Saturn eddy momentum fluxes and convection: First estimates from Cassini images

Genio, Anthony D. Del; Barbara, J.; Ferrier, Joseph; Ingersoll, Andrew P.; West, Robert A.; Vasavada, A. R.; Spitale, J. N.; Porco, C. C.

doi:10.1016/j.icarus.2007.02.013

Cited by 63 publications

(75 citation statements)

References 44 publications

(61 reference statements)

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“…This suggests that in the upper troposphere and lower stratosphere, ascending motions occur on the equatorward side of the jet peak whereas descending motions occur on the poleward side accompanied by adiabatic cooling and warming, in good agreement with results obtained from the Voyagers (Conrath and Pirraglia 1983). This stands in contrast to the tropospheric continuum cloud top level, where the inferred pattern of rising and sinking motions is just the opposite (Del Genio et al 2007a) and not obviously related to the albedo pattern (see section 7.4.2).…”

Section: Albedo Patterns Vs Jets On Saturn Vs Jupitersupporting

confidence: 85%

Saturn Atmospheric Structure and Dynamics

Genio

Achterberg

Baines

et al. 2009

Saturn From Cassini-Huygens

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Section: Albedo Patterns Vs Jets On Saturn Vs Jupitersupporting

confidence: 85%

Saturn Atmospheric Structure and Dynamics

Genio

Achterberg

Baines

et al. 2009

Saturn From Cassini-Huygens

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“…The global turbulent zonal velocity field (u´, v´) and the resulting spectral energy distribution E´K and averaged eddy fluxes <u'v'> were measured in Jupiter using Voyager images (Beebe et al 1980 andIngersoll et al 1981) although they were questioned later by Sromovsky et al (1982). Recently, using Cassini images, eddy motions were measured in some Jupiter (Salyk et al 2006) and Saturn (Del Genio et al 2007) areas, confirming the momentum transfer from the eddies to the eastward jets and the energy conversion rates derived from the Voyagers' analysis. The only published studies of the power spectral laws for the turbulent zonal kinetic energy in…”

supporting

confidence: 54%

Brightness power spectral distribution and waves in Jupiter's upper cloud and hazes

Barrado-Izagirre

Pérez‐Hoyos

Sánchez‐Lavega

2009

Icarus

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To cite this version:N. Barrado-Izagirre, S. Pérez-Hoyos, A. Sánchez-Lavega. Brightness power spectral distribution and waves in Jupiter's upper cloud and hazes. Icarus, Elsevier, 2009, 202 (1) This is a PDF file of an unedited manuscript that has been accepted for publication. As a service to our customers we are providing this early version of the manuscript. The manuscript will undergo copyediting, typesetting, and review of the resulting proof before it is published in its final form. Please note that during the production process errors may be discovered which could affect the content, and all legal disclaimers that apply to the journal pertain. infrared and blue wavelengths, average spectral slopes are n 1 = -1.3 ± 0.4 for shorter wavenumbers (k < 80), and n 2 = -2.5 ± 0.7 for greater wavenumbers, whereas for the ultraviolet n 1 = -1.9 ± 0.4 and n 2 = -0.7 ± 0.4, possibly showing a different dynamical regime. We find a turning point in the spectra between both regimes at wavenumber k ~ 80 (corresponding to L ~ 1000 km) for all wavelengths.

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“…However, the basic mechanism of multiple jet formation due to correlated motion of the smaller-scale eddies does appear to be the same in both cases. 31 Whether or not a spectrally local energy cascade from eddy to jet scales is occurring on the gas giant planets is, to our knowledge, still an open question.…”

Section: -10mentioning

confidence: 99%

Turbulence, waves, and jets in a differentially heated rotating annulus experiment

2008

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A characteristic function to estimate the longitudinal dispersion coefficient in surface water flows over porous media Phys. Fluids 24, 046602 (2012) Frequency and damping of non-axisymmetric surface oscillations of a viscous axisymmetric liquid bridge Phys. Fluids 24, 042103 (2012) Nonlinear resonance in barotropic-baroclinic transfer generated by bottom sills Phys. Fluids 24, 046601 (2012) We report an analog laboratory study of planetary-scale turbulence and jet formation. A rotating annulus was cooled and heated at its inner and outer walls, respectively, causing baroclinic instability to develop in the fluid inside. At high rotation rates and low temperature differences, the flow became chaotic and ultimately fully turbulent. The inclusion of sloping top and bottom boundaries caused turbulent eddies to behave like planetary waves at large scales, and eddy interaction with the zonal flow then led to the formation of several alternating jets at mid-depth. The jets did not scale with the Rhines length, and spectral analysis of the flow indicated a distinct separation between jets and eddies in wavenumber space, with direct energy transfer occurring nonlocally between them. Our results suggest that the traditional "turbulent cascade" picture of zonal jet formation may be an inappropriate one in the geophysically important case of large-scale flows forced by differential solar heating.

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Saturn eddy momentum fluxes and convection: First estimates from Cassini images

Cited by 63 publications

References 44 publications

Saturn Atmospheric Structure and Dynamics

Saturn Atmospheric Structure and Dynamics

Brightness power spectral distribution and waves in Jupiter's upper cloud and hazes

Turbulence, waves, and jets in a differentially heated rotating annulus experiment

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