Exposed subsurface ice sheets in the Martian mid-latitudes

被引：180

作者：

Dundas, Colin M. ^{[1
]}

Bramson, Ali M. ^{[2
]}

Ojha, Lujendra ^{[3
]}

Wray, James J. ^{[4
]}

Mellon, Michael T. ^{[5
]}

Byrne, Shane ^{[2
]}

McEwen, Alfred S. ^{[2
]}

Putzig, Nathaniel E. ^{[6
]}

Viola, Donna ^{[2
]}

Sutton, Sarah ^{[2
]}

Clark, Erin ^{[2
]}

Holt, John W. ^{[7
]}

机构：

[1] US Geol Survey, Astrogeol Sci Ctr, 2255 N Gemini Dr, Flagstaff, AZ 86001 USA

[2] Univ Arizona, Lunar & Planetary Lab, Tucson, AZ 85721 USA

[3] Johns Hopkins Univ, Dept Earth & Planetary Sci, Baltimore, MD 21218 USA

[4] Georgia Inst Technol, Sch Earth & Atmospher Sci, Atlanta, GA 30332 USA

[5] Johns Hopkins Univ, Appl Phys Lab, Laurel, MD USA

[6] Planetary Sci Inst, 1546 Cole Blvd,Suite 120, Lakewood, CO 80401 USA

[7] Univ Texas Austin, Inst Geophys, Jackson Sch Geosci, Austin, TX 78758 USA

来源：

SCIENCE | 2018年 / 359卷 / 6372期

关键词：

GROUND ICE; MARS; STABILITY; DEPOSITS; PLANITIA; METER; AGES;

D O I：

10.1126/science.aao1619

中图分类号：

O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];

学科分类号：

07 ; 0710 ; 09 ;

摘要：

Thick deposits cover broad regions of the Martian mid-latitudes with a smooth mantle; erosion in these regions creates scarps that expose the internal structure of the mantle. We investigated eight of these locations and found that they expose deposits of water ice that can be >100 meters thick, extending downward from depths as shallow as 1 to 2 meters below the surface. The scarps are actively retreating because of sublimation of the exposed water ice. The ice deposits likely originated as snowfall during Mars' high-obliquity periods and have now compacted into massive, fractured, and layered ice. We expect the vertical structure of Martian ice-rich deposits to preserve a record of ice deposition and past climate.

引用

页码：199 / 201

页数：3

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