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  • 1
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    Multi-Instrument Studies of Titan's Surface From Cassini (1997)
    In:  Other Sources
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    Publication Date: 2018-06-08
    Keywords: Earth Resources and Remote Sensing
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  • 2
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    Revised Orbits of Saturn's Small Inner Satellites (2007)
    In:  Other Sources
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    Publication Date: 2018-06-11
    Description: We have updated the orbits of the small inner Saturnian satellites using additional Cassini imaging observations through 2007 March. Statistically significant changes from previously published values appear in the eccentricities and inclinations of Pan and Daphnis, but only small changes have been found in the estimated orbits of the other satellites. We have also improved our knowledge of the masses of Janus and Epimetheus as a result of their close encounter observed in early 2006.
    Keywords: Astrophysics
    Type: The Astronomical Journal; Volume 135; 261
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  • 3
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    Liquid Hydrocarbons on Titan's Surface? How Cassini ISS Observations Fit into the Story (So Far) (2005)
    In:  CASI
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    Publication Date: 2017-10-02
    Description: Titan is the only satellite in our Solar System with a substantial atmosphere, the origins and evolution of which are still not well understood. Its primary (greater than 90%) component is nitrogen, with a few percent methane and lesser amounts of other species. Methane and ethane are stable in the liquid state under the temperature and pressure conditions in Titan s lower atmosphere and at the surface; indeed, clouds, likely composed of methane, have been detected. Photochemical processes acting in the atmosphere convert methane into more complex hydrocarbons, creating Titan s haze and destroying methane over relatively short timescales. Therefore, it has been hypothesized that Titan s surface has reservoirs of liquid methane which serve to resupply the atmosphere. Early observations of Titan s surface revealed albedo patterns which have been interpreted as dark hydrocarbon liquids occupying topographically low regions between higher-standing exposures of bright, water-ice bedrock, although this is far from being the only explanation for the observed albedo contrast. Observations made by the Imaging Science Subsystem during Cassini's approach to Saturn and its first encounters with Titan show the bright and dark regions in greater detail but have yet to resolve the question of whether there are liquids on the surface.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXVI, Part 19; LPI-Contrib-1234-Pt-19
    Format: application/pdf
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  • 4
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    Cassini ISS observations of Jupiter's polar haze (2001)
    In:  Other Sources
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    Publication Date: 2018-06-08
    Keywords: Lunar and Planetary Science and Exploration
    Type: 33rd Annual Meeting of the Division of Planetary Sciences; New Orleans, LA; United States
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  • 5
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    Saturn's rings - Structure, dynamics, and particle properties (1984)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: The current state of knowledge of Saturn's rings is reviewed. A brief historical introduction is given, followed by a discussion of the radial profile of the rings, ring dynamics, features without azimuthal symmetry, ring particle size distribution, and the physical properties of ring particles. The direction for future analysis and observation is considered.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 6
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    Cassini Imaging of Saturn: Southern Hemisphere Winds and Vortices (2006)
    In:  Other Sources
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    Publication Date: 2018-06-11
    Description: High-resolution images of Saturn's southern hemisphere acquired by the Cassini Imaging Science Subsystem between February and October 2004 are used to create maps of cloud morphology at several wavelengths, to derive zonal winds, and to characterize the distribution, frequency, size, morphology, color, behavior, and lifetime of vortices. Nonequatorial wind measurements display only minor differences from those collected since 1981 and reveal a strong, prograde flow near the pole. The region just southward of the velocity minimum at 40.7 deg S is especially active, containing numerous vortices, some generated in the proximity of convective storms. The two eastward jets nearest the pole display periodicity in their longitudinal structure, but no direct analogs to the northern hemisphere's polar hexagon or ribbon waves were observed. Characteristics of winds and vortices are compared with those of Saturn's northern hemisphere and Jupiter's atmosphere.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Journal Of Geophysical Research (ISSN 0148-0227); Volume 111
