| タイトル | Impact Melt in Small Lunar Highlands Craters |
| 本文（外部サイト） | http://hdl.handle.net/2060/20110007190 |
| 著者（英） | Cintala, M. J.; Hawke, B. R.; Robinson, M. S.; Barnouin, O.; Plescia, J. B. |
| 著者所属（英） | NASA Johnson Space Center |
| 発行日 | 2011-03-07 |
| 言語 | eng |
| 内容記述 | Impact-melt deposits are a typical characteristic of complex impact craters, occurring as thick pools on the crater floor, ponds on wall terraces, veneers on the walls, and flows outside and inside the rim. Studies of the distribution of impact melt suggested that such deposits are rare to absent in and around small (km to sub-km), simple impact craters. noted that the smallest lunar crater observed with impact melt was approximately 750 m in diameter. Similarly, theoretical models suggest that the amount of melt formed is a tiny fraction (<1%) of the total crater volume and thus significant deposits would not be expected for small lunar craters. LRO LROC images show that impact-melt deposits can be recognized associated with many simple craters to diameters down to approximately 200 m. The melt forms pools on the crater floor, veneer on the crater walls or ejecta outside the crater. Such melt deposits are relatively rare, and can be recognized only in some fresh craters. These observations indicate that identifiable quantities of impact melt can be produced in small impacts and the presence of such deposits shows that the material can be aggregated into recognizable deposits. Further, the present of such melt indicates that small craters could be reliably radiometrically dated helping to constrain the recent impact flux. |
| NASA分類 | Lunar and Planetary Science and Exploration |
| レポートNO | JSC-CN-22687 |
| 権利 | Copyright, Distribution as joint owner in the copyright |
|
