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Giant Planet Atmospheres: Dynamics and Variability from UV to Near-IR Hubble and Adaptive Optics Imaging. REMOTE SENSING 2022. [DOI: 10.3390/rs14061518] [Citation(s) in RCA: 1] [Impact Index Per Article: 0.5] [Reference Citation Analysis] [Abstract] [Track Full Text] [Subscribe] [Scholar Register] [Indexed: 12/10/2022]
Abstract
Each of the giant planets, Jupiter, Saturn, Uranus, and Neptune, has been observed by at least one robotic spacecraft mission. However, these missions are infrequent; Uranus and Neptune have only had a single flyby by Voyager 2. The Hubble Space Telescope, particularly the Wide Field Camera 3 (WFC3) and Advanced Camera for Surveys (ACS) instruments, and large ground-based telescopes with adaptive optics systems have enabled high-spatial-resolution imaging at a higher cadence, and over a longer time, than can be achieved with targeted missions to these worlds. These facilities offer a powerful combination of high spatial resolution, often <0.05”, and broad wavelength coverage, from the ultraviolet through the near infrared, resulting in compelling studies of the clouds, winds, and atmospheric vertical structure. This coverage allows comparisons of atmospheric properties between the planets, as well as in different regions across each planet. Temporal variations in winds, cloud structure, and color over timescales of days to years have been measured for all four planets. With several decades of data already obtained, we can now begin to investigate seasonal influences on dynamics and aerosol properties, despite orbital periods ranging from 12 to 165 years. Future facilities will enable even greater spatial resolution and, combined with our existing long record of data, will continue to advance our understanding of atmospheric evolution on the giant planets.
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Fischer G, Kurth WS, Gurnett DA, Zarka P, Dyudina UA, Ingersoll AP, Ewald SP, Porco CC, Wesley A, Go C, Delcroix M. A giant thunderstorm on Saturn. Nature 2011; 475:75-7. [DOI: 10.1038/nature10205] [Citation(s) in RCA: 103] [Impact Index Per Article: 7.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Received: 02/10/2011] [Accepted: 05/17/2011] [Indexed: 11/09/2022]
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Fischer G, Gurnett DA, Zarka P, Moore L, Dyudina UA. Peak electron densities in Saturn's ionosphere derived from the low-frequency cutoff of Saturn lightning. ACTA ACUST UNITED AC 2011. [DOI: 10.1029/2010ja016187] [Citation(s) in RCA: 20] [Impact Index Per Article: 1.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
Affiliation(s)
- G. Fischer
- Space Research Institute; Austrian Academy of Sciences; Graz Austria
- Department of Physics and Astronomy; University of Iowa; Iowa City Iowa USA
| | - D. A. Gurnett
- Department of Physics and Astronomy; University of Iowa; Iowa City Iowa USA
| | - P. Zarka
- Observatoire de Paris; Meudon France
| | - L. Moore
- Center for Space Physics; Boston University; Boston Massachusetts USA
| | - U. A. Dyudina
- Geological and Planetary Sciences; California Institute of Technology; Pasadena California USA
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Smith BA, Soderblom LA, Beebe R, Bliss D, Boyce JM, Brahic A, Briggs GA, Brown RH, Collins SA, Cook AF, Croft SK, Cuzzi JN, Danielson GE, Davies ME, Dowling TE, Godfrey D, Hansen CJ, Harris C, Hunt GE, Ingersoll AP, Johnson TV, Krauss RJ, Masursky H, Morrison D, Owen T, Plescia JB, Pollack JB, Porco CC, Rages K, Sagan C, Shoemaker EM, Sromovsky LA, Stoker C, Strom RG, Suomi VE, Synnott SP, Terrile RJ, Thomas P, Thompson WR, Veverka J. Voyager 2 in the uranian system: imaging science results. Science 2010; 233:43-64. [PMID: 17812889 DOI: 10.1126/science.233.4759.43] [Citation(s) in RCA: 81] [Impact Index Per Article: 5.8] [Reference Citation Analysis] [Abstract] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Abstract
