Origin of the anomalously rocky appearance of Tsiolkovskiy crater

被引：23

作者：

Greenhagen, Benjamin T. ^{[1
]}

Neish, Catherine D. ^{[2
]}

Williams, Jean-Pierre ^{[3
]}

Cahill, Joshua T. S. ^{[1
]}

Ghent, Rebecca R. ^{[4
,5
]}

Hayne, Paul O. ^{[6
]}

Lawrence, Samuel J. ^{[7
]}

Petro, Noah E. ^{[8
]}

Bandfield, Joshua L. ^{[9
]}

机构：

[1] Johns Hopkins Univ, Appl Phys Lab, 11100 Johns Hopkins Rd, Laurel, MD 20723 USA

[2] Univ Western Ontario, Dept Earth Sci, Biol & Geol Sci Bldg,Room 1026 1151 Richmond St N, London, ON N6A 5B7, Canada

[3] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, 595 Charles Young Dr East,Box 951567, Los Angeles, CA 90095 USA

[4] Ctr Earth Sci, Dept Earth Sci, 22 Russell St, Toronto, ON M5S 3B1, Canada

[5] Planetary Sci Inst, 1700 East Ft Lowell,Suite 106, Tucson, AZ 85719 USA

[6] CALTECH, Jet Prop Lab, ASU, 4800 Oak Grove Dr, Pasadena, CA 91109 USA

[7] Sch Earth & Space Explorat, POB 871404, Tempe, AZ 85287 USA

[8] NASA, Goddard Space Flight Ctr, 8800 Greenbelt Rd, Greenbelt, MD 20771 USA

[9] Space Sci Inst, 4750 Walnut St,Suite 205, Boulder, CO 80301 USA

来源：

ICARUS | 2016年 / 273卷

关键词：

Moon; surface; Cratering; Impact processes; Geological processes; Regoliths; LUNAR FARSIDE; GIORDANO BRUNO; IMPACT MELT; AGE; FLOWS; MOON; MARE;

D O I：

10.1016/j.icarus.2016.02.041

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Rock abundance maps derived from the Diviner Lunar Radiometer instrument on the Lunar Reconnaissance Orbiter (LRO) show Tsiolkovskiy crater to have high surface rock abundance and relatively low regolith thickness. The location of the enhanced rock abundance to the southeast of the crater is consistent with a massive, well-preserved impact melt deposit apparent in LRO Miniature Radio Frequency instrument circular polarization ratio data. A new model crater age using LRO Lunar Reconnaissance Orbiter Camera imagery suggests that while it originated in the Late Imbrian, Tsiolkovskiy may be the youngest lunar crater of its size (similar to 180 km diameter). Together these data show that Tsiolkovskiy has a unique surface rock population and regolith properties for a crater of its size and age. Explanation of these observations requires mechanisms that produce more large blocks, preserve boulders and large blocks from degradation to regolith, and/or uncover buried rocks. These processes have important implications for formation of regolith on the Moon. (C) 2016 Elsevier Inc. All rights reserved.

引用

页码：237 / 247

页数：11

共 40 条

[1]

[Anonymous], 2011, Planetary Surface Processes

[2] Lunar surface rock abundance and regolith fines temperatures derived from LRO Diviner Radiometer data [J].

Bandfield, Joshua L. ;

Ghent, Rebecca R. ;

Vasavada, Ashwin R. ;

Paige, David A. ;

Lawrence, Samuel J. ;

Robinson, Mark S. .

JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS, 2011, 116

[3]

Barabashov N.P., 1962, INT GEOL REV, V4, P631

[4] Age of Giordano Bruno crater as deduced from the morphology of its secondaries at the Luna 24 landing site [J].

Basilevsky, A. T. ;

Head, J. W. .

PLANETARY AND SPACE SCIENCE, 2012, 73 (01) :302-309

[5]

Boyce J.M., 1977, Lunar and Planetary Science Conference Proceedings, V8, P3495

[6] The Miniature Radio Frequency instrument's (Mini-RF) global observations of Earth's Moon [J].

Cahill, Joshua T. S. ;

Thomson, B. J. ;

Patterson, G. Wesley ;

Bussey, D. Benjamin J. ;

Neish, Catherine D. ;

Lopez, Norberto R. ;

Turner, F. Scott ;

Aldridge, T. ;

McAdam, M. ;

Meyer, H. M. ;

Raney, R. K. ;

Carter, L. M. ;

Spudis, P. D. ;

Hiesinger, H. ;

Pasckert, J. H. .

ICARUS, 2014, 243 :173-190

[7]

Campbell B.A., 2002, RADAR REMOTE SENSING

[8] Initial observations of lunar impact melts and ejecta flows with the Mini-RF radar [J].

Carter, Lynn M. ;

Neish, Catherine D. ;

Bussey, D. B. J. ;

Spudis, Paul D. ;

Patterson, G. Wesley ;

Cahill, Joshua T. ;

Raney, R. Keith .

JOURNAL OF GEOPHYSICAL RESEARCH-PLANETS, 2012, 117

[9]

Cheek L.C., 2012, P 43 LUN PLAN SCI C

[10]

CRADDOCK R, 1988, P LUN PLAN SCI C 18, P331

← 1 2 3 4 →