Constraints on the martian crust away from the InSight landing site

被引：4

作者：

Li, Jiaqi ^{[1
]}

Beghein, Caroline ^{[1
]}

McLennan, Scott M. ^{[2
]}

Horleston, Anna C. ^{[3
]}

Charalambous, Constantinos ^{[4
]}

Huang, Quancheng ^{[5
]}

Zenhausern, Geraldine ^{[6
]}

Bozdag, Ebru ^{[5
]}

Pike, W. T. ^{[4
]}

Golombek, Matthew ^{[7
]}

Lekic, Vedran ^{[8
]}

Lognonne, Philippe ^{[9
]}

Banerdt, W. Bruce ^{[7
]}

机构：

[1] Univ Calif Los Angeles, Dept Earth Planetary & Space Sci, Los Angeles, CA 90095 USA

[2] SUNY Stony Brook, Dept Geosci, Stony Brook, NY 11794 USA

[3] Univ Bristol, Sch Earth Sci, Bristol, Avon, England

[4] Imperial Coll London, Dept Elect & Elect Engn, London, England

[5] Colorado Sch Mines, Dept Geophys, Golden, CO 80401 USA

[6] Swiss Fed Inst Technol, Inst Geophys, Zurich, Switzerland

[7] CALTECH, Jet Prop Lab, Pasadena, CA 91109 USA

[8] Univ Maryland, Dept Geol, College Pk, MD 20742 USA

[9] Univ Paris Cite, Inst Phys Globe Paris, CNRS, F-75005 Paris, France

来源：

NATURE COMMUNICATIONS | 2022年 / 13卷 / 01期

基金：

美国国家航空航天局;

关键词：

SEISMIC DETECTION; MARS; DISCONTINUITIES; VELOCITIES; THICKNESS; WAVES; ROCKS;

D O I：

10.1038/s41467-022-35662-y

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：

The most distant marsquake recorded so far by the InSight seismometer occurred at an epicentral distance of 146.3 & PLUSMN; 6.9(o), close to the western end of Valles Marineris. On the seismogram of this event, we have identified seismic wave precursors, i.e., underside reflections off a subsurface discontinuity halfway between the marsquake and the instrument, which directly constrain the crustal structure away (about 4100-4500 km) from the InSight landing site. Here we show that the Martian crust at the bounce point between the lander and the marsquake is characterized by a discontinuity at about 20 km depth, similar to the second (deeper) intra-crustal interface seen beneath the InSight landing site. We propose that this 20-km interface, first discovered beneath the lander, is not a local geological structure but likely a regional or global feature, and is consistent with a transition from porous to non-porous Martian crustal materials.

引用

页数：10

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