Voyager 2 images of the southern hemisphere of Uranus indicate that submicrometersize haze particles and particles of a methane condensation cloud produce faint patterns in the atmosphere. The alignment of the cloud bands is similar to that of bands on Jupiter and Saturn, but the zonal winds are nearly opposite. At mid-latitudes (-70 degrees to -27 degrees ), where winds were measured, the atmosphere rotates faster than the magnetic field; however, the rotation rate of the atmosphere decreases toward the equator, so that the two probably corotate at about -20 degrees . Voyager images confirm the extremely low albedo of the ring particles. High phase angle images reveal on the order of 10(2) new ringlike features of very low optical depth and relatively high dust abundance interspersed within the main rings, as well as a broad, diffuse, low optical depth ring just inside the main rings system. Nine of the newly discovered small satellites (40 to 165 kilometers in diameter) orbit between the rings and Miranda; the tenth is within the ring system. Two of these small objects may gravitationally confine the e ring. Oberon and Umbriel have heavily cratered surfaces resembling the ancient cratered highlands of Earth's moon, although Umbriel is almost completely covered with uniform dark material, which perhaps indicates some ongoing process. Titania and Ariel show crater populations different from those on Oberon and Umbriel; these were probably generated by collisions with debris confined to their orbits. Titania and Ariel also show many extensional fault systems; Ariel shows strong evidence for the presence of extrusive material. About halfof Miranda's surface is relatively bland, old, cratered terrain. The remainder comprises three large regions of younger terrain, each rectangular to ovoid in plan, that display complex sets of parallel and intersecting scarps and ridges as well as numerous outcrops of bright and dark materials, perhaps suggesting some exotic composition.
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Abstract
Despite major differences in the solar and internal energy inputs, the atmospheres of the four Jovian planets all exhibit latitudinal banding and high-speed jet streams. Neptune and Saturn are the windiest planets, Jupiter is the most active, and Uranus is a tipped-over version of the others. Large oval storm systems exhibit complicated time-dependent behavior that can be simulated in numerical models and laboratory experiments. The largest storm system, the Great Red Spot of Jupiter, has survived for more than 300 years in a chaotic shear zone where smaller structures appear and dissipate every few days. Future space missions will add to our understanding of small-scale processes, chemical composition, and vertical structure. Theoretical hypotheses about the interiors provide input for fluid dynamical models that reproduce many observed features of the winds, temperatures, and cloud patterns. In one set of models the winds are confined to the thin layer where clouds form. In other models, the winds extend deep into the planetary fluid interiors. Hypotheses will be tested further as observations and theories become more exact and detailed comparisons are made.
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Choi DS, Showman AP, Brown RH. Cloud features and zonal wind measurements of Saturn's atmosphere as observed by Cassini/VIMS. ACTA ACUST UNITED AC 2009. [DOI: 10.1029/2008je003254] [Citation(s) in RCA: 37] [Impact Index Per Article: 2.5] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Vasavada AR, Hörst SM, Kennedy MR, Ingersoll AP, Porco CC, Del Genio AD, West RA. Cassini imaging of Saturn: Southern hemisphere winds and vortices. ACTA ACUST UNITED AC 2006. [DOI: 10.1029/2005je002563] [Citation(s) in RCA: 76] [Impact Index Per Article: 4.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Porco CC, Baker E, Barbara J, Beurle K, Brahic A, Burns JA, Charnoz S, Cooper N, Dawson DD, Del Genio AD, Denk T, Dones L, Dyudina U, Evans MW, Giese B, Grazier K, Helfenstein P, Ingersoll AP, Jacobson RA, Johnson TV, McEwen A, Murray CD, Neukum G, Owen WM, Perry J, Roatsch T, Spitale J, Squyres S, Thomas P, Tiscareno M, Turtle E, Vasavada AR, Veverka J, Wagner R, West R. Cassini Imaging Science: Initial Results on Saturn's Atmosphere. Science 2005; 307:1243-7. [PMID: 15731441 DOI: 10.1126/science.1107691] [Citation(s) in RCA: 88] [Impact Index Per Article: 4.6] [Reference Citation Analysis] [Abstract] [MESH Headings] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/03/2022]
Abstract
The Cassini Imaging Science Subsystem (ISS) began observing Saturn in early February 2004. From analysis of cloud motions through early October 2004, we report vertical wind shear in Saturn's equatorial jet and a maximum wind speed of approximately 375 meters per second, a value that differs from both Hubble Space Telescope and Voyager values. We also report a particularly active narrow southern mid-latitude region in which dark ovals are observed both to merge with each other and to arise from the eruptions of large, bright storms. Bright storm eruptions are correlated with Saturn's electrostatic discharges, which are thought to originate from lightning.
