that the observed cloud-level ow is a surface manifestation of convective columns originating from the hot interiors of the planet (Busse, 1976, 1994). Angular momentum conservation in a rapidly rotating planet like Jupiter leads the ow to be aligned…”
BackgroundBolton, S. J., Lunine, J. I., Stevenson, D. J., Connerney, J. E. P., Levin, S., Owen, T., Bagenal, F., Gautier, D., Ingersoll, A. P., Orton, G. S., et al. (2017) · Springer eBooks · doi:10.1007/978-94-024-1560-5_2 · 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
“The second class of models is deep convection models which simulate most or all of the whole 104km-thick molecular hydrogen layer (Busse, 1976; Christensen, 2001, 2002; Manneville and Olson, 1996).”
BackgroundSlantwise convection on fluid planets
O’Neill, M. E., & Kaspi, Y. (2016) · Geophysical Research Letters · doi:10.1002/2016gl071188 · Cited by 13
Thermal convection in a rotating shear flow
Hathaway, D. H., & Somerville, R. C. J. (1987) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091928708210105 · Cited by 13
D‐D Fusion in the Interior of Jupiter?
Ouyed, R., Fundamenski, W., Cripps, G., & Sutherland, P. G. (1998) · The Astrophysical Journal · doi:10.1086/305797 · Cited by 13
“(2) These models cannot explain the strong magnetic Ðeld at the planet surface, as well as its high multipoles, measured by Pioneer 10 and Pioneer 11 & Ness(Busse 1976 ; Acun8 a & Salpeter argued that the Coriolis1976).”
BackgroundCao, H., Bloxham, J., Park, R. S., Militzer, B., Yadav, R. K., Kulowski, L., Stevenson, D. J., & Bolton, S. J. (2023) · The Astrophysical Journal · doi:10.3847/1538-4357/ad0cbb · Cited by 12
The Nontraditional Coriolis Terms and Tropical Convective Clouds
Igel, M. R., & Biello, J. A. (2020) · Journal of the Atmospheric Sciences · doi:10.1175/jas-d-20-0024.1 · Cited by 12
Instability of Zonal Flows in Rotating Spherical Shells: An Application to Jupiter
Wicht, J. (2002) · Icarus · doi:10.1006/icar.2001.6733 · Cited by 12
Deep Convection in the Interior of Major Planets: A Review
Yano, J. (1998) · Australian Journal of Physics · doi:10.1071/p97079 · Cited by 12
“Busse (1976) originally hypothesised that such deep thermal convection drives and maintains the dominant zonal winds (i.e. longitudinally-directed winds) observed at the cloud-level of the atmosphere, and q CSIRO 1998 0004-9506/98/050875$05.00 this hypothesis was later endorsed by Ingersoll and…”
BackgroundInfluentialKaspi, Y. (2008) · doi:10.1575/1912/2492 · Cited by 12
“In Busse's original heuristic picture (Busse, 1976) for multiple zonal jets driven by interaction between cylinders, he suggested that multiple columns at di erent radii from the center may interact to cause alternating jets.”
BackgroundMethodInfluentialCONVECTIVE 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).”
BackgroundJuarez, M. D. L. T., Fisher, B. M., & Orton, G. S. (2002) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091920290027943 · Cited by 11
Ingersoll, A. P., Dobrovolskis, A. R., & JAKOSKY, B. M. (1979) · Reviews of Geophysics · doi:10.1029/rg017i007p01722 · Cited by 11
Gas 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
“In the slices, the cylindrical orientation of the flow at all latitudes is visible, due to the fast rotation used in this simulation (Busse, 1976; Busse & Hood, 1982), and consistent with recent observations indicating the cylindrical nature of the zonal flows on Jupiter (Kaspi et al., 2023).”
BackgroundResultRotvig, J. (2007) · Physical Review E · doi:10.1103/physreve.76.046306 · Cited by 10
Fitzgerald, J. G., & Farrell, B. F. (2018) · Journal of the Atmospheric Sciences · doi:10.1175/jas-d-18-0075.1 · Cited by 9
“edu hypothesized to originate in the planetary interior, such as the production of differential rotation by deep columnar convection (Busse 1976), have also been advanced to explain Jupiter’s jets.”