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  • 7
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    The periodic variation of spokes in Saturn's rings (1982)
    In:  Other Sources
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    Publication Date: 2019-06-28
    Description: The discovery of a periodic variation in spoke activity in Saturn's rings from the analysis of Voyager images is reported. A Fourier power spectrum was computed using a data set generated by quantifying spoke activity observed on the morning (western) half of the rings in Voyager images spanning 5.5 days (about 12 Saturn rotations). A peak approximately 14 sigma above the noise in the frequency domain was found at a period of 621 + or - 22 min. Within the formal error, this value is consistent with the 639.4-min rotation period of Saturn's magnetic field. Maximum spoke activity is most likely to be observed on the morning half of the rings when a particular magnetic field sector coincides with this area. This magnetic sector contains the region which is aligned with local noon at the time of the emission of the SKR (Saturn kilometric radiation). These results suggest that the fundamental period of spoke variation is that of Saturn's magnetic field, and that spoke activity is associated with the region of the field which gives rise to the SKR. Passage of this region through Saturn's shadow may play a significant role in the creation and/or rejuvenation of spokes.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Astronomical Journal; 87; May 1982
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  • 8
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    On the presence of phyllosilicate minerals in the interstellar grains (1975)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The composition of the interstellar silicate dust is investigated. Condensation or alteration of silicate grains at temperatures of a few hundred degrees, in the presence of H2O, would result in hydrous or phyllosilicates, the silicate type most abundant in the type I carbonaceous chondrites. Infrared spectra of small particles (about 0.1 microns) of the high temperature condensates, olivine and pyroxene, at 300 K and 4 K do not give a good match to the interstellar absorption band near 9.8 microns. Laboratory spectra of several phyllosilicates give better agreement as does the spectrum of a carbonaceous chondrite. We propose that the silicates in the interstellar grains are predominantly phyllosilicates and suggest additional spectral tests for this hypothesis.
    Keywords: ASTROPHYSICS
    Type: Astrophysics and Space Science; 35; June 197
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  • 9
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    Saturn's Rings: Pre-Cassini Status and Mission Goals (2001)
    In:  Other Sources
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    Publication Date: 2019-07-18
    Description: Theoretical and observational progress in studies of Saturn's ring system since the mid-1980s is reviewed, focussing on advances in configuration and dynamics, composition and size distribution, dust and meteoroids, interactions of the rings with the planet and the magnetosphere, and relationships between the rings and various satellites. The Cassini instrument suite of greatest relevance to ring studies is also summarized, emphasizing how the individual instruments might work together to solve outstanding problems. The Cassini tour is described from the standpoint of ring studies, and major ring science goals are summarized.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Solar System Decadal Panel on Outer Planets; Unknown
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  • 10
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    The occultation of SAO 78505 by Jupiter (1995)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: On 13 December 1989, Jupiter occulted a star with visual magnitude 8.7 and an estimated K magnitude of 7. We observed the event from Kitt Peak, Arizona, using a 64 x 64 infrared camera at a wavelength of 2.16 microns. The resulting data on refractive defocusing of the stellar signal give information on the temperature of the jovian atmosphere at pressures approximately 2 to 10 microbar, at near-equatorial latitudes. These are the first new stellar-occulation data for the high jovian atmosphere since the widely observed occulation of beta Sco A and C in 1971. Because of improvements in instrumental capability, our data are comparable to the best beta Sco A data though the star is six magnitudes fainter. We derive a mean atmospheric temperature of 176 +/- 12 K on a level surface corresponding to an equatorial radius of 71,880 km and a pressure of 1.8 microbar at a jovi- centric latitude of 8 deg. This result complements the beta Sco results by providing improved precision at low jovicentric latitudes where the fainter star beta Sco C was used in 1971.
    Keywords: ASTRONOMY
    Type: Icarus (ISSN 0019-1035); 113; 1; p. 103-109
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