Difference between revisions of "February 23, 2004"

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=Rocks and Time on the Moon=
 
=Rocks and Time on the Moon=
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<table width="640"  border="0" align="center" cellpadding="6" cellspacing="2">
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      <td width="50%"><h2 align="left">Rocks and Time on the Moon</h2></td>
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  <td width="50%"><h2 align="right">February 23, 2004</h2></td>
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<IMG SRC="images/LPOD-2004-02-23.jpeg" NAME="main_image" border="0"></div>
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      <td><div align="center" span class="main_sm">Image Credit:  [mailto:chuck@observingthesky.org CA Wood</A> based on Figure 7 of Wilhelms (1987)</div></td>
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<table class="story" border="0" bgcolor="#FFFFFF" width="90%" cellpadding="10" align="center"><tr><td>
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  <p class="story" align="center"><b>Rocks and Time on the Moon </b></p>
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  <p class="story" align="left">       
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  What we see on the Moon are rock units, many of which were formed instantaneously. For example, the crater
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        Copernicus disrupted the existing lunar surface and spread deposits as rays and secondary craters - new rock
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        units. Copernicus is one of the largest young craters and its rays define a a chronologic instant in lunar
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        history that we can use to relatively date other rock units. We can safely infer that the surface of Mare Imbrium
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        must be older than Copernicus because the mare is crossed by Copernicus' rays and secondary craters. The formation
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        of large impact basins are much larger, almost Moon wide, events that are used to define time boundaries. Ejecta
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        deposits from the two youngest large basins - Orientale and Imbrium - are nearly instantaneously created rock
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        units. During the 1960s the US Geologic Survey made observations such as these and developed a stratigraphic
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        history of the Moon. That history is summarized in the Survey's Geologic
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        [LPOD-2004-02-03.htm Map of the Moon] and in this chart whose colors approximately match those of
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        the Map. The names Copernican, Eratosthenian, Imbrium, Nectarian and pre-Nectarian are commonly used by lunar
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        scientist to describe periods of lunar history. Note how much activity was squeezed into the first 700 million
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        years, and how little has happened during the last three billion!
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</p>
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  <p class"story"><b>Related Links:</b><br>
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The Geologic History of the Moon by Don E. Wilhelms. US Geol. Surv. PP 1348 (1987).</p>
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  <p class"story"> <b>Tomorrow's LPOD:</b> An Amateur's Moon</p>
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  <p><img src="../../../MainPage/spacer.gif" width="640" height="1"></p>
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  <p align="center" class="main_titles"><b>Author & Editor:</b><br>
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      <a class="one" href="mailto:chuck@observingthesky.org">Charles A. Wood]</p>
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      <p align="center" class="main_titles"><b>Technical Consultant:</b><br>
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      [mailto:anthony@perseus.gr Anthony Ayiomamitis]</p>
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      <p align="center" class="main_titles"><b>[mailto:webmaster@entropysponge.com Contact Webmaster]</b></p>
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      <p align="center" class="main_titles"><b>A service of:</b><br>
 +
      <a class="one" href="http://www.observingthesky.org/">ObservingTheSky.Org</a></p>
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      <p align="center" class="main_titles"><b>Visit these other PODs:</b> <br>
 +
      <a class="one" href="http://antwrp.gsfc.nasa.gov/apod/astropix.html">Astronomy</a> | <a class="one" href="http://www.msss.com/">Mars</a> | <a class="one" href="http://epod.usra.edu/">Earth</a></p></td>
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<p>&nbsp;</p>
  
  

Revision as of 15:35, 4 January 2015

Rocks and Time on the Moon

Rocks and Time on the Moon

February 23, 2004
<IMG SRC="images/LPOD-2004-02-23.jpeg" NAME="main_image" border="0">
Image Credit: [mailto:chuck@observingthesky.org CA Wood</A> based on Figure 7 of Wilhelms (1987)

Rocks and Time on the Moon

What we see on the Moon are rock units, many of which were formed instantaneously. For example, the crater Copernicus disrupted the existing lunar surface and spread deposits as rays and secondary craters - new rock units. Copernicus is one of the largest young craters and its rays define a a chronologic instant in lunar history that we can use to relatively date other rock units. We can safely infer that the surface of Mare Imbrium must be older than Copernicus because the mare is crossed by Copernicus' rays and secondary craters. The formation of large impact basins are much larger, almost Moon wide, events that are used to define time boundaries. Ejecta deposits from the two youngest large basins - Orientale and Imbrium - are nearly instantaneously created rock units. During the 1960s the US Geologic Survey made observations such as these and developed a stratigraphic history of the Moon. That history is summarized in the Survey's Geologic [LPOD-2004-02-03.htm Map of the Moon] and in this chart whose colors approximately match those of the Map. The names Copernican, Eratosthenian, Imbrium, Nectarian and pre-Nectarian are commonly used by lunar scientist to describe periods of lunar history. Note how much activity was squeezed into the first 700 million years, and how little has happened during the last three billion!

Related Links:
The Geologic History of the Moon by Don E. Wilhelms. US Geol. Surv. PP 1348 (1987).

Tomorrow's LPOD: An Amateur's Moon

<img src="../../../MainPage/spacer.gif" width="640" height="1">

Author & Editor:
<a class="one" href="mailto:chuck@observingthesky.org">Charles A. Wood]

Technical Consultant:
Anthony Ayiomamitis

Contact Webmaster

A service of:
<a class="one" href="http://www.observingthesky.org/">ObservingTheSky.Org</a>

Visit these other PODs:
<a class="one" href="http://antwrp.gsfc.nasa.gov/apod/astropix.html">Astronomy</a> | <a class="one" href="http://www.msss.com/">Mars</a> | <a class="one" href="http://epod.usra.edu/">Earth</a>


 


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