BackgroundSimulating 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
“For a detailed discussion on how these two mechanisms work see: Busse (1976), Glatzmaier and Evonuk (2006), Glatzmaier et al.”
BackgroundDynamics of Jupiter's atmosphere
SEIFF, A. (2000) · Nature · doi:10.1038/35001171 · Cited by 9
Transition to Asymmetric Convection Rolls
Busse, F. H. (1987) · Birkhäuser Basel eBooks · doi:10.1007/978-3-0348-7241-6_3 · Cited by 9
Self-citationTwo-dimensional partially ionized magnetohydrodynamic turbulence
Benavides, S., & Flierl, G. R. (2020) · Journal of Fluid Mechanics · doi:10.1017/jfm.2020.500 · Cited by 9
“This includes, among many other things, the formation, characteristics and dynamics of the jets and vortices (Rhines 1975; Busse 1976; Dowling & Ingersoll 1988, 1989; Cho & Polvani 1996; Showman 2007; Scott & Polvani 2007, † Email address for correspondence: santib@mit.edu 2008; Liu et al. 2008;…”
BackgroundInvestigating 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
“Busse (1976) originally proposed that Jupiter's observed surface zonal winds are the surface manifestations of deep zonal flow generated by tilted cylindrical convection columns.”
BackgroundInfluentialTobias, S. M., Oishi, J. S., & Marston, J. B. (2018) · Proceedings of the Royal Society A Mathematical Physical and Engineering Sciences · doi:10.1098/rspa.2018.0422 · Cited by 8
Acoustic and inertial modes in planetary-like rotating ellipsoids
Vidal, J., & Cébron, D. (2020) · Proceedings of the Royal Society A Mathematical Physical and Engineering Sciences · doi:10.1098/rspa.2020.0131 · Cited by 8
“The observed zonal winds at Jupiter’s surface could also be related to deep geostrophic flows [75,76], but different physical scenarios are highly disputed in light of recent high-precision data [77–79].”
BackgroundAnelastic torsional oscillations in Jupiter's metallic hydrogen region
Hori, K., Teed, R., & JONES, C. A. (2019) · Earth and Planetary Science Letters · doi:10.1016/j.epsl.2019.04.042 · Cited by 8
“The surface zonal flows may extend deep into the interior (e.g. Busse, 1976; Jones and Kuzanyan, 2009; Heimpel et al., 2016).”
BackgroundOrigin of the Solar System and its elements
Manuel, O. K., Lee, J. T., Ragland, D. E., MacElroy, J. M. D., Li, B., & Brown, W. K. (1998) · Journal of Radioanalytical and Nuclear Chemistry · doi:10.1007/bf02385384 · Cited by 8
Magnetic reversals of Jupiter and Saturn
Hathaway, D. H., & Dessler, A. J. (1986) · Icarus · doi:10.1016/0019-1035(86)90177-6 · 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
“These cyl-inders are tilted in the direction of rotation and, hence, transfer positive momentum outward, driving the equatorial zonal flows (e.g., Busse, 1976, 1982, 2002; Zhang & Busse, 1987).”
BackgroundResultInfluentialReversal 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
“Since the pioneering work on the rotating annulus by Busse (1976); Busse and Hood (1982), it is known that the boundary curvature directly controls the tilt direction of the convective columns and therefore sets the direction of zonal flows; the equatorial jet is always bound to be prograde unless…”
BackgroundZhang, 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).”
BackgroundEQUATORIAL 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
“The first is that they are generated by thermal convection, partly powered by internal heat, which takes place within the deep interior of 4 Corresponding Author. the planet (Busse 1976).”
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
“On a larger scale, it has been long debated whether Jupiter’s strong zonal winds that are visible at the cloud level are shallow or deep (Busse, 1976; Ingersoll and Pollard, 1982; Vasavada and Showman, 2005).”
