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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
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Cited by
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Diamond, P. H., Itoh, S. ‐., Itoh, K., & Hahm, T. S. (2005) · Plasma Physics and Controlled Fusion · doi:10.1088/0741-3335/47/5/r01 · Cited by 1,942
A New Look at the Saturn System: The Voyager 2 Images
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Cassini Imaging of Jupiter's Atmosphere, Satellites, and Rings
Porco, C. C., West, R. A., McEwen, A. S., C, A. D. D. G., Ingersoll, A. P., Thomas, P. C., Squyres, S. W., Luke Dones, B., Murray, C. D., Johnson, T. V., et al. (2003) · Science · doi:10.1126/science.1079462 · Cited by 489
A quarter-century of H-mode studies
Wagner, F. (2007) · Plasma Physics and Controlled Fusion · doi:10.1088/0741-3335/49/12b/s01 · Cited by 411
ZONAL FLOWS AND LONG-LIVED AXISYMMETRIC PRESSURE BUMPS IN MAGNETOROTATIONAL TURBULENCE
Johansen, A., Youdin, A. N., & Klahr, H. H. (2009) · The Astrophysical Journal · doi:10.1088/0004-637x/697/2/1269 · Cited by 405
“Busse (1976) proposed that these flows arise from an inverse cascade of thermally driven convection in giant planet interiors.”
BackgroundSEIFF, A., Kirk, D. B., Knight, T. C. D., Young, R. E., Mihalov, J. D., Young, L. A., Milos, F. S., Schubert, G., Blanchard, R. C., & Atkinson, D. H. (1998) · Journal of Geophysical Research Atmospheres · doi:10.1029/98je01766 · Cited by 361
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Bolton, 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) · Space Science Reviews · doi:10.1007/s11214-017-0429-6 · Cited by 342
“Deep roots and their large inertia may be the key to this longevity (Busse 1976; Ingersoll and Pollard 1982).”
BackgroundJovian 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
“On this basis, Busse (1976) suggested that the Taylor–Proudman theorem (Taylor 1923) holds throughout the interior.”
BackgroundInfluentialA comparison of the interiors of Jupiter and Saturn
Guillot, T. (1999) · Planetary and Space Science · doi:10.1016/s0032-0633(99)00043-4 · Cited by 321
“…and in particular the presence and strength of convection in their interiors, are difficult to assess (Stevenson and Salpeter 1977; see also Busse 1976, Zhang & Schubert 1996), this property is a chance because it allows us to constrain their interior density profiles, by measuring the…”
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
Jupiter’s atmospheric jet streams extend thousands of kilometres deep
Kaspi, Y., Galanti, E., Hubbard, W. B., Stevenson, D. J., Bolton, S. J., IESS, L., Guillot, T., Bloxham, J., Connerney, J. E. P., Cao, H., et al. (2018) · Nature · doi:10.1038/nature25793 · Cited by 268
Stevenson, D. J. (1983) · Reports on Progress in Physics · doi:10.1088/0034-4885/46/5/001 · Cited by 262
Spiralling columnar convection in rapidly rotating spherical fluid shells
Zhang, K. (1992) · Journal of Fluid Mechanics · doi:10.1017/s0022112092001526 · Cited by 229
Geophysical and astrophysical fluid dynamics beyond the traditional approximation
Gerkema, T., Zimmerman, J. T. F., Maas, L. R. M., & van Haren, H. (2008) · Reviews of Geophysics · doi:10.1029/2006rg000220 · Cited by 223
Convection driven zonal flows and vortices in the major planets
Busse, F. H. (1994) · Chaos An Interdisciplinary Journal of Nonlinear Science · doi:10.1063/1.165999 · Cited by 219
Self-citationConstraints on deep seated zonal winds inside Jupiter and Saturn.
LIU, J., GOLDREICH, P., & STEVENSON, D. (2008) · Icarus · doi:10.1016/j.icarus.2007.11.036 · Cited by 208
“Busse (1976, 1983, 1994) advocates deep flows.”
