Observations and Analysis of Longitudinal Thermal Waves on Jupiter

Deming, Drake; Reuter, Dennis C.; Jennings, Donald E.; Bjoraker, G. L.; McCabe, George H.; Fast, K. E.; Wiedemann, Günter

doi:10.1006/icar.1996.5658

Cited by 30 publications

(28 citation statements)

References 23 publications

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“…Fig. 2b shows a wave pattern in the mid-NEB in the upper troposphere (p < 500 mbar), similar to that observed by previous studies [e.g., Magalhaes et al, 1990;Orton et al, 1994;Deming et al, 1997;Li et al, 2006;Fisher et al, 2016]. The warm crests have a central latitude of 13 − 15 • N, and the wave pattern is latitudinally confined to the bright belt at 10 − 17 • N (±1 • ).…”

Section: Upper Tropospheric Neb Wavesupporting

confidence: 84%

“…Previous studies have suggested multiple origins for these NEB thermal waves, ranging from forcing by phenomena in the deeper interior [Magalhaes et al, 1990;Deming et al, 1997]; forcing by tropospheric meteorology and convective plumes [Andrews et al, 1987]; flow disturbances around vortices [e.g., around White Spot Z, Li et al, 2006]; instabilities associated with the changing sign of the potential vorticity gradient [Achterberg and Flasar, 1996;Read et al, 2006;Rogers et al, 2016]; or the breaking of low-phase-speed Rossby waves generated by convection in the equatorial region, propagating poleward and depositing energy in regions where u approaches zero [Fisher et al, 2016]. This latter mechanism was based on numerical simulations able to qualitatively reproduce observations [Fisher et al, 2016], and therefore does not require any flow perturbations related to an NEB expansion.…”

Section: Upper Tropospheric Neb Wavementioning

confidence: 99%

“…These periods coincide with expansion events [1] and [2] in Section S1. Observations in this period was supplemented by Deming et al [1989Deming et al [ , 1997 between 1987 and 1993 during their search for planetary p-mode oscillations, identifying wavenumbers in the 2-15 range (with peaks at wavenumbers 6-11) and a westward phase speed of 5 m/s [Deming et al, 1997]. Unlike Orton's survey, the waves of Deming et al appeared to cover the whole tropical domain.…”

Section: A2 Supplemental S2: Previous Detections Of Mid-neb Wavesmentioning

confidence: 99%

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Jupiter's North Equatorial Belt expansion and thermal wave activity ahead of Juno's arrival

Fletcher

Orton

Sinclair

et al. 2017

Geophysical Research Letters

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The dark colors of Jupiter's North Equatorial Belt (NEB, 7–17°N) appeared to expand northward into the neighboring zone in 2015, consistent with a 3–5 year cycle. Inversions of thermal‐IR imaging from the Very Large Telescope revealed a moderate warming and reduction of aerosol opacity at the cloud tops at 17–20°N, suggesting subsidence and drying in the expanded sector. Two new thermal waves were identified during this period: (i) an upper tropospheric thermal wave (wave number 16–17, amplitude 2.5 K at 170 mbar) in the mid‐NEB that was anticorrelated with haze reflectivity; and (ii) a stratospheric wave (wave number 13–14, amplitude 7.3 K at 5 mbar) at 20–30°N. Both were quasi‐stationary, confined to regions of eastward zonal flow, and are morphologically similar to waves observed during previous expansion events.

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Section: Upper Tropospheric Neb Wavesupporting

confidence: 84%

Section: Upper Tropospheric Neb Wavementioning

confidence: 99%

Section: A2 Supplemental S2: Previous Detections Of Mid-neb Wavesmentioning

confidence: 99%

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Jupiter's North Equatorial Belt expansion and thermal wave activity ahead of Juno's arrival

Fletcher

Orton

Sinclair

et al. 2017

Geophysical Research Letters

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“…Because of these qualities, planetary waves become a very important subject of study. Among the giant planets, they have also been detected in Jupiter's equatorial temperature field (Magalhaes et al, 1989(Magalhaes et al, , 1990Orton et al, 1991;Deming et al, 1989Deming et al, , 1997, and in Satum's polar visible clouds ("the hexagon") (Godfrey, 1988) and in the mid-latitude temperature field (Achterberg and Flasar, 1996). In this paper we present evidence for the first time of the existence of planetary waves in the jovian subpolar stratosphere as traced by aerosol particulates.…”