BackgroundRadiative–Convective Latitudinal Gradients for Jupiter and Saturn Models with a Radiative Zone
Gierasch, P. J. (1999) · Icarus · doi:10.1006/icar.1999.6193 · Cited by 7
Chaotic transitions of convection rolls in a rapidly rotating annulus
Or, A. C. (1994) · Journal of Fluid Mechanics · doi:10.1017/s0022112094000224 · Cited by 7
Yano, J. (1987) · Journal of the Meteorological Society of Japan Ser II · doi:10.2151/jmsj1965.65.3_313 · Cited by 7
Double column instabilities in the barotropic annulus
Lin, R. Q. (1990) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091929008208937 · Cited by 7
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
Small-scale and large-scale dynamos in global convection simulations of solar-like stars
Warnecke, J., Korpi, M. J., Rheinhardt, M., Viviani, M., & Prabhu, A. (2025) · Astronomy and Astrophysics · doi:10.1051/0004-6361/202451085 · Cited by 6
Wind-induced odd gravitational harmonics of Jupiter
Kong, D., Zhang, K., & Schubert, G. (2015) · Monthly Notices of the Royal Astronomical Society Letters · doi:10.1093/mnrasl/slv036 · Cited by 6
Jupiter's Turbulent Power Spectra From Hubble Space Telescope
Cosentino, R., Simon, A. A., & Morales-Juberías, R. (2019) · Journal of Geophysical Research Planets · doi:10.1029/2018je005762 · Cited by 6
Liao, X., Zhang, K., & Feng, T. (2005) · The Astrophysical Journal · doi:10.1086/432368 · Cited by 6
“Fast zonal flows and giant stable vortices in major planets such as Jupiter are thought to be driven and maintained by convective instabilities (Busse 1976; Aurnou & Olson 2001; Jones et al. 2003; Aubert et al. 2003).”
BackgroundA shallow convective model for Jupiter's alternating wind bands
Chan, K. L., & Mayr, H. G. (2008) · Journal of Geophysical Research Atmospheres · doi:10.1029/2008je003124 · Cited by 6
Baroclinic Model of Jupiter’s Great Red Spot
Suetin, B. P., Zhmur, V. V., & Chkhetiani, О. G. (2023) · Izvestiya Atmospheric and Oceanic Physics · doi:10.1134/s0001433823030088 · Cited by 5
“The convective nature of flows on Jupiter and other giant planets was proposed in (Busse, 1976, 1994) and (Keller, Yavorskaya 1974; Yavorskaya and Belyaev, 1982).”
BackgroundChachan, Y., & Stevenson, D. J. (2019) · Icarus · doi:10.1016/j.icarus.2018.12.020 · Cited by 5
“Cloud-top motion extended deep into the planet as flows on cylinders (Busse, 1976) is plausible provided the cylinders are external to the electrically conducting region.”
BackgroundLi, 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
“, Busse, 1976; Heimpel et al., 2005; Heimpel and Aurnou, 2007] suggest that the bottom boundary of the deep convection is at about 0.9 RJ (RJ is the radius of Jupiter). Liu et al. [2008] discuss the importance of Lorentz forces in constraining the depth of the Jovian circulation.”
BackgroundInfluentialThe 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
Low-dimensional dynamo modelling and symmetry-breaking bifurcations
Donner, R. V., Norbert Seehafer, B., Sanjuán, M. A. F., & Feudel, F. (2006) · Physica D Nonlinear Phenomena · doi:10.1016/j.physd.2006.08.022 · Cited by 5
“The roll pattern resembles columnar convection structures in rotating spherical shells [28,29] as have been observed by space-craft missions in the”
BackgroundStability of plane parallel shear flow in a rotating layer heated from below
Kaiser, R., & von Wahl, W. (1998) · Calculus of Variations and Partial Differential Equations · doi:10.1007/s005260050090 · Cited by 5
Flat rotation curves according to the fragmentation/shear flow model of galaxy formation
Brown, W. K. (1984) · Astrophysics and Space Science · doi:10.1007/bf00651212 · Cited by 5
One-dimensional dynamics of zonal jets on rapidly rotating spherical shells
Stuhne, G. R. (2001) · Physica D Nonlinear Phenomena · doi:10.1016/s0167-2789(00)00180-9 · 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
“Convection-driven equatorial jet formation has been extensively studied and modeled in the past [e.g., ( 46,47 )].”
