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  • 2010-2014  (1)
  • 1970-1974  (3)
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  • 1
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    The naive airway hyperresponsiveness of the A/J mouse is Kit-mediated [Genetics] (2011)
    National Academy of Sciences
    Details
    Publication Date: 2011-08-03
    Description: There is a wide variation among humans and mice in airway hyperresponsiveness (AHR) in the absence of allergen sensitization, i.e., naïve AHR. Because mast cell (MC) activation is thought to mediate AHR in atopic asthmatic subjects, we asked whether MCs mediate naïve AHR in A/J mice. We generated an A/J congenic strain lacking c-Kit by introgression of the Wv mutation, which resulted in the elimination of MCs and the abrogation of naïve AHR. Imatinib, which disrupts Kit signaling, also abrogated AHR in A/J mice. Remarkably, introduction of the Vga9 Mitf mutation into the A/J background resulted in the ablation of MCs but did not ameliorate AHR. These results indicate that c-Kit is required for development of AHR in an MC-independent fashion.
    Print ISSN: 0027-8424
    Electronic ISSN: 1091-6490
    Topics: Biology , Medicine , Natural Sciences in General
    Published by National Academy of Sciences
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    PAPER CURRENT
  • 2
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    Photogeology. Part A: Relative ages of some near-side and far-side terra plains based on Apollo 16 metric photography (1972)
    In:  CASI
    Details
    Publication Date: 2005-11-30
    Description: Relative age measurements were made for 14 light plains areas, using 30X enlargements of Apollo 16 metric camera photography. Results indicate that: (1) Crater morphology and frequency studies consistently indicate that the Fra Mauro Formation has received 2.5 to 3 times as much impact flux as the Cayley Formation. (2) Crater counts and relative age dating indicate that the Cayley Formation is only slightly older than the oldest mare units. (3) Assuming the rubidium-strontium ages of Apollo 14 basalt breccias give minimum age for Fra Mauro Formation, the Cayley Formation must have been generated throughout a period of less than 100 million years, approximately 3.8 to 3.9 billion years ago. (4) The Cayley Formation ages obtained on the near side and far side are the same, indicating a synchrony throughout the moon in these units. (5) The linear relationship as predicted by the small impact erosion model between net accumulated flux and the maximum diameter of a crater that could be eroded below recognition is confirmed.
    Keywords: SPACE SCIENCES
    Type: NASA. Lyndon B. Johnson Space Center Apollo 16 Prelim. Sci. Rept.; 4 p
    Format: text
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    NASA TECHNICAL REPORTS
  • 3
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    Relative ages of some near-side Mare units based on Apollo 17 metric photographs (1973)
    In:  CASI
    Details
    Publication Date: 2006-01-11
    Description: Relative flux ages were determined for 110 areas on parts of Serenitatis, Vaporum, and Imbrium, using Apollo 17 metric photographs. The crater-morphology technique for determining relative ages is described. It is concluded that these maria formed over an interval of 1.5 billion years, extending from 3.7 to 2.2 billion years ago.
    Keywords: SPACE SCIENCES
    Type: NASA. Johnson Space Center Apollo 17 Prelim. Sci. Rept.; 3 p
    Format: text
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    NASA TECHNICAL REPORTS
  • 4
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    Ages of the lunar nearside light plains and maria (1974)
    In:  Other Sources
    Details
    Publication Date: 2019-07-13
    Description: An extension of a previous work on relative age mapping for the lunar nearside is presented. The ages were determined from Apollo (Hasselblad, metric, and panoramic) and Lunar Orbiter photographs; three major subdivisions were observed: maria and two older light plains units. The plains units center around 3.8 b.y. and 4.0 b.y., respectively. Ages of maria decrease westward. The oldest maria is 3.7 b.y.; it comprises Mare Tranquillitatis and two small areas in southeastern Mare Imbrium. Oceanus Procellarum, southwestern Mare Imbrium, northern Mare Humorum, and northwestern Mare Serenitatis contain the youngest maria; the youngest of these formed about 1.7 b.y. ago. Emplacement of all three subdivisions occurred over a 2.3 b.y. interval. The three-stage model of mare emplacement proposed by Soderblom (1970a) is confirmed. Thus the sequence is (1) high-Ti basalts in the eastern hemisphere, (2) low-Ti basalts filling circular ring-maria, and (3) high-Ti basalts in the western hemisphere.
    Keywords: LUNAR AND PLANETARY EXPLORATION
    Type: Lunar Science Conference; Mar 18, 1974 - Mar 22, 1974; Houston, TX
    Format: text
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    NASA TECHNICAL REPORTS
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