Textures of the soils and rocks at Gusev crater from Spirit's Microscopic Imager

Science

Volumn 305, Issue 5685, 2004, Pages 824-826

  Herkenhoff, K E ^a   Squyres, S W ^b   Arvidson, R ^c   Bass, D S ^d   Bell III, J F ^b   Bertelsen, P ^e   Cabrol, N A ^f   Gaddis, L ^a   Hayes, A G ^b   Hviid, S F ^g   Johnson, J R ^a   Kinch, K M ^h   Madsen, M B ^e   Maki, J N ^d   McLennan, S H ⁱ   McSween, H Y ^j   Rice Jr , J W ^k   Sims, M ^f   Smith, P H ^l   Soderblom, L A ^a   Spanovich, N ^l   Sullivan, R ^b   Wang, A ^m   more..

^a U S GEOLOGICAL SURVEY   (United States)

^b Department of Obstetrics Gynecology   (United States)

^c WASHINGTON UNIVERSITY   (United States)

^d CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^e UNIVERSITY OF COPENHAGEN   (Denmark)

^f NASA AMES RESEARCH CENTER   (United States)

^g MAX PLANCK INSTITUT FÜR SONNENSYSTEMFORSCHUNG   (Germany)

^h AARHUS UNIVERSITY   (Denmark)

ⁱ STONY BROOK UNIVERSITY   (United States)

^j UNIVERSITY OF TENNESSEE   (United States)

^k ARIZONA STATE UNIVERSITY   (United States)

^l UNIVERSITY OF ARIZONA   (United States)

^m WASHINGTON UNIVERSITY   (United States)

more..

Author keywords

[No Author keywords available]

Indexed keywords

ABRASION; DUST; IMAGING SYSTEMS; MINERALOGY; SOILS; TEXTURES; VOLCANIC ROCKS; WIND EFFECTS;

AGGLOMERATES; GUSEV CRATER, MARS; MICROSCOPIC IMAGERS;

MARTIAN SURFACE ANALYSIS;

CRATER; LITHOLOGY; MARS; PLANETARY SURFACE; TEXTURE;

ARTICLE; ASTRONOMY; DUST; IMAGE ANALYSIS; MINERALIZATION; PRIORITY JOURNAL; ROCK; SOIL ANALYSIS; SPACE FLIGHT; SURFACE PROPERTY; VOLCANO; WEATHERING; WIND;

EMMELICHTHYS STRUHSAKERI;

EID: 3843058906     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.3050824     Document Type: Article

References (25)

1. K. E. Herkenhoff et al., J. Geophys. Res. 108, 8065 (2003).
2. S. W. Squyres, et al., J. Geophys. Res. 108, 8062 (2003).
3. J. F. Bell III et al., J. Geophys. Res. 108, 8063 (2003).
4. J. N. Maki et al., J. Geophys. Res. 108, 8071 (2003).
5. A martian solar day has a mean period of 24 hours 39 min 35.244 s and is referred to as a sol to distinguish it from a roughly 3% shorter solar day on Earth. A martian sidereal day, as measured with respect to the fixed stars, is 24 hours 37 min 22.663 s, as compared with 23 hours 56 min 04.0905 s for Earth. See www.giss.nasa.gov/ tools/mars24 for more information.
6. The term martian soil is used here to denote any loose, unconsolidated materials that can be distinguished from rocks, bedrock, or strongly cohesive sediments. No implication of the presence or absence of organic materials or living matter is intended.
7. R. E. Arvidson et al., Science 305, 821 (2004).
8. P. Bertelsen et al., Science 305, 827 (2004).
9. S. W. Squyres et al., Science 305, 794 (2004).
10. J. F. Bell III et al., Science 305, 800 (2004).
11. R. V. Morris et al., Science 305, 833 (2004).
12. S. Gorevan et al., J. Geophys. Res. 108, 8068 (2003).
13. R. Gellert et al., Science 305, 829 (2004).
14. The ability to resolve individual grains with the MI depends on the illumination of the scene and the contrast between the grain and its surroundings. Typically, an object must subtend at least 3 pixels to be recognized in an image.
15. G. Landis et al., in Lunar and Planetary Science XXXV (LPI Publication 1197, Lunar and Planetary Institute, Houston, CD-ROM, 2004).
16. J. B. Butler, S. N. Lane, J. H. Chandler, J. Hydraulic Res. 39, 1 (2001).
17. D. M. Rubin, J. Sed. Res. 74, 160 (2004).
18. We used NIH Image, version 1.63 (24).
19. C. K. Wentworth, J. Geol. 30, 377 (1922).
20. R. Greeley et al., Science 305, 810 (2004).
21. Names have been assigned to areographic features by the Mars Exploration Rover (MER) team for planning and operations purposes. The names are not formally recognized by the International Astronomical Union.
22. H. Y. McSween et al., Science 305, 842 (2004).
23. P. R. Christensen et al., Science 305, 837 (2004).
24. J. Wagner et al., in preparation.
25. The U.S. Geological Survey MER Team developed MI software and created various data products, including some of those displayed in this issue: B. Archinal, J. Barrett, K. Becker, T. Becker, D. Burr, D. Cook, T. Hare, A. Howington-Kraus, R. Kirk, E. Lee, M. Rosiek, B. Sucharski, T. Sucharski, and J. Torson (project engineer). The Ames MER team and Mark Lemmon developed software to merge focal sections and generate anaglyphs from them. The MER Rover Planners provided excellent support of the MI investigation by commanding the arm and MI dust cover. Reviews of this paper by M. Chapman, L. Keszthelyi, S. Thompson, C. Weitz, and four anonymous referees are much appreciated. The work described here was supported by the NASA Jet Propulsion Laboratory Mars Exploration Rover project. The use of trade, product, or firm names in this paper does not imply endorsement by the U. S. government.