Atmospheric Dynamics of the Outer Planets
Ingersoll, A. P. (1990) · Science · doi:10.1126/science.248.4953.308 · Cited by 199
Ingersoll, A. P., & Pollard, D. (1982) · Icarus · doi:10.1016/0019-1035(82)90169-5 · Cited by 193
A suppression of differential rotation in Jupiter’s deep interior
Guillot, T., Miguel, Y., Militzer, B., Hubbard, W. B., Kaspi, Y., Galanti, E., Cao, H., Helled, R., Wahl, S. M., IESS, L., et al. (2018) · Nature · doi:10.1038/nature25775 · Cited by 190
“We adopt a four-layer structure for the interior models: (1) a helium-poor upper envelope in which hydrogen is in molecular form, (2) a helium-rich, metallichydrogen lower envelope, (3) a dilute core which consists of helium-rich metallic hydrogen with an increase of the heavy-element content and (4) a central dense c…”
BackgroundMethodInfluentialFormation of Jets and Equatorial Superrotation on Jupiter
Schneider, T., & Liu, J. (2008) · Journal of the Atmospheric Sciences · doi:10.1175/2008jas2798.1 · Cited by 169
“…posit as the driver of the general circulation either differential radiative heating of the atmosphere or intrinsic convective heat fluxes (e.g., Busse 1976, 1994; Williams 1979; Ingersoll et al. 2004; Vasavada and Showman 2005); however, they do not reproduce all large-scale features of the…”
BackgroundATMOSPHERIC DYNAMICS OF BROWN DWARFS AND DIRECTLY IMAGED GIANT PLANETS
Showman, A. P., & Kaspi, Y. (2013) · The Astrophysical Journal · doi:10.1088/0004-637x/776/2/85 · Cited by 153
“(Busse 1976; Kaspi et al. 2009) and there can be no flow crossing these surfaces.”
BackgroundThe deep wind structure of the giant planets: Results from an anelastic general circulation model
Kaspi, Y., Flierl, G. R., & Showman, A. P. (2009) · Icarus · doi:10.1016/j.icarus.2009.03.026 · Cited by 149
“…1978, 1979; Cho and Polvani, 1996; Smith, 2003; Kaspi and Flierl, 2007; Showman, 2007; Scott and Polvani, 2007), while the other approach (Busse, 1970, 1976) claimed the zonal surface velocities are surface manifestation of concentric rotating cylinders (Taylor columns) penetrating the…”
BackgroundThe Galileo Probe Doppler Wind Experiment: Measurement of the deep zonal winds on Jupiter.
Atkinson, D. H., Pollack, J. B., & Seiff, A. (1998) · Journal of Geophysical Research: Planets · doi:10.1029/98je00060 · Cited by 143
Planetary magnetic fields: Observations and models
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Finite-amplitude convection in rotating spherical fluid shells
Tilgner, A., & Busse, F. H. (1997) · Journal of Fluid Mechanics · doi:10.1017/s0022112096004259 · Cited by 126
Self-citationCompressible convection in the deep atmospheres of giant planets
JONES, C. A., & Kuzanyan, K. M. (2009) · Icarus · doi:10.1016/j.icarus.2009.05.022 · Cited by 122
“This was also seen in Busse (2002), who attributes it to an influence of the zonal flow on the convection.”
InfluentialMechanisms of Jet Formation on the Giant Planets
Liu, J., & Schneider, T. (2010) · Journal of the Atmospheric Sciences · doi:10.1175/2010jas3492.1 · Cited by 135
“…models posit as the driver of the flow either the differential radiative heating of the upper atmosphere (e.g., Williams 1979, 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).”
