Distal ejecta from lunar impacts: Extensive regions of rocky deposits

被引:43
作者
Bandfield, Joshua L. [1 ]
Cahill, Joshua T. S. [2 ]
Carter, Lynn M. [3 ]
Neish, Catherine D. [4 ]
Patterson, G. Wesley [2 ]
Williams, Jean-Pierre [5 ]
Paige, David A. [5 ]
机构
[1] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA
[2] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA
[3] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA
[4] Univ Western Ontario, Dept Earth Sci, 1151 Richmond St, London, ON N6A 3K7, Canada
[5] Univ Calif Los Angeles, Earth Planetary & Space Sci, Los Angeles, CA 90095 USA
关键词
Moon; surface; Impact processes; Infrared observations; Radar observations; RADIOMETER EXPERIMENT; CRATER; MOON; TEMPERATURES; CONSTRAINTS; MERCURY;
D O I
10.1016/j.icarus.2016.05.013
中图分类号
P1 [天文学];
学科分类号
0704 ;
摘要
Lunar Reconnaissance Orbiter (LRO) Diviner Radiometer, Mini-RF, and LRO Camera data were used to identify and characterize rocky lunar deposits that appear well separated from any potential source crater. Two regions are described: 1) A similar to 18,000 km(2) area with elevated rock abundance and extensive melt ponds and veneers near the antipode of Tycho crater (167.5 degrees E, 42.5 degrees N). This region has been identified previously, using radar and imaging data. 2) A much larger and more diffuse region, covering 730,000 km(2), centered near 310 degrees E, 35 degrees S, containing elevated rock abundance and numerous granular flow deposits on crater walls. The rock distributions in both regions favor certain slope azimuths over others, indicating a directional component to the formation of these deposits. The spatial distribution of rocks is consistent with the arrival of ejecta from the west and northwest at low angles (similar to 10-30 degrees) above the horizon in both regions. The derived age and slope orientations of the deposits indicate that the deposits likely originated as ejecta from the Tycho impact event. Despite their similar origin, the deposits in the two regions show significant differences in the datasets. The Tycho crater antipode deposit covers a smaller area, but the deposits are pervasive and appear to be dominated by impact melts. By contrast, the nearside deposits cover a much larger area and numerous granular flows were triggered. However, the features in this region are less prominent with no evidence for the presence of impact melts. The two regions appear to be surface expressions of a distant impact event that can modify surfaces across wide regions, resulting in a variety of surface morphologies. The Tycho impact event may only be the most recent manifestation of these processes, which likely have played a role in the development of the regolith throughout lunar history. (C) 2016 Elsevier Inc. All rights reserved.
引用
收藏
页码:282 / 299
页数:18
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