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  • 1
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    A close-up look at Io from Galileo's near-infrared mapping spectrometer (2000)
    In:  Other Sources
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    Publication Date: 2011-08-24
    Description: Infrared spectral images of Jupiter's volcanic moon Io, acquired during the October and November 1999 and February 2000 flybys of the Galileo spacecraft, were used to study the thermal structure and sulfur dioxide distribution of active volcanoes. Loki Patera, the solar system's most powerful known volcano, exhibits large expanses of dark, cooling lava on its caldera floor. Prometheus, the site of long-lived plume activity, has two major areas of thermal emission, which support ideas of plume migration. Sulfur dioxide deposits were mapped at local scales and show a more complex relationship to surface colors than previously thought, indicating the presence of other sulfur compounds.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Science (ISSN 0036-8075); Volume 288; 5469; 1201-4
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  • 2
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    Triton's geyser-like plumes - Discovery and basic characterization (1990)
    In:  Other Sources
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    Publication Date: 2011-08-19
    Description: One model for the mechanism driving the plumes of the four active geyser-like eruptions observed by Voyager 2 on Triton is a heating up of nitrogen ice in a subsurface greenhouse environment, where nitrogen gas pressurized by solar heating explosively vents to the surface carrying clouds of ice and dark particles into the atmosphere. A temperature increase of less than 4 K above the ambient surface value of 38 + or - 3 K suffices to drive the plumes to 8-km altitude. Each eruption may last a year or more, over the course of which 0.1 cu km of ice is sublimed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Science (ISSN 0036-8075); 250; 410-415
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  • 3
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    A Close-Up View of Io in the Infrared: NIMS Results from the Galileo Fly-Bys (2000)
    In:  Other Sources
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    Publication Date: 2017-10-02
    Description: We report the initial results obtained by the Galileo Near-Infrared Mapping Spectrometer during the fly-bys of Io. Our data reveals, for the first time, the detailed thermal structure of hot spots and the local distribution of SO2 frost.
    Keywords: Lunar and Planetary Science and Exploration
    Type: Lunar and Planetary Science XXXI; LPI-Contrib-1000
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  • 4
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    Low-velocity impact craters in ice and ice-saturated sand with implications for Martian crater count ages (1979)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The paper reports on a series of low-velocity impact experiments performed in ice and ice-saturated sand. It is found that crater diameters in ice-saturated sand were about 2 times larger than in the same energy and velocity range in competent blocks of granite, basalt and cement, while craters in ice were 3 times larger. It is shown that if this dependence of crater size on strength persists to large hypervelocity impact craters, then surface of geologic units composed of ice or ice-saturated soil would have greater crater count ages than rocky surfaces with identical influx histories. Among the conclusions are that Martian impact crater energy versus diameter scaling may also be a function of latitude.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research; 84; Dec. 30
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  • 5
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    The role of volatiles and lithology in the impact cratering process (1980)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: A survey of published descriptions of 32 of the largest, least eroded terrestrial impact structures shows that the amount of melt at craters in crystalline rocks is approximately two orders of magnitude greater than that at craters in sedimentary rocks. A model is proposed for the impact process, and it is examined whether the difference in melt abundance is due to differences in the amount of melt generated in various target materials or due to differences in the fate of the melt during late stages of the impact. The model accounts semiquantitatively for the effects of porosity and water and volatile content on the cratering process. Important features of the model are noted. Even if the recondensation of released volatiles is very efficient, the cumulative effect of repeated impacts on accreting planets would be to continually transfer volatiles toward the outer surface. By this process, volatiles might be enriched toward the outer layer of a growing planet.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Reviews of Geophysics and Space Physics; 18; Feb. 198
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  • 6