BackgroundInfluentialHeimpel, M., & Aurnou, J. (2007) · Icarus · doi:10.1016/j.icarus.2006.10.023 · Cited by 122
“In a pioneering study, Busse (1976) proposed that the jovian surface zonal flows could be a manifestation of deep convection.”
BackgroundInfluentialSimulation of deep-seated zonal jets and shallow vortices in gas giant atmospheres
Heimpel, M., Gastine, T., & Wicht, J. (2016) · Nature Geoscience · doi:10.1038/ngeo2601 · Cited by 119
SCOTT, R. K., & Polvani, L. M. (2007) · Journal of the Atmospheric Sciences · doi:10.1175/jas4003.1 · Cited by 111
“One line of research, pioneered by Busse (1976) , has argued that the alternating bands are the surface signature of convective circulations that extend deep into those planets, with concentric cylinders rotating parallel to the planetary axis of rotation and intersecting the planets’ surface.”
A model of mean zonal flows in the major planets
Busse, F. H. (1983) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091928308221746 · Cited by 116
Self-citationConrath, B. J., & Pirraglia, J. A. (1983) · Icarus · doi:10.1016/0019-1035(83)90148-3 · Cited by 115
The effects of vigorous mixing in a convective model of zonal flow on the ice giants.
Aurnou, J., Heimpel, M., & Wicht, J. (2007) · Icarus · doi:10.1016/j.icarus.2007.02.024 · Cited by 107
“Models by Hubbard et al. (1991), based on fitting the observed J2 and J4 gravitational moments, have shown that the surface zonal flows on Uranus and Neptune cannot extend globally on cylinders to great depths into their interiors, as first proposed for Jupiter by Busse (1976).”
Rhines, P. B. (1994) · Chaos An Interdisciplinary Journal of Nonlinear Science · doi:10.1063/1.166011 · Cited by 101
Gravitational signature of Jupiter's internal dynamics
Kaspi, Y., Hubbard, W. B., Showman, A. P., & Flierl, G. R. (2010) · Geophysical Research Letters · doi:10.1029/2009gl041385 · Cited by 94
“Due to Jupiter’s internal heat source and rapid rotation it has been suggested [Busse, 1976; Ingersoll and Pollard, 1982] that the observed surface zonal flows on Jupiter extend to the interior along cylinders parallel to the axis of rotation.”
BackgroundConfirmation of bistable stellar differential rotation profiles
Käpylä, P. J., Korpi, M. J., & Brandenburg, A. (2014) · Astronomy and Astrophysics · doi:10.1051/0004-6361/201423412 · Cited by 91
Deep zonal winds can result from shallow driving in a giant-planet atmosphere
Showman, A. P., Gierasch, P. J., & Lian, Y. (2006) · Icarus · doi:10.1016/j.icarus.2006.01.019 · Cited by 89
“In the “deep-forcing” scenario, convection cells that extend throughout the molecular hydrogen envelope (a depth of perhaps ∼104 km) drive differential rotation in the interior that manifests as jets at the cloud level (e.g., Busse, 1976; Aurnou and Olson, 2001; Christensen,”
BackgroundAtmospheric Circulation of ExoplanetsPreprint
Showman, A. P., Cho, J. Y. K., & Kristen Menou, A. (2009) · arXiv (Cornell University) · doi:10.48550/arxiv.0911.3170 · Cited by 113
Galileo Doppler Measurements of the Deep Zonal Winds at Jupiter
Atkinson, D. H., Pollack, J. B., & SEIFF, A. (1996) · Science · doi:10.1126/science.272.5263.842 · Cited by 87
Convection in a rotating cylindrical annulus. Part 2. Transitions to asymmetric and vacillating flow
Or, A. C., & Busse, F. H. (1987) · Journal of Fluid Mechanics · doi:10.1017/s0022112087000144 · Cited by 86
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Cassini Ring Seismology as a Probe of Saturn’s Interior. I. Rigid Rotation
Mankovich, C. R., Marley, M. S., Fortney, J. J., & Movshovitz, N. (2019) · The Astrophysical Journal · doi:10.3847/1538-4357/aaf798 · Cited by 84
Inferring the depth of the zonal jets on Jupiter and Saturn from odd gravity harmonics
Kaspi, Y. (2012) · Geophysical Research Letters · doi:10.1029/2012gl053873 · Cited by 84
A strong decrease in Saturn's equatorial jet at cloud level
Sánchez-Lavega, A., Pérez-Hoyos, S., Rojas, J. F., Hueso, R., & French, R. G. (2003) · Nature · doi:10.1038/nature01653 · Cited by 78
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“Deep roots and their large inertia may be the key to this longevity (Busse 1976, Ingersoll and Pollard, 1982).”
