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  • LUNAR AND PLANETARY EXPLORATION  (7)
  • 1
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    Chemical and isotopic measurements of micrometeoroids by secondary ion mass spectrometry (A0187-2) (1984)
    In:  CASI
    Details
    Publication Date: 2006-02-14
    Description: The objective of this experiment is to measure the chemical and isotopic composition of interplanetary dust particles of mass greater than 10 to the minus 10 power G for most of thermator elements expected to be present.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: NASA. Langley Research Center Long Duration Exposure Facility (LDEF); p 131-134
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  • 2
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    The interplanetary micrometeoroid flux and lunar primary and secondary microcraters (1985)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: It is proposed that considerable care is required to properly interpret either spacecraft in situ data or lunar crater data as well as near-earth data; in the case of the former, complications may arise which may be attributed to secondary lunar ejecta impacts, in the latter, they may result from impacting earth-orbiting debris. Experimental evidence suggests that most impact pits on lunar rocks with pit diameters smaller than 7 micrometers have been generated by lunar secondary ejecta impacts and not by primary meteoroid impacts. It is also found that lunar crater production rates are more accurate when deduced from meteoroid space experiments and not from solar flare track ages. It is concluded that in so far as all of the above qualifications are taken into account, a self-consistent meteoroid flux versus mass distribution is obtained.
    Keywords: LUNAR AND PLANETARY EXPLORATION
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  • 3
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    Morphology and chemistry of projectile residue in small experimental impact craters (1983)
    In:  Other Sources
    Details
    Publication Date: 2011-08-18
    Description: Small-scale impact craters (5-7 mm in diameter) were produced with a light gas gun in high purity Au and Cu targets using soda lime glass (SL) and man-made basalt glass (BG) as projectiles. Maximum impact velocity was 6.4 km/s resulting in peak pressures of approximately 120-150 GPa. Copious amounts of projectile melts are preserved as thin glass liners draping the entire crater cavity; some of this liner may be lost by spallation, however. SEM investigations reveal complex surface textures including multistage flow phenomena and distinct temporal deposition sequences of small droplets. Inasmuch as some of the melts were generated at peak pressures greater than 120 GPa, these glasses represent the most severely shocked silicates recovered from laboratory experiments to date. Major element analyses reveal partial loss of alkalis; Na2O loss of 10-15 percent is observed, while K2O loss may be as high as 30-50 percent. Although the observed volatile loss in these projectile melts is significant, it still remains uncertain whether target melts produced on planetary surfaces are severely fractionated by selective volatilization processes.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Journal of Geophysical Research, Supplement (ISSN 0148-0227); 88; B353-B36
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  • 4
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    Collisional balance of the meteoritic complex (1985)
    In:  Other Sources
    Details
    Publication Date: 2011-08-19
    Description: The present study has the objective to reevaluate the size distribution of interplanetary meteoroids on the basis of the most recent data, and to analyze the probable nature of the sinks and sources of meteoritic material. The flux of interplanetary meteorites at 1 AU is discussed, taking into account general characteristics, lunar crater distribution, flux curves, spatial densities, and cross-sectional distribution and light scattering. Collisional effects are examined, giving attention to catastrophic collisions, collision rate, and destroyed mass and generated fragments. The effect of radiation pressure on small particles is considered along with the difference between the lunar and interplanetary flux models, collisional evolution at 1 AU, potential sources for large meteoroids, and observational evidence of losses of small micrometeoroids.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Icarus (ISSN 0019-1035); 62; 244-272
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  • 5
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    On dust emissions from the jovian system (1994)
    In:  Other Sources
    Details
    Publication Date: 2019-01-25
    Description: As described by Grun et al. the dust impact detector on the Ulysses spacecraft detected a totally unexpected series of dust streams in the outer solar system near the orbit of Jupiter. Five considerations lead us to believe that the dust streams emanate from the jovian system itself: (1) the dust streams only occur within about 1 AU of the jovian system, with the strongest stream being the one closest to Jupiter (about 550 R(sub J) away); (2) the direction from which they arrive is never far from the line-of-sight direction to Jupiter; (3) the time period between streams is about 28 (plus or minus 3) days; (4) the impact velocities are very high - mostly around 40 km s(exp -1); and (5) we can think of no cometary, asteroidal, or interstellar source that could give rise to the above four phenomena; such streams have never before been detected.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Workshop on the Analysis of Interplanetary Dust Particles; p 57-58
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  • 6
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    On dust emissions from the jovian system (1993)
    In:  Other Sources
    Details
    Publication Date: 2019-01-25
    Description: As described by Gruen et al., the dust impact detector on the Ulysses spacecraft detected a totally unexpected series of dust streams in the outer solar system near the orbit of Jupiter. Five considerations lead us to believe that the dust streams emanate from the jovian system itself: the dust streams only occur within about 1 AU of the jovian system, with the strongest stream being the one closest to Jupiter (about 550 R(sub J) away); the direction from which they arrive is never far from the line-of-sight direction to Jupiter; the time period between streams is about 28 (+/- 3) days; the impact velocities are very high--mostly around 40 km/s; and we can think of no cometary, asteroidal, or interstellar source that could give rise to the above four phenomena (such streams have never before been detected).
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar and Planetary Inst., Twenty-Fourth Lunar and Planetary Science Conference. Part 3: N-Z; p 1587-1588
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  • 7
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    Lunar microcraters - Implications for the micrometeoroid complex (1975)
    In:  Other Sources
    Details
    Publication Date: 2019-06-27
    Description: (For abstract see issue 03, p. 459, Accession no. A75-13187)
    Keywords: LUNAR AND PLANETARY EXPLORATION
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