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  • Other Sources  (9)
  • 1985-1989  (9)
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  • 1
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    Cratering history of the Uranian satellites - Umbriel, Titania, and Oberon (1987)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: Crater size-frequency data for Umbriel, Titania, and Oberon are presented, and the implications of those data are discussed in terms of the geologic histories of these bodies and the populations of objects that have cratered them. The surfaces of Oberon and Umbriel are old and are inferred to date to a period early in their histories when the cratering rate was significantly higher than at present. No significant endogenic resurfacing appears to have occurred on either body after that inferred period of intense cratering. Titania exhibits the youngest surface of these three and appears to have undergone almost complete endogenic resurfacing. Among the Uranian satellites the surfaces of Oberon and Umbriel are interpreted to be the oldest, that of Titania intermediate, and those of Ariel and parts of Miranda the youngest. The size-frequency distributions for these satellites have an average slope of about -3, indicative of a steep crater production function. The cumulative size-frequency data for these Uranian satellites may be interpreted to indicate that parts of their surfaces are saturated with craters at small diameters.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research (ISSN 0148-0227); 92; 14918-14
    Format: text
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    NASA TECHNICAL REPORTS
  • 2
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    Impact cratering history of the Saturnian satellites (1985)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: The impact flux history of the Saturn system has been modelled, and absolute ages estimated. The model assumes that the general history of impact flux was similar to that of the inner solar system and that the dominant source of material in the postaccretionary phases was external to the Saturn system. Population I and II craters represent the synheavy and postheavy bombardment periods, respectively. Observed crater densities are representative of the actual ages and do not appear to be saturation-equilibrium surfaces. It is concluded that some of the satellites have geologic histories which extend to about 3.5 b.y. Significant endogenic resurfacing has occurred on several satellite surfaces, which indicates that thermal conditions and material compositions are more complicated than might have been anticipated prior to Voyager encounters.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research (ISSN 0148-0227); 90; 2029-203
    Format: text
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  • 3
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    Late-stage flood lavas in the Elysium region, Mars (1987)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: In the southeastern part of the Elysium region is a unit that exhibits little texture and a generally low albedo and that has a very low crater frequency. This unit has been mapped as smooth plains material and previously interpreted as an eolian deposit on the basis of Mariner 9 images. More recently, the unit was mapped as material deposited during a channeling episode. The author interprets the smooth plains unit as being a volcanic deposit composed of low viscosity lava flows: both flood lavas and individual flows. The reasons for these conclusions are given and briefly discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1986; p 336-338
    Format: application/pdf
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  • 4
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    Orbital dynamics of the Uranian satellites based on Voyager data (1987)
    In:  CASI
    Details
    Publication Date: 2013-08-31
    Description: The satellites of Uranus all have significant non-zero eccentricities and in the case of Miranda a significant inclination as well. The Voyager 2 encounter with Uranus in January 1986, provided more accurate estimates of the masses and sizes of the satellites. Orbital history and possible tidal heating were reexamined by using the Voyager data. The relevant orbital dynamics equations are described.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA, Washington, Reports of Planetary Geology and Geophysics Program, 1986; p 23-25
    Format: application/pdf
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  • 5
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    Terrestrial Analogs for Planetary Wrinkle Ridges (1985)
    In:  CASI
    Details
    Publication Date: 2014-10-09
    Description: Wrinkle ridges are common physiographic features on the terrestrial planets. Their origin has remained enigmatic, although two different types of models, volcanic and tectonic, have been proposed. The major impediment to deciphering the origin of wrinkle ridges has been the lack of a terrestrial analog. Seven terrestrial analogs were discussed, two in detail. Their implications for the origin for planetary wrinkle ridges were considered. All of the terrestrial analogs were formed in compressional environments and are the surface breaks of thrust faults.
    Keywords: GEOPHYSICS
    Type: NASA, Washington Repts. of Planetary Geol. and Geophys. Program, 1984; p 482-484
    Format: text
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  • 6
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    Chronology of surface units on the icy satellites of Saturn (1985)
    In:  Other Sources
    Details
    Publication Date: 2019-08-13
    Description: Because the impact flux history in the Saturnian system has been similar in its general form to that for the inner solar system and Jupiter, it is possible to develop an absolute calibration model for the relative ages derived from the density of impact craters. This has been done by identifying the density at which the crater populations change characteristics from that during post-accretion heavy bombardment to a later population of low but continuous flux. The transition between these two populations occurred at a known time throughout the solar system, 3.9 by, and provides an absolute calibration point on which to construct a calibration curve. Results based on calibrating relative age data to this absolute flux model suggest that most surfaces are ancient, greater than 3.9 by (or within several 100 million years). Only Enceladus and Dione have had prolonged activity that has resulted in resurfacing. The activity on Enceladus was probably driven by tidal forces, whereas the mechanism for driving resurfacing on Dione has yet to be identified.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Format: text
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  • 7
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    Cratering history of Miranda - Implications for geologic processes (1988)
    In:  Other Sources
    Details
    Publication Date: 2019-08-27
    Description: The terrain of Miranda, which is the least cratered and therefore pressumably youngest of the Uranian moons, encompasses more heavily cratered and coronae regions, of which the former are, again pressumably, the oldest. The coronae are also variably cratered; of these, Elsinore and Arden Coronae have similar, intermediate crater frequencies, and may therefore have formed simultaneously. The Inverness Corona is the youngest of the major terrains. Periods of global expansion are implied by grabben formation that may have occurred both before and after the formation of the coronae.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus (ISSN 0019-1035); 442-461
    Format: text
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  • 8
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    Cratering history of Miranda (1987)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: The surface of the southern hemisphere of Miranda imaged by Voyager 2 is divisible into two general types of terrain: cratered terrain, characterized by numerous craters and undulating intercrater plains; and basins, circular to rectangular areas of complex morphology having large-scale albedo markings. To determine the relative ages of the terrains and the length of geological activity, crater-frequency data were compiled for various parts of the cratered terrain and basins. Crater-frequency data indicate that the cratered terrain is the oldest terrain on Miranda and that it was locally resurfaced.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Reports of Planetary Geology and Geophysics Program, 1986; p 9-11
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  • 9
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    Geology and cratering history of Ariel (1987)
    In:  CASI
    Details
    Publication Date: 2019-08-28
    Description: The surface of Ariel imaged by Voyager 2 can be divided into several types of terrain on the basis of morphology: cratered terrain, subdued terrain, ridged terrain, and plains. Crater statistics were compiled for each of the terrain types. Despite differing morphology, the various terrains on Ariel do not exhibit large variations in crater frequency. None of the observed surfaces on Ariel record the period of accretion. It seems that conditions appropriate for resurfacing could have occurred during the early history of Ariel.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Reports of Planetary Geology and Geophysics Program, 1986; p 19-21
    Format: application/pdf
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