Difference between revisions of "April 13, 2011"
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=Refined Ages= | =Refined Ages= | ||
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<em>Kaguya Terrain Camera image (a) and derived mare ages (d) from [http://adsabs.harvard.edu/abs/2011E%26PSL.302..255M Tomokatsu Morota and colleagues] (2011)</em><br /> | <em>Kaguya Terrain Camera image (a) and derived mare ages (d) from [http://adsabs.harvard.edu/abs/2011E%26PSL.302..255M Tomokatsu Morota and colleagues] (2011)</em><br /> | ||
<br /> | <br /> | ||
− | The ages of lunar lava flows are important because these surface rocks provide evidence about the thermal | + | The ages of lunar lava flows are important because these surface rocks provide evidence about the thermal |
− | evolution of the lunar interior. Based on radiometric dating of returned samples, lunar volcanism occurred | + | evolution of the lunar interior. Based on radiometric dating of returned samples, lunar volcanism occurred |
− | between about 4.3 and 2.5 billion years. But Apollo and Luna samples come from only 10 locations so | + | between about 4.3 and 2.5 billion years. But Apollo and Luna samples come from only 10 locations so |
− | there are many places that remain un sampled and undated. As we have seen [http://lpod. | + | there are many places that remain un sampled and undated. As we have seen [http://www2.lpod.org/wiki/May_4,_2010 before] counting the number |
− | of impact craters has become an effective proxy for radiometric dating so that we can count craters and infer | + | of impact craters has become an effective proxy for radiometric dating so that we can count craters and infer |
− | model ages for all the maria. Japanese scientists have now refined crater counting using 10 m resolution | + | model ages for all the maria. Japanese scientists have now refined crater counting using 10 m resolution |
− | images from the Terrain Camera on the Kaguya spacecraft. There crater counts were within the north western | + | images from the Terrain Camera on the Kaguya spacecraft. There crater counts were within the north western |
− | part of the Moon where prior work indicated the youngest lunar maria lavas were located. The new results | + | part of the Moon where prior work indicated the youngest lunar maria lavas were located. The new results |
− | confirm that lavas erupted in a ribbon (orange) west of Kepler and also east of Bessarion. These lavas are | + | confirm that lavas erupted in a ribbon (orange) west of Kepler and also east of Bessarion. These lavas are |
− | 1.5 to 1.6 billion year old - the youngest on the Moon - so it would be expected that their vents would be easily | + | 1.5 to 1.6 billion year old - the youngest on the Moon - so it would be expected that their vents would be easily |
− | detected, but I don't see them in a quick search. Also, notice the patch of yellow in the middle of Mare Imbrium. | + | detected, but I don't see them in a quick search. Also, notice the patch of yellow in the middle of Mare Imbrium. |
− | This 1.8 b.y. old lava flow is surrounded by lavas about 3 b.y. old; I wonder if the vent for these yellow flows | + | This 1.8 b.y. old lava flow is surrounded by lavas about 3 b.y. old; I wonder if the vent for these yellow flows |
− | was along one of Imbrium inner basin rings? | + | was along one of Imbrium inner basin rings? |
<br /> | <br /> | ||
<em>[mailto:tychocrater@yahoo.com Chuck Wood]</em><br /> | <em>[mailto:tychocrater@yahoo.com Chuck Wood]</em><br /> | ||
<br /> | <br /> | ||
<strong>Related Links</strong><br /> | <strong>Related Links</strong><br /> | ||
− | [http://adsabs.harvard.edu/abs/2011E%26PSL.302..255M Timing and characteristics of the latest mare eruption on the Moon]. T. Morota and colleagues (2011). <em>Earth | + | [http://adsabs.harvard.edu/abs/2011E%26PSL.302..255M Timing and characteristics of the latest mare eruption on the Moon]. T. Morota and colleagues (2011). <em>Earth |
and Planetary Science Letters</em>, Volume 302, Issue 3-4, p. 255-266.<br /> | and Planetary Science Letters</em>, Volume 302, Issue 3-4, p. 255-266.<br /> | ||
<br /> | <br /> | ||
<hr /> | <hr /> | ||
+ | <p><b>Yesterday's LPOD:</b> [[April 12, 2011|50 Years Ago]] </p> | ||
+ | <p><b>Tomorrow's LPOD:</b> [[April 14, 2011|Welcome Back, Mario]] </p> | ||
+ | <!-- End of content --> | ||
+ | {{wiki/ArticleFooter}} |
Latest revision as of 08:22, 28 October 2018
Refined Ages
Kaguya Terrain Camera image (a) and derived mare ages (d) from Tomokatsu Morota and colleagues (2011)
The ages of lunar lava flows are important because these surface rocks provide evidence about the thermal
evolution of the lunar interior. Based on radiometric dating of returned samples, lunar volcanism occurred
between about 4.3 and 2.5 billion years. But Apollo and Luna samples come from only 10 locations so
there are many places that remain un sampled and undated. As we have seen before counting the number
of impact craters has become an effective proxy for radiometric dating so that we can count craters and infer
model ages for all the maria. Japanese scientists have now refined crater counting using 10 m resolution
images from the Terrain Camera on the Kaguya spacecraft. There crater counts were within the north western
part of the Moon where prior work indicated the youngest lunar maria lavas were located. The new results
confirm that lavas erupted in a ribbon (orange) west of Kepler and also east of Bessarion. These lavas are
1.5 to 1.6 billion year old - the youngest on the Moon - so it would be expected that their vents would be easily
detected, but I don't see them in a quick search. Also, notice the patch of yellow in the middle of Mare Imbrium.
This 1.8 b.y. old lava flow is surrounded by lavas about 3 b.y. old; I wonder if the vent for these yellow flows
was along one of Imbrium inner basin rings?
Chuck Wood
Related Links
Timing and characteristics of the latest mare eruption on the Moon. T. Morota and colleagues (2011). Earth
and Planetary Science Letters, Volume 302, Issue 3-4, p. 255-266.
Yesterday's LPOD: 50 Years Ago
Tomorrow's LPOD: Welcome Back, Mario
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