BackgroundExperimental Determination of Zonal Winds Driven by Tides
Morize, C., Bars, M. L., Gal, P. L., & Tilgner, A. (2010) · Physical Review Letters · doi:10.1103/physrevlett.104.214501 · Cited by 76
Kaspi, Y., Galanti, E., Showman, A. P., Stevenson, D. J., Guillot, T., IESS, L., & Bolton, S. J. (2020) · Space Science Reviews · doi:10.1007/s11214-020-00705-7 · Cited by 77
“These ideas also emerged in the 1970s, with the seminal papers of Busse (1970, 1976), and have evolved to more complex interior convention 3D simulations (e.g., Busse 1994; Sun et al. 1993; Christensen 2001; Aurnou and Olson 2001; Wicht et al. 2002; Heimpel et al. 2005; Kaspi et al. 2009; Jones and…”
BackgroundConfirmation of bistable stellar differential rotation profiles
Käpylä, P. J., Korpi, M. J., & Brandenburg, A. (2014) · Springer Link (Chiba Institute of Technology) · doi:10.1051/0004-6361/201423412/pdf · Cited by 74
Origin of Jupiter’s cloud-level zonal winds remains a puzzle even after Juno
Kong, D., Zhang, K., Schubert, G., & Anderson, J. D. (2018) · Proceedings of the National Academy of Sciences · doi:10.1073/pnas.1805927115 · Cited by 73
Equatorial superrotation in shallow atmospheres
SCOTT, R. K., & Polvani, L. M. (2008) · Geophysical Research Letters · doi:10.1029/2008gl036060 · Cited by 69
“These strong jet streams are dynamical in origin but, despite much attention over several decades, the actual dynamical processes involved remain controversial, to the extent that there is still debate over whether their origins lie in deep convection throughout the planetary interior [1], or rather in shallow turbule…”
BackgroundSromovsky, L. A., Revercomb, H. E., Krauss, R. J., & SUOMI, V. E. (1983) · Journal of Geophysical Research Atmospheres · doi:10.1029/ja088ia11p08650 · Cited by 73
Cassini Ring Seismology as a Probe of Saturn's Interior I: Rigid Rotation
Mankovich, C. R., Marley, M. S., Fortney, J. J., & Movshovitz, N. (2019) · eScholarship (California Digital Library) · Cited by 71
Deep winds on Jupiter as measured by the Galileo probe
Atkinson, D. H., Ingersoll, A. P., & SEIFF, A. (1997) · Nature · doi:10.1038/41718 · Cited by 69
“On the other hand, if the winds drew their energy from internal heat, they might continue down indefinitely into the fluid interior of Jupite”
BackgroundBanded Surface Flow Maintained by Convection in a Model of the Rapidly Rotating Giant Planets
Sun, Z., Schubert, G., & Glatzmaier, G. A. (1993) · Science · doi:10.1126/science.260.5108.661 · Cited by 66
Differential rotation driven by convection in a rapidly rotating annulus
Busse, F. H., & Hood, L. L. (1982) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091928208209005 · Cited by 65
Self-citationFormation of Jets by Baroclinic Instability on Gas Planet Atmospheres
Kaspi, Y., & Flierl, G. R. (2007) · Journal of the Atmospheric Sciences · doi:10.1175/jas4009.1 · Cited by 60
Convection in rapidly rotating spherical fluid shells
Busse, F. H., & Cuong, P. G. (1977) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091927708240369 · Cited by 64
Self-citationPerryman, M. A. C. (2011) · Cambridge University Press eBooks · doi:10.1017/cbo9780511994852.011 · Cited by 71
The Galileo probe mission to Jupiter: Science overview
