Difference between revisions of "March 30, 2004"
| (5 intermediate revisions by the same user not shown) | |||
| Line 1: | Line 1: | ||
__NOTOC__ | __NOTOC__ | ||
=Silicic Domes?= | =Silicic Domes?= | ||
| + | <!-- Start of content --> | ||
<table width="640" border="0" align="center" cellpadding="6" cellspacing="2"> | <table width="640" 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-2004-03-30.jpeg|LPOD-2004-03-30b.jpeg}}</div> | |
</td> | </td> | ||
</tr> | </tr> | ||
| Line 19: | Line 20: | ||
<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 class="story" align="center"><b>Silicic Domes? </b></p> | <p class="story" align="center"><b>Silicic Domes? </b></p> | ||
| − | <p class="story" align="left"> Lunar volcanism was pervasive, producing mare lava [ | + | <p class="story" align="left"> Lunar volcanism was pervasive, producing mare lava [[February_8,_2004|flows]] and associated |
| − | features such as sinuous [ | + | features such as sinuous [[February_29,_2004|rilles]], pyroclastic |
| − | [ | + | [[February_10,_2004|deposits]] and [[March_26,_2004|domes]]. The magmas that made |
these features were basalts - melted mantle rocks rich in silica, oxygen, iron and magnesium. The latter two | these features were basalts - melted mantle rocks rich in silica, oxygen, iron and magnesium. The latter two | ||
elements give basalts the dark color we see in the maria. Lunar scientists have hunted for other types of | elements give basalts the dark color we see in the maria. Lunar scientists have hunted for other types of | ||
volcanic rocks, and these two domes near the crater Gruithuisen are the best known examples. Gruithuisen Gamma is | volcanic rocks, and these two domes near the crater Gruithuisen are the best known examples. Gruithuisen Gamma is | ||
about 20 km wide and 1200 m high; Gruithuisen Delta is 13 km wide and 1550 m high. Their steep sides suggest they | about 20 km wide and 1200 m high; Gruithuisen Delta is 13 km wide and 1550 m high. Their steep sides suggest they | ||
| − | were formed by more viscous lavas than normal mare domes such as those near [ | + | were formed by more viscous lavas than normal mare domes such as those near [[January_2,_2004|Cauchy]] |
| − | Cauchy] and [ | + | and [[March_26,_2004|Hortensius]]. Mathematical models of dome growth reaffirm this |
idea. On Earth, lavas with similar flow characteristics to the Gruithuisen domes are rhyolites, dacites and | idea. On Earth, lavas with similar flow characteristics to the Gruithuisen domes are rhyolites, dacites and | ||
basaltic andesites - rocks with more silica and less iron and magnesium than basalts. If these lunar domes are | basaltic andesites - rocks with more silica and less iron and magnesium than basalts. If these lunar domes are | ||
| Line 39: | Line 40: | ||
[http://www.agu.org/pubs/crossref/2003/2002JE001909.shtml Lunar Gruithuisen and Mairan domes: Rheology and mode of emplacement]<br> | [http://www.agu.org/pubs/crossref/2003/2002JE001909.shtml Lunar Gruithuisen and Mairan domes: Rheology and mode of emplacement]<br> | ||
[http://www.lpi.usra.edu/research/lunar_orbiter/images/img/iv_145_h1.jpg Lunar Orbiter IV view]</p> | [http://www.lpi.usra.edu/research/lunar_orbiter/images/img/iv_145_h1.jpg Lunar Orbiter IV view]</p> | ||
| − | <p | + | <p><b>Yesterday's LPOD:</b> [[March 29, 2004|Hoover Dam (and Surroundings)]] </p> |
| + | <p><b>Tomorrow's LPOD:</b> [[March 31, 2004|Great Graben!]] </p> | ||
</td></tr> | </td></tr> | ||
</table> | </table> | ||
| Line 51: | Line 53: | ||
<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> | ||
| − | < | + | <!-- 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> | ||
<p> </p> | <p> </p> | ||
| − | ---- | + | <!-- End of content --> |
| − | + | {{wiki/ArticleFooter}} | |
| − | |||
Latest revision as of 19:14, 7 February 2015
Silicic Domes?
|
Image Credit: Tan Wei Leong |
|
Silicic Domes? Lunar volcanism was pervasive, producing mare lava flows and associated features such as sinuous rilles, pyroclastic deposits and domes. The magmas that made these features were basalts - melted mantle rocks rich in silica, oxygen, iron and magnesium. The latter two elements give basalts the dark color we see in the maria. Lunar scientists have hunted for other types of volcanic rocks, and these two domes near the crater Gruithuisen are the best known examples. Gruithuisen Gamma is about 20 km wide and 1200 m high; Gruithuisen Delta is 13 km wide and 1550 m high. Their steep sides suggest they were formed by more viscous lavas than normal mare domes such as those near Cauchy and Hortensius. Mathematical models of dome growth reaffirm this idea. On Earth, lavas with similar flow characteristics to the Gruithuisen domes are rhyolites, dacites and basaltic andesites - rocks with more silica and less iron and magnesium than basalts. If these lunar domes are made of silica-rich magma the next question is why? Technical Details: Related Links: Yesterday's LPOD: Hoover Dam (and Surroundings) Tomorrow's LPOD: Great Graben! |
|
Author & Editor: |
COMMENTS?
Register, Log in, and join in the comments.