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    A constraint on impact theories of chondrule formation (1977)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The association between agglutinates and chondrule-like spherules, which characterizes the assemblage of impact-derived melt products in lunar regolith samples and some gas-rich achondrites, is not found in primitive chondrites. This observation suggests that impacts into a parent-body regolith are unlikely to have produced the chondrules. We believe that if chondrules were formed from impact melt, it was probably generated by jetting during particle-to-particle collisions, presumably in the nebula.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Earth and Planetary Science Letters; 35; 1, Ma; May 1977
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  • 7
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    From regolith to rock by shock (1975)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: The purpose of this study is to relate the various mechanisms by which material is shock-lithified in terrestrial analogs of the lunar regolith to specific conditions of cratering, thereby making more specific the possible conditions of formation of rock from regolith by shock processes on the lunar surface. A model for shock-lithification of terrestrial and lunar regolith is proposed in which air or an air-water mixture initially in the pores of terrestrial soil affects the behavior of a soil-air-water system under shock-loading. Shock compression of porous terrestrial regolith by relatively small impact events give rise to three pressure regimes: (1) regime 1 - at pressures below 100 kb, material is compacted and weakly shock-lithified; (2) regime 2 - at pressures between 100 and 200 kb, material may be fragmented if the induced pore pressure exceeds the strength of the weak lithification mechanisms; and (3) at pressure above 200 kb, material is strongly lithified but may greatly expand in volume due to the pressure of pore gases. The three other regimes (below 50 kb, between 50 and 100 kb, and above 100 kb) associated with shock compression of lunar regolith are identified and discussed.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 8
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    Concerning the meteoritic origin of the Puchezh-Katunki crater (1973)
    In:  Other Sources
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    Publication Date: 2019-06-27
    Description: Criticism of the works of Vardaniants (1961) and Goretskii (1962) regarding the origin of the Puchezh-Katunki crater, and development of a new hypothesis regarding this disturbance. Although Vardaniants defines the Puchezh-Katunki disturbance as a structure of explosive nature and assumes that the explosion originated as a consequence of accumulation of gases in the crystalline basement of the Russian platform, he lacks evidence to qualify this explosion as coming from a depth. Goretskii's tectonic-injection hypothesis attributes the formation of the disturbance to penetration of an intrusion of basic and ultrabasic rocks into the Paleozoic rocks of the platform. It is shown that, even if the intrusion were spread somewhere at depth, it could not account for the extent of the deformation in the disturbance. It is suggested that this disturbance is of meteoritic origin, since the structure and morphology of the region are similar to the sloping conical surface produced by an explosive meteor crater. The energy, mass, and size of the asteroid which could cause such a disturbance are estimated, and it is shown that the probability of the occurrence of an impact of this size is finite over geological time.
    Keywords: SPACE SCIENCES
    Type: Meteoritics; 8; Sept. 30
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  • 9
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    Impact conditions required for formation of melt by jetting in silicates (1977)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: It is demonstrated that the process of jetting which occurs when particles collide at oblique angles may produce melt at much lower velocities than are required for melt production in head-on collisions. The minimum velocities of impact required for jetting in aluminum, bronzitite, dunite, and quartz are calculated by the method of shock polars. The analysis, which depends on stated assumptions about attained pressures and the occurrence of jetting, uses shock-velocity particle-velocity equations of state with three shock regimes. The treatment indicates that jetting should arise in bronzitite, dunite, and quartz at relative velocities as low as 1-2 km/sec. At such velocities material which passes near the stagnation point in the jet-forming region is subjected to sufficiently high pressures so that it is probably melted.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Symposium on Planetary Cratering Mechanics; Sep 13, 1976 - Sep 17, 1976; Flagstaff, AZ
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  • 10
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    Shocked basalt from Lonar Impact Crater, India, and experimental analogues (1976)
    In:  Other Sources
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    Publication Date: 2019-07-13
    Description: Samples of Lonar basalts were experimentally shocked in vacuum to pressures between 200 and 650 kbar by a 20 mm, high-velocity gun. Plagioclase and palagonite in experimentally shocked samples show deformation similar to that in the naturally shocked rocks, but pyroxene does not show optically resolvable edge melting. It is estimated that pressures in excess of 800-1000 kbar are required for the formation of totally shock-melted rocks from nonporous basalt.
    Keywords: EARTH RESOURCES AND REMOTE SENSING
    Type: Lunar Science Conference; Mar 15, 1976 - Mar 19, 1976; Houston, TX
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