Young, R. E. (1998) · Journal of Geophysical Research Atmospheres · doi:10.1029/98je01051 · Cited by 58
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Patterns of convection in rotating spherical shells
Simitev, R. D., & Busse, F. H. (2003) · New Journal of Physics · doi:10.1088/1367-2630/5/1/397 · Cited by 57
“Contents”
Self-citationSTARSPOTS DUE TO LARGE-SCALE VORTICES IN ROTATING TURBULENT CONVECTION
Käpylä, P. J., Mantere, M. J., & Hackman, T. (2011) · The Astrophysical Journal · doi:10.1088/0004-637x/742/1/34 · Cited by 55
“The giant planets Jupiter and Saturn are also likely to have outer convection zones (e.g. Busse 1976), but they rotate much faster than the Sun.”
BackgroundOn the relationship between zonal jets and dynamo action in giant planets
Heimpel, M. H., & Pérez, N. G. (2011) · Geophysical Research Letters · doi:10.1029/2011gl047562 · Cited by 54
“1 [6] Models of convection and flow in rotating spheres have postulated that zonal flows extend into the deep interior [ Busse, 1976, 1983; Yano et al., 2003].”
BackgroundSimulating Jupiter’s weather layer. Part I: Jet spin-up in a dry atmosphere
Young, R. M. B., Read, P. L., & Wang, Y. (2018) · Icarus · doi:10.1016/j.icarus.2018.12.005 · Cited by 49
“Jupiter’s composition implies that its H-He atmosphere must remain continuously fluid to great depths, but until very recently it was not even possible to determine whether the observed large-scale meteorological circulations penetrate deep into the planet (Busse, 1976) or are relatively shallow, as observed on Uranus…”
BackgroundInfluentialStable stratification promotes multiple zonal jets in a turbulent jovian dynamo model
Gastine, T., & Wicht, J. (2021) · Icarus · doi:10.1016/j.icarus.2021.114514 · Cited by 53
Superrotation in Planetary Atmospheres
Imamura, T., Mitchell, J. L., Lebonnois, S., Kaspi, Y., Showman, A. P., & Korablev, O. (2020) · Space Science Reviews · doi:10.1007/s11214-020-00703-9 · Cited by 52
“The alternative approach suggests that the observed jets are the surface manifestation of convective columns originating from the hot interiors of the giant planets (Busse 1976; Busse 1994).”
BackgroundTeleconvection: Remotely Driven Thermal Convection in Rotating Stratified Spherical Layers
Zhang, K., & Schubert, G. (2000) · Science · doi:10.1126/science.290.5498.1944 · Cited by 51
Zhang, K., Kong, D., & Schubert, G. (2015) · The Astrophysical Journal · doi:10.1088/0004-637x/806/2/270 · Cited by 50
A convective model for the zonal jets in the atmospheres of Jupiter and Saturn
Condie, S. A., & Rhines, P. B. (1994) · Nature · doi:10.1038/367711a0 · Cited by 49
Deep rotating convection generates the polar hexagon on Saturn
Yadav, R. K., & Bloxham, J. (2020) · Proceedings of the National Academy of Sciences · doi:10.1073/pnas.2000317117 · Cited by 45
Li, L., Conrath, B. J., Gierasch, P. J., Achterberg, R. K., Nixon, C. A., Simon, A. A., Flasar, F. M., Banfield, D., Baines, K. H., West, R. A., et al. (2010) · Journal of Geophysical Research Atmospheres · doi:10.1029/2010je003631 · Cited by 47
“Other model studies assume that the internal heat and related convection are randomly or uniformly distributed over the outer planets [Busse, 1976, 1983; Christensen, 2001;Heimpel and Aurnou, 2007;Aurnou et al., 2007; Chan and Mayr, 2008; Schneider and Liu, 2008].”
