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  • 1
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    Elemental abundances in interplanetary dust (1974)
    In:  Other Sources
    Details
    Publication Date: 2011-08-16
    Description: The paper reports on measurements taken of elemental abundances in two interplanetary dust grains. Meteoroidal residue found inside micrometeoritic craters was discovered by optically scanning the 800 sq cm aluminum surface of the S-228 transuranic cosmic-ray experiment exposed to space for 67d during the Skylab-IV mission. Crater analyses for two randomly sampled meteoroids showed a composition consistent with troilite in the 9 micron-minute particle. Chondritic abundances were found in the 30 micron-minute particle. Particles of similar size and chemistry were common in carbonaceous chondrite meteorites. The inferred grain sizes within the 30 micron-minute particle provided evidence for the similarity to carbonaceous chondrites rather than to other meteorite types.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Nature; 252; Dec
    Format: text
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    NASA TECHNICAL REPORTS
  • 2
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    Physical properties of interplanetary grains (1976)
    In:  CASI
    Details
    Publication Date: 2016-06-07
    Description: Morphological analyses of micrometeorite craters found on lunar rocks and laboratory simulation experiments are used to formulate a meteoritic interplanetary dust particle for optical scattering calculations that is roughly spherical and has a density of 2g cm/3. The model particle has chondritic elemental abundances and also contains a high content of finely dispersed carbon.
    Keywords: ASTROPHYSICS
    Type: NASA. Goddard Space Flight Center The Study of Comets, Part 2; p 962-982
    Format: application/pdf
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    NASA TECHNICAL REPORTS
  • 3
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    An upper limit for the flux of interstellar dust grains in the solar system (1977)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: Data from the LEAM (Lunar Ejecta and Meteorite experiment, a micrometeorite detector at the Apollo 17 landing site) have been examined for evidence of interstellar (IS) dust grains traversing the solar system. The analysis technique considers IS grains approaching the solar system from the local solar apex. A model calculates the grains' hyperbolic orbits into the solar system and predicts the impact directions on the moon. The observations are then compared with the predicted impact directions to measure the IS dust flux. No evidence has been found (at the 97.5% confidence level) for a flux greater than about 6 hundred-thousandths per sq m/sec for particles of at least 2 by 10 to the -14th power g.
    Keywords: ASTROPHYSICS
    Type: Symposium on Minor Constituents and Excited Species; Jun 08, 1976 - Jun 19, 1976; Philadelphia, PA; US|Symposium on Minor Constituents and Excited Species; Jun 09, 1976 - Jun 10, 1976
    Format: text
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    NASA TECHNICAL REPORTS
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