Difference between revisions of "July 19, 2004"
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=The Best Lunar Lava Flow= | =The Best Lunar Lava Flow= | ||
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| + | {{HoverImage|LPOD-2004-07-19.jpeg|LPOD-2004-07-19b.jpeg}} | ||
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| + | <td><div align="center" span class="main_sm"><p>Image Credit: <span class="one">[http://www.lpi.usra.edu/expmoon/Apollo15/A15_Photography_metric.html Apollo 15 - 1555]</span> (L) and [mailto:kcpaulhk@yahoo.com.hk KC Pau] (R) </p></div></td> | ||
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| + | <p class="story" align="center"><b>The Best Lunar Lava Flow</b></p> | ||
| + | <p class="story" align="left"> | ||
| + | Samples brought from the Moon confirmed that the maria are made of basaltic lava. But their ages are so ancient that little morphological evidence remains of the millions of individual lava flows that built the thick mare piles. Only one set of relatively young lava flows - perhaps 2.5 billion years - is still detectable, barely. Discovered on photographs made in 1966 with the Lunar & Planetary Lab's 61" Catalina Telescope, the flows were beautifully documented during the Apollo 15 mission. They remained poorly imaged from Earth until June 27 of this year when KC Pau acquired this marvelous image of western Mare Imbrium. With a co-longitude of 29 degrees, KC's image is nearly the same sun angle as the Apollo Metric Camera image. This is a thin flow, estimated to be about 35 m thick, and was erupted before the formation of the Zirkel mare ridge. How do we know that? Well, notice that the source of the lava flow is to the west of La Hire, and that the lava flowed eastward and downhill toward the Imbrium Basin center. The flow could not have climbed over the mare ridge, which must have formed later. The flows were the last part of the filling of Mare Imbrium, and the ridges are part of the subsidence of the mare caused by the weight of the entire mare fill. </p> | ||
| + | <blockquote> | ||
| + | <p align="right" class="story">— [mailto:tychocrater@yahoo.com Chuck Wood]</p></blockquote> | ||
| + | <p class="story"><b>Technical Details:</b><br> | ||
| + | June 27, 2004. 10" f/6 Newtonian reflector with 2.5x Barlow and Philips Toucam Pro; the seeing was under average. This is L98 of the Lunar 100.</p> | ||
| + | <p class="story"><b>Related Links:</b> <br> | ||
| + | [http://observingthesky.org/index.php?p=174 Pau Observatory] <br> | ||
| + | [http://www.lpi.usra.edu/research/cla/info/b17/ Catalina Image] (see bottom) <br> | ||
| + | A. Rukl, Atlas of the Moon, charts 10 & 20</p> | ||
| + | <p><b>Yesterday's LPOD:</b> [[July 18, 2004|A New Hit DVD]] </p> | ||
| + | <p><b>Tomorrow's LPOD:</b> [[July 20, 2004|The Beginning of the End of the Future]] </p> | ||
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| + | <td><p align="center" class="main_titles"><b>Author & Editor:</b><br> | ||
| + | [mailto:tychocrater@yahoo.com Charles A. Wood]</p> | ||
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Latest revision as of 19:21, 7 February 2015
The Best Lunar Lava Flow
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Image Credit: Apollo 15 - 1555 (L) and KC Pau (R) |
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The Best Lunar Lava Flow Samples brought from the Moon confirmed that the maria are made of basaltic lava. But their ages are so ancient that little morphological evidence remains of the millions of individual lava flows that built the thick mare piles. Only one set of relatively young lava flows - perhaps 2.5 billion years - is still detectable, barely. Discovered on photographs made in 1966 with the Lunar & Planetary Lab's 61" Catalina Telescope, the flows were beautifully documented during the Apollo 15 mission. They remained poorly imaged from Earth until June 27 of this year when KC Pau acquired this marvelous image of western Mare Imbrium. With a co-longitude of 29 degrees, KC's image is nearly the same sun angle as the Apollo Metric Camera image. This is a thin flow, estimated to be about 35 m thick, and was erupted before the formation of the Zirkel mare ridge. How do we know that? Well, notice that the source of the lava flow is to the west of La Hire, and that the lava flowed eastward and downhill toward the Imbrium Basin center. The flow could not have climbed over the mare ridge, which must have formed later. The flows were the last part of the filling of Mare Imbrium, and the ridges are part of the subsidence of the mare caused by the weight of the entire mare fill. Technical Details: Related Links: Yesterday's LPOD: A New Hit DVD Tomorrow's LPOD: The Beginning of the End of the Future |
Author & Editor: |
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