<?xml version='1.0' encoding='utf-8'?>
<oai_dc:dc xmlns:dc="http://purl.org/dc/elements/1.1/" xmlns:oai_dc="http://www.openarchives.org/OAI/2.0/oai_dc/" xmlns:xsi="http://www.w3.org/2001/XMLSchema-instance" xsi:schemaLocation="http://www.openarchives.org/OAI/2.0/oai_dc/ http://www.openarchives.org/OAI/2.0/oai_dc.xsd">
  <dc:contributor>M. H. Carr</dc:contributor>
  <dc:contributor>H. Masursky</dc:contributor>
  <dc:contributor>R.W. Shorthill</dc:contributor>
  <dc:contributor>T.W. Thompson</dc:contributor>
  <dc:creator>S.H. Zisk</dc:creator>
  <dc:date>1971</dc:date>
  <dc:description>&lt;p&gt;&lt;span id="_mce_caret" data-mce-bogus="1" data-mce-type="format-caret"&gt;&lt;span&gt;Recently completed high-resolution radar maps of the moon contain information on the decimeter-scale structure of the surface. When this information is combined with eclipse thermal-enhancement data and with high-resolution Lunar Orbiter photography, the surface morphology is revealed in some detail. A geological history for certain features and subareas can be developed, which provides one possible framework for the interpretation of the findings from the Apollo 15 landing. Frequency of decimeter- and meter-size blocks in and around lunar craters, given by the remote-sensed data, supports a multilayer structure in the Palus Putredinis mare region, as well as a great age for the bordering Apennine Mountains scarp.&lt;/span&gt;&lt;/span&gt;&lt;/p&gt;</dc:description>
  <dc:format>application/pdf</dc:format>
  <dc:identifier>10.1126/science.173.3999.808</dc:identifier>
  <dc:language>en</dc:language>
  <dc:publisher>American Association for the Advancement of Science</dc:publisher>
  <dc:title>Lunar Apennine-Hadley region: Geological implications of earth-based radar and infrared measurements</dc:title>
  <dc:type>article</dc:type>
</oai_dc:dc>