Evolution and persistence of 5‐μm hot spots at the Galileo probe entry latitude

Ortiz, J. L.; Orton, Glenn S.; Friedson, A. J.; Stewart, S. T.; Fisher, B.; Spencer, J. R.

doi:10.1029/98je00696

Cited by 93 publications

(91 citation statements)

References 36 publications

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“…3 [3]. Interestingly these values are similar to the ones that Ortiz et al [4] found when studying the hot spots movement in the IR. After this we tried to apply the same interpretation to the symmetrical marks appearing in the southern limit of the SEB (7º S).…”

Section: Hot Spotssupporting

confidence: 77%

Dynamics and Clouds in Jupiter Equatorial Zone

Arregi

Rojas

Hueso

et al. 2010

Astrophysics and Space Science Proceedings

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In this work we show a study of the dynamics and clouds in the equatorial zone of Jupiter. The studied area is wider than the pure Equatorial Zone (EZ) ranging from the southern limit of the South Equatorial Belt (SEB) to the northern limit of the North Equatorial Belt (NEB).We have used images from the Cassini flyby in December 2000 (wavelengths of 752 and 939 nm)) and from the Galileo orbiter taken in 1999 and 2001 (wavelengths of 559 and 756 nm). When needed we have used images from the International Outer Planet Watch (IOPW) database to complete the time coverage of the dataset.In visible wavelengths the study of the dark-bluish regions in the northern limit of the NEB that corresponds to the infrared (IR) "hot spots" show that they have the characteristics of a Rossby wave and can be explained as some Rossby wave induced effect. Nevertheless trying to explain the smaller and more abundant dark marks situated on the southern limit of the SEB in the same way has proven to be much more difficult. We will describe too our measurements of an anticyclonic white oval situated near the SEB dark marks.Finally we will present three train gravity waves that we have found in Galileo maps near the Equator.

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Section: Hot Spotssupporting

confidence: 77%

Dynamics and Clouds in Jupiter Equatorial Zone

Arregi

Rojas

Hueso

et al. 2010

Astrophysics and Space Science Proceedings

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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: 99%

“…This result is often used as evidence that the winds are deep, though one should remember that beyond the point that this is just a single measurement, the data only accounts for a depth of ISH km which are no more than H:PP% of the radius of Jupiter. In addition the probe entered in a hot-spot (the equatorial zone is punctuated with 10-13 such S m spots (Ortiz et al, 1998)), which may have anomalous dynamics because of non-zonal motions that have been associated with them .…”

Section: The Wind Structurementioning

confidence: 99%

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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“…Note that this section does not deal with the trapped equatorial Rossby wave pattern on the NEBs [and its associated hotspots and plumes, Allison, 1990;Ortiz et al, 1998;Showman and Dowling, 2000;Baines et al, 2002;Friedson, 2005;Arregi et al, 2006;Choi et al, 2013].…”

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

confidence: 99%

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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Evolution and persistence of 5‐μm hot spots at the Galileo probe entry latitude

Cited by 93 publications

References 36 publications

Dynamics and Clouds in Jupiter Equatorial Zone

Dynamics and Clouds in Jupiter Equatorial Zone

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

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

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