Section: Introductionmentioning

confidence: 52%

A system of circumpolar waves in Jupiter's stratosphere

Sánchez‐Lavega¹,

Hueso²,

Acarreta³

1998

Geophysical Research Letters

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Abstract. We report on the optical identification on Hubble Space Telescope (HST) and Voyager 1 archived images, of a circumpolar system of Jovian stratospheric quasi-stationary waves, centered at planetographic latitudes-53%-62 ø, and-67 ø with averaged zonal wavenumbers 23, 11, and 12 respectively. The most conspicuous wave is detected in the 890-nm strong absorption band of methane at -67 ø latitude. Its amplitude changes in a matter of days, stretching and contracting but preserving the number of components in the latitude circle. This wave has been observed during several years and seems to be a persistent, long-term phenomena in Jupiter's atmosphere.

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“…Wavenumber IH waves were found at equatorial latitudes at depths between PUH mbar and I bar by several authors (Magalhaes et al, 1989;Orton et al, 1994;Harrington et al, 1996;Deming et al, 1997). The source of the waves is unknown and hypothesis range from vertical propagation of Rossby waves (Orton et al, 1994) and mixed Rossbygravity waves (Deming et al, 1997), to connection with the plumes in the equatorial hot-spots (Ortiz et al, 1998;Showman and Dowling, 2000) or association with deep convective cells (Magalhaes et al, 1989). The near stationary appearance of these waves with respect to system III implies possibly a dynamical link between the interior bulk rotation of the planet (Irwin, 2003).…”

Section: The Thermal Structurementioning

confidence: 95%

Turbulent convection in an anelastic rotating sphere : a model for the circulation on the giant planets

Kaspi¹

2008

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This thesis studies the dynamics of a rotating compressible gas sphere, driven by internal convection, as a model for the dynamics on the giant planets. We develop a new general circulation model for the Jovian atmosphere, based on the MITgcm dynamical core augmenting the nonhydrostatic model. The grid extends deep into the planet's interior allowing the model to compute the dynamics of a whole sphere of gas rather than a spherical shell (including the strong variations in gravity and the equation of state). Dierent from most previous 3D convection models, this model is anelastic rather than Boussinesq and thereby incorporates the full density variation of the planet.We show that the density gradients caused by convection drive the system away from an isentropic and therefore barotropic state as previously assumed, leading to signicant baroclinic shear. This shear is concentrated mainly in the upper levels and associated with baroclinic compressibility eects. The interior ow organizes in large cyclonically rotating columnar eddies parallel to the rotation axis, which drive upgradient angular momentum eddy uxes, generating the observed equatorial superrotation. Heat uxes align with the axis of rotation, contributing to the observed at meridional emission. We show the transition from weak convection cases with symmetric spiraling columnar modes similar to those found in previous analytic linear theory, to more turbulent cases which exhibit similar, though less regular and solely cyclonic, convection columns which manifest on the surface in the form of waves embedded within the superrotation. We develop a mechanical understanding of this system and scaling laws by studying simpler congurations and the dependence on physical properties such as the rotation period, bottom boundary location and forcing structure.These columnar cyclonic structures propagate eastward, driven by dynamics similar to that of a Rossby wave except that the restoring planetary vorticity gradient 3 is in the opposite direction, due to the spherical geometry in the interior. We further study these interior dynamics using a simplied barotropic annulus model, which shows that the planetary vorticity radial variation causes the eddy angular momentum ux divergence, which drives the superrotating equatorial ow. In addition we study the interaction of the interior dynamics with a stable exterior weather layer, using a quasigeostrophic two layer channel model on a beta plane, where the columnar interior is therefore represented by a negative beta eect. We nd that baroclinic instability of even a weak shear can drive strong, stable multiple zonal jets. For this model we nd an analytic nonlinear solution, truncated to one growing mode, that exhibits a multiple jet meridional structure, driven by the nonlinear interaction between the eddies. Finally, given the density eld from our 3D convection model we derive the high order gravitational spectra of Jupiter, which is a measurable quantity for the upcoming JUNO mission to Jupiter. Glenn Flierl, my...

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Observations and Analysis of Longitudinal Thermal Waves on Jupiter

Cited by 30 publications

References 23 publications

Jupiter's North Equatorial Belt expansion and thermal wave activity ahead of Juno's arrival

Jupiter's North Equatorial Belt expansion and thermal wave activity ahead of Juno's arrival

A system of circumpolar waves in Jupiter's stratosphere

Turbulent convection in an anelastic rotating sphere : a model for the circulation on the giant planets

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