Results from the Mars Pathfinder camera

被引：227

作者：

Smith, PH

Bell, JF

Bridges, NT

Britt, DT

Gaddis, L

Greeley, R

Keller, HU

Herkenhoff, KE

Jaumann, R

Johnson, JR

Kirk, RL

Lemmon, M

Maki, JN

Malin, MC

Murchie, SL

Oberst, J

Parker, TJ

Reid, RJ

Sablotny, R

Soderblom, LA

Stoker, C

Sullivan, R

Thomas, N

Tomasko, MG

Ward, W

Wegryn, E

机构：

[1] CORNELL UNIV,ITHACA,NY 14853

[2] CALTECH,JET PROP LAB,PASADENA,CA 91109

[3] US GEOL SURVEY,FLAGSTAFF,AZ 86001

[4] ARIZONA STATE UNIV,TEMPE,AZ 85287

[5] MAX PLANCK INST AERON,KATHENBURG LINDAU,GERMANY

[6] DLR,BERLIN,GERMANY

[7] MALIN SPACE SCI SYST,SAN DIEGO,CA

[8] JOHNS HOPKINS UNIV,APPL PHYS LAB,BALTIMORE,MD 21218

[9] NASA,AMES RES CTR,MOFFETT FIELD,CA 94035

来源：

SCIENCE | 1997年 / 278卷 / 5344期

关键词：

D O I：

10.1126/science.278.5344.1758

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：

Images of the martian surface returned by the Imager for Mars Pathfinder (IMP) show a complex surface of ridges and troughs covered by rocks that have been transported and modified by fluvial, aeolian, and impact processes. Analysis of the spectral signatures in the scene (at 440- to 1000-nanometer wavelength) reveal three types of rock and four classes of soil. Upward-looking IMP images of the predawn sky show thin, bluish clouds that probably represent water ice forming on local atmospheric haze (opacity similar to 0.5). Haze particles are about 1 micrometer in radius and the water vapor column abundance is about 10 precipitable micrometers.

引用

页码：1758 / 1765

页数：8

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[1] VISIBLE AND NEAR-INFRARED DIFFUSE REFLECTANCE SPECTRA OF PYROXENES AS APPLIED TO REMOTE-SENSING OF SOLID OBJECTS IN SOLAR-SYSTEM [J].