Difference between revisions of "April 13, 2011"
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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" rel="nofollow Tomokatsu Morota and colleagues] (2011)</em><br /> |
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The ages of lunar lava flows are important because these surface rocks provide evidence about the thermal <br /> | The ages of lunar lava flows are important because these surface rocks provide evidence about the thermal <br /> | ||
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was along one of Imbrium inner basin rings? <br /> | was along one of Imbrium inner basin rings? <br /> | ||
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| − | <em>[mailto:tychocrater@yahoo.com Chuck Wood]</em><br /> | + | <em>[mailto:tychocrater@yahoo.com" rel="nofollow Chuck Wood]</em><br /> |
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<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 <br /> | + | [http://adsabs.harvard.edu/abs/2011E%26PSL.302..255M" rel="nofollow Timing and characteristics of the latest mare eruption on the Moon]. T. Morota and colleagues (2011). <em>Earth <br /> |
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 /> | ||
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Revision as of 22:15, 4 January 2015
Refined Ages
Kaguya Terrain Camera image (a) and derived mare ages (d) from " rel="nofollow 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?
" rel="nofollow Chuck Wood
Related Links
" rel="nofollow 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.