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Affiliation(s)
- C C Porco
- Cassini Imaging Central Laboratory for Operations, Space Science Institute, 4750 Walnut Street, Suite 205, Boulder, CO 80301, USA.
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Sanchez-Lavega A, Lecacheux J, Gomez JM, Colas F, Laques P, Noll K, Gilmore D, Miyazaki I, Parker D. Large-Scale Storms in Saturn's Atmosphere During 1994. Science 1996. [DOI: 10.1126/science.271.5249.631] [Citation(s) in RCA: 37] [Impact Index Per Article: 1.3] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/02/2022]
Affiliation(s)
- A. Sanchez-Lavega
- A. Sanchez-Lavega, Departamento de Física Aplicada I, Escuelo Tecnica Superior Ingenieros, Universidad Pais Vasco, Alda. Urquijo s/n, 48013 Bilbao, Spain
| | - J. Lecacheux
- J. Lecacheux, Department des Recherches Spatiales, Observatoire Meudon, 92195 Meudon, France
| | - J. M. Gomez
- J. M. Gomez, Grup Estudis Astronomics, Apartado 9481, 08080 Barcelona, Spain
| | - F. Colas
- F. Colas, Bureau des Longitudes, 77 Avenue Denfert Rochereau, 75014 Paris, France
| | - P. Laques
- P. Laques, Observatoire Pic-du-Midi, 65200 Bagneres de Bigorre, France
| | - K. Noll
- K. Noll and D. Gilmore, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - D. Gilmore
- K. Noll and D. Gilmore, Space Telescope Science Institute, 3700 San Martin Drive, Baltimore, MD 21218, USA
| | - I. Miyazaki
- I. Miyazaki, Oriental Astronomical Association, Naha-shi, Okinawa, Japan
| | - D. Parker
- D. Parker, Association of Lunar and Planetary Observers, Coral Gables, FL 33156, USA
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Sanchez-Lavega A, Lecacheux J, Colas F, Laques P. Temporal behavior of cloud morphologies and motions in Saturn's atmosphere. ACTA ACUST UNITED AC 1993. [DOI: 10.1029/93je01777] [Citation(s) in RCA: 27] [Impact Index Per Article: 0.9] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/09/2022]
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Limaye SS, Sromovsky LA. Winds of Neptune: Voyager observations of cloud motions. ACTA ACUST UNITED AC 1991. [DOI: 10.1029/91ja01701] [Citation(s) in RCA: 41] [Impact Index Per Article: 1.2] [Reference Citation Analysis] [Track Full Text] [Journal Information] [Subscribe] [Scholar Register] [Indexed: 11/10/2022]
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Abstract
The hexagonal, pole-centered cloud feature in Saturn's northern atmosphere, as revealed in Voyager close-encounter imaging mosaics, may be interpreted as a stationary Rossby wave. The wave is embedded within a sharply peaked eastward jet (of 100 meters per second) and appears to be perturbed by at least one anticyclonic oval vortex immediately to the south. The effectively exact observational determination of the horizontal wave number and phase speed, applied to a simple model dispersion relation, suggests that the wave is vertically trapped and provides a diagnostic template for further modeling of the deep atmospheric stratification.
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