BackgroundZonal jets in rotating convection with mixed mechanical boundary conditions
Aurnou, J. M., & Heimpel, M. H. (2004) · Icarus · doi:10.1016/j.icarus.2004.01.013 · Cited by 47
Geophysical fluid dynamics: whence, whither and why?
Vallis, G. K. (2016) · Proceedings of the Royal Society A Mathematical Physical and Engineering Sciences · doi:10.1098/rspa.2016.0140 · Cited by 45
“The original Jovian dichotomy was that there is either a shallow weather layer, rather like on a terrestrial planet with β-plane turbulence giving rise to jets [105], or deep Taylor columns of which the jets are surface manifestations [106].”
BackgroundGlatzmaier, G. A., & Olson, P. L. (1993) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091929308203589 · Cited by 45
Observational evidence for cylindrically oriented zonal flows on Jupiter
Kaspi, Y., Galanti, E., Park, R. S., Duer, K., Gavriel, N., Durante, D., IESS, L., Parisi, M., Buccino, D., Guillot, T., et al. (2023) · Nature Astronomy · doi:10.1038/s41550-023-02077-8 · Cited by 44
“Moreover, the analysis provides direct observational evidence that the cloud-level winds extend inwards along the direction of the spin axis, as has been suggested in theoretical studies 18,19 .”
Scaling laws for convection and jet speeds in the giant planets
Showman, A. P., Kaspi, Y., & Flierl, G. R. (2010) · Icarus · doi:10.1016/j.icarus.2010.11.004 · Cited by 44
“• Next, we attempted to explain the jet speeds obtained by Christensen (2002) and Kaspi et al. (2009) in three-dimensional numerical simulations of convection with free-slip boundaries.”
BackgroundMethodMultiple jets and zonal flow on Jupiter
JONES, C. A., Rotvig, J., & Abdulrahman, A. (2003) · Geophysical Research Letters · doi:10.1029/2003gl016980 · Cited by 44
Convection in a rotating cylindrical annulus Part 3. Vacillating and spatially modulated flows
Schnaubelt, M., & Busse, F. H. (1992) · Journal of Fluid Mechanics · doi:10.1017/s0022112092000399 · Cited by 44
Self-citationA full, self-consistent treatment of thermal wind balance on oblate fluid planets
Galanti, E., Kaspi, Y., & Tziperman, E. (2016) · Journal of Fluid Mechanics · doi:10.1017/jfm.2016.687 · Cited by 42
“1982) and Hubbard (1999) used potential theory to calculate the gravity moments due to internal flows, by extending the observed cloud-level winds along cylinders throughout the planet as suggested by Busse (1976). This approach takes into account the oblateness of the planet, yet is only possible for the barotropic ca…”
BackgroundInfluentialEvidence 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. (2021) · Geophysical Research Letters · doi:10.1029/2021gl095651 · Cited by 43
“Consistently, deep convection models of Jupiter also show barotropic flows (e.g., Busse, 1976; Aurnou and Olson, 2001).”
