Difference between revisions of "July 16, 2004"
| (5 intermediate revisions by the same user not shown) | |||
| Line 1: | Line 1: | ||
__NOTOC__ | __NOTOC__ | ||
=Raisin Pits= | =Raisin Pits= | ||
| + | <!-- Start of content --> | ||
<table width="85%" border="0" align="center" cellpadding="6" cellspacing="2"> | <table width="85%" border="0" align="center" cellpadding="6" cellspacing="2"> | ||
<tr> | <tr> | ||
| Line 8: | Line 9: | ||
<tr> | <tr> | ||
<td colspan="2"><div align="center"> | <td colspan="2"><div align="center"> | ||
| − | {{HoverImage|LPOD-2004-07-16.jpeg|}} | + | {{HoverImage|LPOD-2004-07-16.jpeg|LPOD-2004-07-16b.jpeg}} |
</div></td> | </div></td> | ||
</tr> | </tr> | ||
| Line 14: | Line 15: | ||
<table width="100%" border="0" cellpadding="8"> | <table width="100%" border="0" cellpadding="8"> | ||
<tr> | <tr> | ||
| − | <td><div align="center"><p>Image Credit: Apollo 17 Metric Camera Image M2444</div></td> | + | <td><div align="center" span class="main_sm"><p>Image Credit: Apollo 17 Metric Camera Image M2444</p></div></td> |
</tr> | </tr> | ||
</table> | </table> | ||
| Line 22: | Line 23: | ||
Rays and pits go hand in hand. The formation of crater rays was one of the totally misunderstood features on the Moon until Gene Shoemaker studied Meteor Crater in Arizona in the 1950s. He discovered that the impact event threw out streams of boulders and rocky blocks that gouged the surrounding surface and deposited material from beneath the crater onto the surface. He proposed exactly the same origin for lunar crater rays, an idea supported by his observation of small pits along Copernicus' rays crossing southern Mare Imbrium. This dramatic Apollo 17 view wonderfully displays both the bright rays and the secondary crater pits from Copernicus. The crater itself is obliquely viewed near the horizon about 400 km distant. Most of the elongated and overlapping small secondary craters are embedded in the light hued rays. But why are rays bright? In 1985, Carle Pieters (Brown University) and her colleagues showed that the bright ray material was highland rocks excavated by the impact of Copernicus. Highland materials are bright because they are made predominately of the light colored aluminum-rich mineral anorthosite. But, you should say, Copernicus impacted into the dark mare lavas of Mare Insularum. Yes, but the lavas are thin and they overly highland anorthosites! We are beginning to understand how the Moon works!</p> | Rays and pits go hand in hand. The formation of crater rays was one of the totally misunderstood features on the Moon until Gene Shoemaker studied Meteor Crater in Arizona in the 1950s. He discovered that the impact event threw out streams of boulders and rocky blocks that gouged the surrounding surface and deposited material from beneath the crater onto the surface. He proposed exactly the same origin for lunar crater rays, an idea supported by his observation of small pits along Copernicus' rays crossing southern Mare Imbrium. This dramatic Apollo 17 view wonderfully displays both the bright rays and the secondary crater pits from Copernicus. The crater itself is obliquely viewed near the horizon about 400 km distant. Most of the elongated and overlapping small secondary craters are embedded in the light hued rays. But why are rays bright? In 1985, Carle Pieters (Brown University) and her colleagues showed that the bright ray material was highland rocks excavated by the impact of Copernicus. Highland materials are bright because they are made predominately of the light colored aluminum-rich mineral anorthosite. But, you should say, Copernicus impacted into the dark mare lavas of Mare Insularum. Yes, but the lavas are thin and they overly highland anorthosites! We are beginning to understand how the Moon works!</p> | ||
<blockquote> | <blockquote> | ||
| − | <p align="right" class="story">— [mailto:tychocrater@yahoo.com Chuck Wood]</p></ | + | <p align="right" class="story">— [mailto:tychocrater@yahoo.com Chuck Wood]</p></blockquote> |
| + | <p class="story" align="left"><b>Related Links: </b><br> | ||
| + | Hawke, B.R and others (2004) The origin of lunar crater rays. Icarus 170, 1-16.<br> | ||
| + | Pieters, C.M. and others (1985) The nature of crater rays: the Copernicus example. Journal of Geophysical Research 90, 12393-12413.</p> | ||
| + | <p><b>Yesterday's LPOD:</b> [[July 15, 2004|Licking the Moon]] </p> | ||
| + | <p><b>Tomorrow's LPOD:</b> [[July 17, 2004|Our Moon]] </p> | ||
| + | </tr> | ||
| + | </table> | ||
| + | <!-- start bottom --> | ||
| + | <table width="100%" border="0" cellspacing="2" cellpadding="4"> | ||
| + | <tr> | ||
| + | <td><hr></td> | ||
</tr> | </tr> | ||
<tr> | <tr> | ||
<td><p align="center" class="main_titles"><b>Author & Editor:</b><br> | <td><p align="center" class="main_titles"><b>Author & Editor:</b><br> | ||
[mailto:tychocrater@yahoo.com Charles A. Wood]</p> | [mailto:tychocrater@yahoo.com Charles A. Wood]</p> | ||
| − | < | + | <!-- Cleanup of credits --> |
| − | + | <!-- Cleanup of credits --> | |
| − | < | + | <!-- Cleanup of credits --> |
| − | + | <!-- Cleanup of credits --> | |
| − | < | + | <!-- Cleanup of credits --> |
| − | + | <!-- Cleanup of credits --> | |
| + | <!-- Cleanup of credits --> | ||
</tr> | </tr> | ||
</table> | </table> | ||
| Line 38: | Line 51: | ||
<div align="center"></div> | <div align="center"></div> | ||
<p> </p> | <p> </p> | ||
| − | ---- | + | <!-- End of content --> |
| − | + | {{wiki/ArticleFooter}} | |
| − | |||
Latest revision as of 18:21, 7 February 2015
Raisin Pits
|
Image Credit: Apollo 17 Metric Camera Image M2444 |
|
Raisin Pits Rays and pits go hand in hand. The formation of crater rays was one of the totally misunderstood features on the Moon until Gene Shoemaker studied Meteor Crater in Arizona in the 1950s. He discovered that the impact event threw out streams of boulders and rocky blocks that gouged the surrounding surface and deposited material from beneath the crater onto the surface. He proposed exactly the same origin for lunar crater rays, an idea supported by his observation of small pits along Copernicus' rays crossing southern Mare Imbrium. This dramatic Apollo 17 view wonderfully displays both the bright rays and the secondary crater pits from Copernicus. The crater itself is obliquely viewed near the horizon about 400 km distant. Most of the elongated and overlapping small secondary craters are embedded in the light hued rays. But why are rays bright? In 1985, Carle Pieters (Brown University) and her colleagues showed that the bright ray material was highland rocks excavated by the impact of Copernicus. Highland materials are bright because they are made predominately of the light colored aluminum-rich mineral anorthosite. But, you should say, Copernicus impacted into the dark mare lavas of Mare Insularum. Yes, but the lavas are thin and they overly highland anorthosites! We are beginning to understand how the Moon works! Related Links: Yesterday's LPOD: Licking the Moon Tomorrow's LPOD: Our Moon |
Author & Editor: |
COMMENTS?
Register, Log in, and join in the comments.
