Difference between revisions of "June 29, 2011"
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=New Ages for Old Rocks= | =New Ages for Old Rocks= | ||
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| − | <em>maps from [http://www.sciencedirect.com/science/article/pii/S0012821X10007909 Tomokatsu Morota and others, 2011]</em><br /> | + | <em>maps from [http://www.sciencedirect.com/science/article/pii/S0012821X10007909" rel="nofollow Tomokatsu Morota and others, 2011]</em><br /> |
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Counting craters is a mundane (and boring) task that nonetheless results in information that is critical for<br /> | Counting craters is a mundane (and boring) task that nonetheless results in information that is critical for<br /> | ||
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Apollo samples that have been radiometrically dated in laboratories on Earth provide calibration, but we<br /> | Apollo samples that have been radiometrically dated in laboratories on Earth provide calibration, but we<br /> | ||
didn't land on lavas of enough different ages to be confident of the calibration for ages younger than about<br /> | didn't land on lavas of enough different ages to be confident of the calibration for ages younger than about<br /> | ||
| − | 2 billion years. This chart is the latest [ | + | 2 billion years. This chart is the latest [/May+4%2C+2010 attempt] to determine model ages for the maria on the western hemi-<br /> |
sphere of the Moon. It is based on crater counts on the Terrain Camera images of the Kaguya spacecraft,<br /> | sphere of the Moon. It is based on crater counts on the Terrain Camera images of the Kaguya spacecraft,<br /> | ||
which had better resolution and coverage that Lunar Orbiter IV images used for earlier work. According to<br /> | which had better resolution and coverage that Lunar Orbiter IV images used for earlier work. According to<br /> | ||
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nearby lavas in eastern Imbrium - I always assumed they were the same age<br /> | nearby lavas in eastern Imbrium - I always assumed they were the same age<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 /> |
<br /> | <br /> | ||
<strong>Related Links</strong><br /> | <strong>Related Links</strong><br /> | ||
| − | Tomokatsu Morota and others (2011) [http://www.sciencedirect.com/science/article/pii/S0012821X10007909 Timing and characteristics of the latest mare eruption on the Moon.]<br /> | + | Tomokatsu Morota and others (2011) [http://www.sciencedirect.com/science/article/pii/S0012821X10007909" rel="nofollow Timing and characteristics of the latest mare eruption on the Moon.]<br /> |
<em>Earth and Planetary Science Letters</em>; Volume 302, Issues 3-4, 1 February 2011, Pages 255-266.<br /> | <em>Earth and Planetary Science Letters</em>; Volume 302, Issues 3-4, 1 February 2011, Pages 255-266.<br /> | ||
<br /> | <br /> | ||
<hr /> | <hr /> | ||
Revision as of 22:18, 4 January 2015
New Ages for Old Rocks
maps from " rel="nofollow Tomokatsu Morota and others, 2011
Counting craters is a mundane (and boring) task that nonetheless results in information that is critical for
understanding lunar history. The older a lunar surface is the longer it has been recording impact cratering
events. So lunar scientists count the number of impact craters on an area to estimate its age of formation.
The ages determined are called model ages, rather than real ages because the conversion to ages
depends on mathematical models of how rapidly the rate of cratering declined through lunar history, what
the distribution of impact velocities was likely to have been, and what corrections are necessary becaue
the Earth may have gravitationally attracted projectiles that otherwise would miss the Moon. Fortunately,
Apollo samples that have been radiometrically dated in laboratories on Earth provide calibration, but we
didn't land on lavas of enough different ages to be confident of the calibration for ages younger than about
2 billion years. This chart is the latest [/May+4%2C+2010 attempt] to determine model ages for the maria on the western hemi-
sphere of the Moon. It is based on crater counts on the Terrain Camera images of the Kaguya spacecraft,
which had better resolution and coverage that Lunar Orbiter IV images used for earlier work. According to
these results there are no lavas younger than about 1.2 billion years, in contrast to some previous estimates
of ages of 0.8 to 1.0 b.y. Otherwise the results are similar to earlier ones, with the youngest lavas in Eastern
Procellarum, and some yellow ones that flowed into the center of Mare Imbrium. There are many things to
think about - for example, the top layers of lavas on Imbrium span about 800 million years - it wasn't filled
quickly! And the mare material on the floor of Plato is a few hundred million years younger than most of the
nearby lavas in eastern Imbrium - I always assumed they were the same age
" rel="nofollow Chuck Wood
Related Links
Tomokatsu Morota and others (2011) " rel="nofollow Timing and characteristics of the latest mare eruption on the Moon.
Earth and Planetary Science Letters; Volume 302, Issues 3-4, 1 February 2011, Pages 255-266.