The Westward Drift of Jupiter's Polar Cyclones Explained by a Center‐of‐Mass Approach
Gavriel, N., & Kaspi, Y. (2023) · Geophysical Research Letters · doi:10.1029/2023gl103635 · Cited by 4
“This is in agreement with the small Rossby number near the poles, suggesting the 2D Taylor-Proudman theorem regime (Busse, 1976; Vallis, 2017).”
ResultA rapidly time-varying equatorial jet in Jupiter’s deep interior
Bloxham, J., Cao, H., Stevenson, D. J., Connerney, J. E. P., & Bolton, S. J. (2024) · Nature · doi:10.1038/s41586-024-07046-3 · Cited by 4
“If steady, it would probably be a manifestation of deep dynamo convective flow (and jets are anticipated as part of that flow 4–9 ) but if time dependent on a timescale much shorter than the convective turnover timescale of several hundred years, it would probably have a different origin.”
BackgroundEddy-driven Zonal Jet Flows in the Laboratory
Read, P. L., Afanasyev, Y. D., Aurnou, J. M., & Lemasquerier, D. (2024) · Comptes Rendus Physique · doi:10.5802/crphys.213 · Cited by 5
Yamazaki, Y. H., & Read, P. L. (2006) · Advances in Space Research · doi:10.1016/j.asr.2006.03.025 · Cited by 4
Kong, D. (2022) · Physical Review Fluids · doi:10.1103/physrevfluids.7.074803 · Cited by 4
The GalileoJupiter Probe Doppler Wind Experiment
Atkinson, D. H. (2001) · Solar System Research · doi:10.1023/a:1012348103693 · Cited by 4
Taylor–Proudman columns in non‐hydrostatic divergent baroclinic and barotropic flows
Juárez, M. D. L. T. (2009) · Quarterly Journal of the Royal Meteorological Society · doi:10.1002/qj.483 · Cited by 4
Vertical wind shear on Jupiter from Cassini images
Li, L., Ingersoll, A. P., Vasavada, A. R., Simon, A. A., C, A. D. D. G., Ewald, S. P., Porco, C. C., & West, R. A. (2006) · AGUFM · 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
“By contrast, the deep model suggests that the flow is organised in deep concentric rotating cylinders, with jets their external representation, (see Busse (1970), Busse (1976)).”
BackgroundObservational 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
Liao, X., Zhang, K., & Li, L. (2012) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091929.2011.641960 · Cited by 3
“…character of the fluid motion has been widely used to study convection-driven differential rotation in rapidly rotating spherical systems (see, e.g. Busse 1976, Cardin and Olson 1994, Chen and Zhang 2002, Aubert et al. 2003, Liao et al. 2005, Gillet and Jones 2006) by assuming that the velocity of…”
BackgroundGeostrophic motions of a Boussinesq fluid in a thick rotating spherical shell
Lesueur, V., Abouelainine, A., Mangeney, A., & Drossart, P. (1999) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091929908203696 · Cited by 3
Parameterized rotating convection for core and planetary atmosphere dynamics
Zhang, K. (1991) · Geophysical Research Letters · doi:10.1029/91gl00137 · Cited by 3
Metadata
- Authors
- Busse, F. H.
- Affiliations
- University of California, Los Angeles (US)
- Corresponding author
- Busse, F.H.
- ORCID
- Busse, F.H.
- Venue
- Icarus
- Publisher
- Elsevier BV
- Published
- 1976-10
- Volume
- 29
- Issue
- 2
- Pages
- 255-260
- ISSN
- 0019-1035 (ISSN-L)
- OpenAlex
- W2074802867
- Cited by
- 278
- References
- 15
- Citations by year
- 2026: 3 · 2025: 4 · 2024: 5 · 2023: 8 · 2022: 9 · 2021: 6 · 2020: 11 · 2019: 9 · 2018: 34 · 2017: 10 · 2016: 8 · 2015: 9 · 2014: 4 · 2013: 5 · 2012: 7
- FWCI
- 2.52
- Type
- journal article
- Language
- en
- Open access
- closed
- Locations
- Icarus (publishedVersion)
- ERef Bayreuth (University of Bayreuth) (submittedVersion)
- Funders
- National Science Foundation
- 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 atmosphere, convection, latitudinal structure, internal heating, Boussinesq approximation, eddy viscosity, turbulent flow
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