Small‐scale waves on Jupiter: A reanalysis of New Horizons, Voyager, and Galileo data

Simon-Miller, A. A.; Li, Liming; Reuter, Dennis C.

doi:10.1002/2015gl063433

Cited by 19 publications

(21 citation statements)

References 21 publications

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“…Therefore, it seems that Saturn's equatorial zonal winds keep increasing from the tropopause, which is around 50 hPa (Fletcher et al, 2010), to the 2,000 hPa pressure level. Such a picture is qualitatively similar to the vertical variation of Jupiter's equatorial zonal winds measured by the Galileo Probe (Atkinson, 2001;Atkinson et al, 1996Atkinson et al, , 1997Atkinson et al, , 1998 and the Cassini spacecraft Li et al, 2006;Simon et al, 2015;Simon-Miller et al, 2006), in which Jupiter's equatorial zonal winds keep increasing from the tropopause~100 hPa to the pressure level around 5,000 hPa.…”

Section: Resultssupporting

confidence: 77%

Saturn's Global Zonal Winds Explored by Cassini/VIMS 5‐μm Images

Studwell

Jiang

et al. 2018

Geophysical Research Letters

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The Cassini Visual and Infrared Mapping Spectrometer (VIMS) 5‐μm images are used to derive Saturn's global zonal winds around the 2,000‐hPa level. The comparison of zonal winds between 2,000 and 300–500 hPa shows a general consistency of wind structure between the two pressure levels on a global scale. However at some latitudes, the magnitude of the zonal winds differs between these levels. The equatorial zonal winds are stronger downward, while the zonal winds in the middle and high latitudes are generally weaker downward. These new wind measurements also imply that barotropic and baroclinic instabilities probably exist through the relatively deep atmosphere at some latitudes. Finally, our analysis reveals that the VIMS winds in the two polar regions are basically constant with time except for a westerly jet centered at ~88°N, which decreased from 135 ± 7 m/s in 2008 to 91 ± 12 m/s in 2017.

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Section: Resultssupporting

confidence: 77%

Saturn's Global Zonal Winds Explored by Cassini/VIMS 5‐μm Images

Studwell

Jiang

et al. 2018

Geophysical Research Letters

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“…The only previous phenomena similar to the HAC are the shadows that were detected in mesoscale waves near the terminator in New Horizons observations [ Simon et al ., ], but these were at much lower latitudes. Rages et al .…”

Section: Resultsmentioning

confidence: 99%

“…The only previous phenomena similar to the HAC are the shadows that were detected in mesoscale waves near the terminator in New Horizons observations [Simon et al, 2015], but these were at much lower latitudes. Rages et al [1999] detected polar haze layers near the same high latitude using Galileo high-resolution images of Jupiter's limb.…”

Section: 1002/2016gl072443mentioning

confidence: 92%

The first close‐up images of Jupiter's polar regions: Results from the Juno mission JunoCam instrument

Orton

Hansen

Caplinger

et al. 2017

Geophysical Research Letters

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During Juno's first perijove encounter, the JunoCam instrument acquired the first images of Jupiter's polar regions at 50–70 km spatial scale at low emission angles. Poleward of 64–68° planetocentric latitude, where Jupiter's east‐west banded structure breaks down, several types of discrete features appear on a darker background. Cyclonic oval features are clustered near both poles. Other oval‐shaped features are also present, ranging in size from 2000 km down to JunoCam's resolution limits. The largest and brightest features often have chaotic shapes. Two narrow linear features in the north, associated with an overlying haze feature, traverse tens of degrees of longitude. JunoCam also detected an optically thin cloud or haze layer past the northern nightside terminator estimated to be 58 ± 21 km (approximately three scale heights) above the main cloud deck. JunoCam will acquire polar images on every perijove, allowing us to track the state and evolution of longer‐lived features.

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“…Cameras on the New Horizons spacecraft also saw 300 km waves and were able to measure the phase speed (Simon et al 2015a), which turned out to be to the east and 90 m s −1 faster than the local zonal flow. This high speed was not predicted by either of the two earlier models (Flasar & Gierasch 1986;Bosak & Ingersoll 2002), but these waves are not the same in appearance, being centered symmetrically on the equator and extending over a much larger longitude range.…”

Section: Wave Typesmentioning

confidence: 99%

“…Mesoscale waves, as revealed by cloud patterns, have been observed on Jupiter since the 1980s. Voyager-ISS (Hunt & Muller 1979;Flasar & Gierasch 1986), New Horizon with its Multispectral Visible Imaging Camera (MVIC) and its Long Range Reconnaissance Imager (LORRI; Simon et al 2015a), and Galileo-NIMS (Arregi et al 2009) all detected wavy features on the underlying clouds at wavelengths ranging from the violet (416 nm) to the NIR (975 nm). All these wavelengths found similar pressure levels no deeper than 0.8 bar, corresponding to the upper troposphere, and where the ammonia cloud deck is predicted to occur (West et al 2004;Atreya et al 2005).…”

Section: Introductionmentioning

confidence: 99%

Characterization of Mesoscale Waves in the Jupiter NEB by Jupiter InfraRed Auroral Mapper on board Juno

Adriani

Moriconi

Altieri

et al. 2018

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In 2017, the Jupiter InfraRed Auroral Mapper (JIRAM), on board the NASA-ASI Juno mission, observed a wide longitude region (50°W-80°E in System III) that was perturbed by a wave pattern centered at 15°N in the Jupiter's North Equatorial Belt (NEB). We analyzed JIRAM data acquired on 2017 July 10 using the M-channel and on 2017 February 2 with the spectrometer. The two observations occurred at different times and at slightly different latitudes. The waves appear as clouds blocking the deeper thermal emission. The wave crests are oriented north-south, and the typical wave packet contains 10 crests and 10 troughs. We used Fourier analysis to rigorously determine the wavenumbers associated with the observed patterns at a confidence level of 90%. Wavelet analysis was also used to constrain the spatial localization of the largest energies involved in the process and determine the wavelengths carrying the major contribution. We found wavelengths ranging from 1400 to 1900 km, and generally decreasing toward the west. Where possible, we also computed a vertical location of the cloud pressure levels from the inversion of the spectral radiances measured by the JIRAM spectrometer. The waves were detected at pressure levels consistent with the NH 3 as well as NH 4 SH clouds. Phase velocities could not be determined with sufficient confidence to discriminate whether the alternating crests and troughs are a propagating wave or a manifestation of a fluid dynamical instability.

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Small‐scale waves on Jupiter: A reanalysis of New Horizons, Voyager, and Galileo data

Cited by 19 publications

References 21 publications

Saturn's Global Zonal Winds Explored by Cassini/VIMS 5‐μm Images

Saturn's Global Zonal Winds Explored by Cassini/VIMS 5‐μm Images

The first close‐up images of Jupiter's polar regions: Results from the Juno mission JunoCam instrument

Characterization of Mesoscale Waves in the Jupiter NEB by Jupiter InfraRed Auroral Mapper on board Juno

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