Cassini Imaging of Jupiter's Atmosphere, Satellites, and Rings

Porco, C. C.; West, Robert A.; McEwen, A. S.; Genio, Anthony D. Del; Ingersoll, Andrew P.; Thomas, P. C.; Squyres, S. W.; Dones, L.; Murray, C. D.; Johnson, T. V.; Burns, Joseph A.; Brahic, A.; Neukum, G.; Veverka, J.; Barbara, J.; Denk, T.; Evans, Michael; Ferrier, Joseph; Geissler, P. E.; Helfenstein, P.; Roatsch, Thomas; Throop, H. B.; Tiscareno, Matthew S.; Vasavada, A. R.

doi:10.1126/science.1079462

Cited by 431 publications

(478 citation statements)

References 53 publications

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“…1. The zonal wind profile at cloud level is very similar to previously known profiles [1] showing no significant differences. The meridional wind values are at the images resolution limit but they are never higher than 2 ms -1 .…”

Section: Zonal and Meridional Wind Profilessupporting

confidence: 70%

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: Zonal and Meridional Wind Profilessupporting

confidence: 70%

Dynamics and Clouds in Jupiter Equatorial Zone

Arregi

Rojas

Hueso

et al. 2010

Astrophysics and Space Science Proceedings

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“…where u cl (θ ) are the observed cloud level winds [38]. Varying systematically the free parameter H gives a continuous set of wind profiles, which depend on one parameter that allows us to explore the dynamic gravity harmonics resulting from the wind.…”

Section: S2 Calculating the Dynamical Contribution To Jmentioning

confidence: 99%

Atmospheric confinement of jet streams on Uranus and Neptune

Kaspi

Showman

Hubbard

et al. 2013

Nature

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Supplementary Informationvalues we use a suite of core/envelope internal structure models, with a wide range of core depths, core densities and envelope density profiles.The core is taken to be of constant density with the core density ranging between 0.8 × 10 4 < ρ core < 1.2 × 10 4 kg m −3 , and core radius extending up to 30% of the planetary radius on Neptune (0 < r core < 0.3 R, where R is the mean planetary radius), and 20% on Uranus, following the widest possible range of core densities given by [16, 17, 19]. We systematically explore this parameter space where for each case of ρ core and r core we then match an envelope represented by a 6th order polynomial with a monotonic density distribution so that ρ static = ρ core for 0 < r < r core (S1)where β = r/R is the normalized radius. The coefficients (a n ) are determined by constraints on the static density (ρ static ). The first constraint on the static density is that the density is zero at the surface, satisfied by setting the sum of the six polynomial coefficients to zero at β = 1. The second constraint is that the integrated density over the entire volume must equal to the planetary mass.The third constraint is that the density derivative at β = 1 equals the derivative of the density at the 1 bar pressure level (equal to -0.1492 and -0.2425 kg m −4 for Uranus and Neptune respectively,[31]). The first degree term in Eq. S2 is missing so that the derivative of the density goes to zero at the center for models with no core, and another constraint sets this value to zero at the core-envelope boundary for models with cores. The last constraint limits the value of J 2 to within the error estimates of the observed value of 3341.29 ± 0.72 × 10 −6 and 3408.43 ± 4.50 × 10 −6 for 1 Uranus and Neptune respectively [14, 15]. Since we are interested in determining the resulting J 4 we do not impose any constraints on J 4 , as done in most studies where the J 4 is constrained to within the observed values of J 4 (e.g., [13]). For cases with no core the density at β = 0 is not constrained, and its derivative at β = 0 is set to zero.Uranus Neptune 25

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“…With Cassini's December 2000 flyby, Jupiter was once again under scrutiny. Images in methane absorption bands revealed a diffuse pattern with wavenumber ∼14-18 over the NEB [Porco et al, 2003;Rogers et al, 2004]. Spectral maps of Jupiter at 7-16 µm revealed a series of wave-like NEB features near 250 mbar [Flasar et al, 2004], which were explored via near-simultaneous methane-band and thermal observations by Li et al [2006].…”

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

confidence: 99%

“…Rogers [2017] estimates 5-7 months for the completion of the expansion (except in 2000, where events proceeded more slowly), with a revival of the NTrZ white coloration (i.e., southward recession of the NEB) starting anywhere from 1-3 years post expansion, although these estimates are subjective and based on incomplete temporal sampling. [Porco et al, 2003] in equirectangular coordinates. A full historical overview can be found in [Rogers, 2017].…”

Section: A1 Supplemental S1: History Of Neb Expansions 1987-2012mentioning

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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Cassini Imaging of Jupiter's Atmosphere, Satellites, and Rings

Cited by 431 publications

References 53 publications

Dynamics and Clouds in Jupiter Equatorial Zone

Dynamics and Clouds in Jupiter Equatorial Zone

Atmospheric confinement of jet streams on Uranus and Neptune

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

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