Difference between revisions of "February 18, 2005"
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=Memory of a Crater= | =Memory of a Crater= | ||
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| − | <tr><td><div align="center" class="main_sm">Image Credit: [mailto:starman2@charter.net Wes Higgins]</p> | + | <tr><td><div align="center" class="main_sm"><p>Image Credit: [mailto:starman2@charter.net Wes Higgins]</p> |
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<p align="center"><b>Memory of a Crater</b></p> | <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> | <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> | + | <blockquote> |
| − | <p align="left" | + | <p align="right">— [mailto:tychocrater@yahoo.com Chuck Wood]</p></blockquote> |
| + | <p align="left"><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> | ||
<p><b>Related Links:</b><br> | <p><b>Related Links:</b><br> | ||
[http://www.higginsandsons.com/astro/ Wes' Web site ] | [http://www.higginsandsons.com/astro/ Wes' Web site ] | ||
<br>Rukl Plate 20 | <br>Rukl Plate 20 | ||
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| + | <p><b>Yesterday's LPOD:</b> [[February 17, 2005|Keeping Up With The Smythiis]] </p> | ||
| + | <p><b>Tomorrow's LPOD:</b> [[February 19, 2005|Looking Across Orientale]] </p> | ||
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<p align="center" class="main_titles"><b>Author & Editor:</b><br> | <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> | ||
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Latest revision as of 15:11, 15 March 2015
Memory of a Crater
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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: Yesterday's LPOD: Keeping Up With The Smythiis Tomorrow's LPOD: Looking Across Orientale |
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Author & Editor: |
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