Difference between revisions of "February 18, 2005"
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=Memory of a Crater= | =Memory of a Crater= | ||
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<table width="85%" border="0" align="center" cellpadding="6" cellspacing="2"> | <table width="85%" border="0" align="center" cellpadding="6" cellspacing="2"> | ||
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| − | + | <td width="50%"><h2><nobr>Memory of a Crater</nobr></h2></td> | |
| − | + | </tr> | |
</table> | </table> | ||
<table width="85%" border="0" align="center" cellpadding="6" cellspacing="2"> | <table width="85%" border="0" align="center" cellpadding="6" cellspacing="2"> | ||
| − | + | <tr><td colspan="2" valign="top"><div align="center"> | |
| − | + | <img src="archive/2005/02/images/LPOD-2005-02-18.jpeg" border="0"> | |
| − | + | </div></td> | |
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</table> | </table> | ||
<table width="80%" border="0" align="center" cellpadding="8"> | <table width="80%" border="0" align="center" cellpadding="8"> | ||
| − | + | <tr><td><div align="center" class="main_sm">Image Credit: [mailto:starman2@charter.net Wes Higgins]</p> | |
| − | + | </div></td> | |
| − | + | </tr> | |
| − | + | </table> | |
<br> | <br> | ||
<table class="story" border="0" bgcolor="#FFFFFF" width="90%" cellpadding="10" align="center"><tr><td> | <table class="story" border="0" bgcolor="#FFFFFF" width="90%" cellpadding="10" align="center"><tr><td> | ||
| − | + | <p align="center"><b>Memory of a Crater</b></p> | |
| − | + | <p align="left">Craters form on an existing surface, which will continue to change in the future. For example, the 30 km wide Lambert is excavated into Mare Imbrium lavas, and the crater’s ridges of continuous ejecta visibly lie on the mare surface. A few subsequent random impacts have formed craters on these deposits, and at least two small younger craters are seen inside Lambert. The daubs of grayish rays and perhaps a cluster of secondary craters to the right of Lambert and another at the center left edge of the image demonstrate that ejecta from Copernicus has also slightly modified this area. But all landscape modifications are not as modest. Consider the ghostly ring south of Lambert. This feature (Lambert R - R for ruin) could be some exotic volcanic structure, perhaps similar to a terrestrial ring dike, but more likely it is the remnant of a hapless impact crater that formed on a lower, intermediate level of Imbrium’s lavas, before the basin was filled with its final thickness of lava. The rising level of Imbrium lavas must have climbed the flanks of the crater and, finally reaching a low spot, cascaded down into the 55 km wide pit. It appears that the mare lavas completely inundated the crater, leaving only a few low arcuate ridges, joined by wrinkle ridges. There is one other unusual feature to note – on the left side of Lambert there is a flat, narrow ridge about 40 km long that feathers into the surrounding lava. The origin of this flow-like ridge is a mystery.</p> | |
| − | + | <blockquote><p align="right">— [mailto:tychocrater@yahoo.com Chuck Wood]</blockquote> | |
<p align="left"><p><b>Technical Details:</b><br> | <p align="left"><p><b>Technical Details:</b><br> | ||
Nov 5, 2004.Starmaster 18" Newt. Reflector , FL=8200mm, no filters, DMK-21F04 Firewire camera, 30FPS, stack of 804 frames from 1250.Related Links: </p> | Nov 5, 2004.Starmaster 18" Newt. Reflector , FL=8200mm, no filters, DMK-21F04 Firewire camera, 30FPS, stack of 804 frames from 1250.Related Links: </p> | ||
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<br>Rukl Plate 20 | <br>Rukl Plate 20 | ||
<p align="left"><b>Tomorrow's LPOD: </b> Looking Acroos Orientale</p> | <p align="left"><b>Tomorrow's LPOD: </b> Looking Acroos Orientale</p> | ||
| − | + | </tr> | |
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</table> | </table> | ||
<br> | <br> | ||
<table width="100%" border="0" cellspacing="2" cellpadding="4"> | <table width="100%" border="0" cellspacing="2" cellpadding="4"> | ||
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| − | + | <td><hr></td> | |
| − | + | </tr> | |
| − | + | <tr><td> | |
| − | + | <p align="center" class="main_titles"><b>Author & Editor:</b><br> | |
| − | + | [mailto:tychocrater@yahoo.com Charles A. Wood]</p> | |
| − | + | <p align="center" class="main_titles"><b>Technical Consultant:</b><br> | |
| − | + | [mailto:anthony@perseus.gr Anthony Ayiomamitis]</p> | |
| − | + | <p align="center" class="main_titles"><b>Contact Translator:</b><br> | |
| − | + | [mailto:pablolonnie@yahoo.com.mx" class="one Pablo Lonnie Pacheco Railey] (Es)<br> | |
| − | + | [mailto:chlegrand@free.fr" class="one Christian Legrand] (Fr)</p> | |
| − | + | <p align="center" class="main_titles"><b>[mailto:webuser@observingthesky.org Contact Webmaster]</b></p> | |
| − | + | <p align="center" class="main_titles"><b>A service of:</b><br> | |
| − | + | [http://www.observingthesky.org/" class="one ObservingTheSky.Org]</p> | |
| − | + | <p align="center" class="main_titles"><b>Visit these other PODs:</b> <br> | |
| − | + | [http://antwrp.gsfc.nasa.gov/apod/astropix.html" class="one Astronomy] | [http://www.msss.com/" class="one Mars] | [http://epod.usra.edu/" class="one Earth]</p> | |
| − | + | </td></tr> | |
</table> | </table> | ||
<p> </p> | <p> </p> | ||
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===COMMENTS?=== | ===COMMENTS?=== | ||
Click on this icon [[image:PostIcon.jpg]] at the upper right to post a comment. | Click on this icon [[image:PostIcon.jpg]] at the upper right to post a comment. | ||
Revision as of 18:29, 4 January 2015
Memory of a Crater
<nobr>Memory of a Crater</nobr> |
<img src="archive/2005/02/images/LPOD-2005-02-18.jpeg" border="0"> |
Image Credit: Wes Higgins
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|
Memory of a Crater Craters form on an existing surface, which will continue to change in the future. For example, the 30 km wide Lambert is excavated into Mare Imbrium lavas, and the crater’s ridges of continuous ejecta visibly lie on the mare surface. A few subsequent random impacts have formed craters on these deposits, and at least two small younger craters are seen inside Lambert. The daubs of grayish rays and perhaps a cluster of secondary craters to the right of Lambert and another at the center left edge of the image demonstrate that ejecta from Copernicus has also slightly modified this area. But all landscape modifications are not as modest. Consider the ghostly ring south of Lambert. This feature (Lambert R - R for ruin) could be some exotic volcanic structure, perhaps similar to a terrestrial ring dike, but more likely it is the remnant of a hapless impact crater that formed on a lower, intermediate level of Imbrium’s lavas, before the basin was filled with its final thickness of lava. The rising level of Imbrium lavas must have climbed the flanks of the crater and, finally reaching a low spot, cascaded down into the 55 km wide pit. It appears that the mare lavas completely inundated the crater, leaving only a few low arcuate ridges, joined by wrinkle ridges. There is one other unusual feature to note – on the left side of Lambert there is a flat, narrow ridge about 40 km long that feathers into the surrounding lava. The origin of this flow-like ridge is a mystery. Technical Details: Related Links: Tomorrow's LPOD: Looking Acroos Orientale |
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Author & Editor: Technical Consultant: Contact Translator: A service of: Visit these other PODs: |
COMMENTS?
Click on this icon File:PostIcon.jpg at the upper right to post a comment.