Earth-Based Radio Tracking of the Galileo Probe for Jupiter Wind Estimation
Folkner, W. M., Preston, R. A., Border, J. S., Navarro, J., Wilson, W. E., & Oestreich, M. (1997) · Science · doi:10.1126/science.275.5300.644 · Cited by 42
Transitions to chaotic thermal convection in a rapidly rotating spherical fluid shell
Sun, Z., Schubert, G., & Glatzmaier, G. A. (1993) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091929308203576 · Cited by 42
Generation of mean flows by thermal convection
Busse, F. H. (1983) · Physica D Nonlinear Phenomena · doi:10.1016/0167-2789(83)90273-7 · Cited by 41
Self-citationBastin, M. E., & Read, P. L. (1998) · Physics of Fluids · doi:10.1063/1.869530 · Cited by 40
Differential rotation in Jupiter: A comparison of methods
Wisdom, J., & Hubbard, W. B. (2015) · Icarus · doi:10.1016/j.icarus.2015.12.030 · Cited by 39
“The observed zonal wind profile may extend all the way through the planet (Busse, 1976) or be surficial (Williams, 1978).”
BackgroundInfluentialVertical 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) · Journal of Geophysical Research Atmospheres · doi:10.1029/2005je002556 · Cited by 39
Interaction of moist convection with zonal jets on Jupiter and Saturn
Li, L., Ingersoll, A. P., & Huang, X. (2005) · Icarus · doi:10.1016/j.icarus.2005.08.016 · Cited by 40
“Deep convection extending through the planet from north to south (Busse, 1976) makes westerly equatorial jets possible in theory.”
BackgroundPenetrative Convection and Zonal Flow on Jupiter
Zhang, K., & Schubert, G. (1996) · Science · doi:10.1126/science.273.5277.941 · Cited by 39
Global dynamics and thermal structure of Jupiter's atmosphere
Flasar, F. M. (1986) · Icarus · doi:10.1016/0019-1035(86)90140-5 · Cited by 38
The Saturnian ribbon feature—A baroclinically unstable model
Godfrey, D. A., & Moore, V. (1986) · Icarus · doi:10.1016/0019-1035(86)90026-6 · Cited by 39
Anelastic spherical dynamos with radially variable electrical conductivity
Dietrich, W., & JONES, C. A. (2018) · Icarus · doi:10.1016/j.icarus.2018.01.003 · Cited by 37
“The columns exhibit a consistent tilt leading to Reynolds stress, which pumps zonal angular momentum outwards, e.g. Busse (1976) ; Christensen (2001) ; Aubert (2005) .”
BackgroundOrigins of atmospheric zonal winds
Yano, J., Talagrand, O., & Drossart, P. (2003) · Nature · doi:10.1038/421036a · Cited by 37
Deep convection–driven vortex formation on Jupiter and Saturn
Yadav, R. K., Heimpel, M. H., & Bloxham, J. (2020) · Science Advances · doi:10.1126/sciadv.abb9298 · Cited by 35
“Presence of such large anticyclonic vortices has not been reported in conventional spherical shell simulations of the outer convective layers of giant planets ( 11 – 15 ); therefore, the deeper dynamo layer is the key for triggering them.”
Flasar, F. M., & Gierasch, P. J. (1978) · Geophysical & Astrophysical Fluid Dynamics · doi:10.1080/03091927808242636 · Cited by 34
Garcia‐Melendo, E., Sánchez-Lavega, A., & Dowling, T. E. (2005) · Icarus · doi:10.1016/j.icarus.2005.02.012 · Cited by 34
Observations and Analysis of Longitudinal Thermal Waves on Jupiter
Deming, D., Reuter, D. C., Jennings, D. E., Bjoraker, G. L., McCabe, G. H., Fast, K. E., & Wiedemann, G. (1997) · Icarus · doi:10.1006/icar.1996.5658 · Cited by 33
From Penetrative Convection to Teleconvection
Zhang, K., & Schubert, G. (2002) · The Astrophysical Journal · doi:10.1086/340288 · Cited by 33
“This is the first time that the multilayer roll structure of convection, suggested by Busse (1976), has been found in a rotating linear spherical convective system.”
BackgroundInfluentialStable, baroclinic eddies on Jupiter and Saturn: A laboratory analog and some observational tests
Read, P. L. (1986) · Icarus · doi:10.1016/0019-1035(86)90141-7 · Cited by 33
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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