Wind-related processes detected by the Spirit rover at Gusev crater, Mars

Science

Volumn 305, Issue 5685, 2004, Pages 810-821

  Greeley, R ^a   Squyres, S W ^b   Arvidson, R E ^c   Bartlett, P ^d   Bell III, J F ^b   Blaney, D ^e   Cabrol, N A ^f   Farmer, J ^a   Farrand, B ^g   Golombek, M P ^e   Gorevan, S P ^d   Grant, J A ^h   Haldemann, A F C ^e   Herkenhoff, K E ⁱ   Johnson, J ⁱ   Landis, G ^e   Madsen, M B ^j   McLennan, S H ^k   Moersch, J ^l   Rice Jr , J W ^a   Richter, L ^m   Ruff, S ^a   Sullivan, R J ^b   Thompson, S D ^a   Wang, A ^c   Weitz, C M ⁿ   Whelley, P ^a   more..

^a ARIZONA STATE UNIVERSITY   (United States)

^b Department of Molecular Biology and Genetics   (United States)

^c WASHINGTON UNIVERSITY   (United States)

^d HONEYBEE ROBOTICS   (United States)

^e CALIFORNIA INSTITUTE OF TECHNOLOGY   (United States)

^f NASA AMES RESEARCH CENTER   (United States)

^g UNIVERSITY OF COLORADO   (United States)

^h DEPARTMENT OF PALEOBIOLOGY   (United States)

ⁱ U S GEOLOGICAL SURVEY   (United States)

^j UNIVERSITY OF COPENHAGEN   (Denmark)

^k STONY BROOK UNIVERSITY   (United States)

^l UNIVERSITY OF TENNESSEE   (United States)

^m GERMAN AEROSPACE CENTER DLR   (Germany)

ⁿ NASA HEADQUARTERS   (United States)

more..

Author keywords

[No Author keywords available]

Indexed keywords

ABRASION; PLANETARY LANDERS; ROCKS; SEDIMENTS; UNMANNED VEHICLES; WIND EFFECTS;

GUSEV CRATER, MARS; SPIRIT ROVER; WIND DEFLECTION; WIND-ABRADED ROCKS;

MARTIAN SURFACE ANALYSIS;

CRATER; DEFLATION; EOLIAN PROCESS; MARS; PLANETARY SURFACE;

ARTICLE; ASTRONOMY; ATMOSPHERE; CALIBRATION; IMAGE ANALYSIS; PHYSICS; PRIORITY JOURNAL; ROCK; SEDIMENT; SPACE FLIGHT; WIND;

EVOLUTION, PLANETARY; EXTRATERRESTRIAL ENVIRONMENT; MARS; WIND;

EMMELICHTHYS STRUHSAKERI;

EID: 3843068624     PISSN: 00368075     EISSN: None     Source Type: Journal    
DOI: 10.1126/science.1100108     Document Type: Article

References (39)

1. Reviewed by R. Greeley, N. Lancaster, S. Lee, P. Thomas, in Mars, H. H. Kieffer, B. Jakosky, Eds. (Univ. of Arizona Press, Tucson, AZ, 1992). pp. 730-766.
2. S. W. Squyres et al., Science 305, 794 (2004).
3. J. A. Crisp et al., J. Geophys. Res. 108, 10.1029/ 2002JE002038 (2003).
4. M. P. Golombek et al., J. Geophys. Res. 108, 10.1029/ 2003JE002074 (2003).
5. M. P. Golombek et al., Lunar Planet. Sci. XXXV, abstr. 2185 (2004).
6. At 0.19 (36), the landing site has the lowest albedo as determined from orbit of the entire landing ellipse. From analysis of broadband (0.4 to 1.0 μm) images from the MER Pancam; the average albedo measured from the surface is 0.25 ± 0.05 (10).
7. 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 this 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.
8. "Dust" is an imprecise term but is commonly used for material on Earth that is smaller than about 40 μm and that is transported primarily in suspension. Estimates for dust on Mars suggest diameters of a few micrometers, although these particles are thought to stick together in some cases, possibly by electrostatic charges, to form aggregates of larger sizes (37).
9. R. E. Arvidson et al., Science 305, 821 (2004).
10. 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.
11. J. F. Belt III et al., Science 305, 800 (2004).
12. K. E. Herkenhoff et al., J. Geophys. Res. 108, 10.1029/ 2003JE002076 (2003).
13. J. B. Pollack et al., J. Geophys. Res. 82, 4479 (1977).
14. P. H. Smith et al., Science 278, 1758 (1997).
15. M. G. Tomasko, L. R. Doose, M. Lemmon, P. H. Smith, E. Wegryn, J. Geophys. Res. 104, 8987 (1999).
16. P. R. Christensen et al., Science 305, 837 (2004).
17. K. Y. McSween et al., Science 305, 842 (2004).
18. K. E. Herkenhoff et al., Science 305, 824 (2004).
19. J. F. Bell et al., Icarus 158, 56 (2002).
20. J. L. Bandfield, J. Geophys. Res. 107, 10.1029/ 2001JE001510 (2002).
21. R. P. Sharp, J. Geol. 71, 617 (1963).
22. Ripples are bedforms composed of sand and granules that are moved by surface creep induced by the impact of saltating sands, whereas dunes are larger bedforms typically composed of finer sands and not formed directly by saltation processes.
23. R. Greeley et al., J. Geophys. Res. 104, 8573 (1999).
24. M. P. Golombek, N. T. Bridges, J. Geophys. Res. 105, 1841 (2000).
25. J. A. Grant et al., Science 305, 807 (2004).
26. R. Greeley, J. D. Iversen, Wind as a Geological Process: Earth, Mars, Venus, and Tiran (Cambridge Univ. Press, Cambridge, 1985).
27. R. Greeley, J. D. Iversen, Geophys. Res. Lett. 14, 925 (1987).
28. M. R. Raupach, Boundary-Layer Meterol. 60, 375 (1992).
29. M. R. Raupach, D. A. Gillette, J. F. Leyes, J. Geophys. Res. 98, 3023 (1993).
30. N. T. Bridges et al., J. Geophys. Res. 104, 8595 (1999).
31. R. Greeley et al., J. Geophys. Res. 87, 10009 (1992).
32. N. T. Bridges et al., Planet. Space Sci. 52, 199 (2004).
33. S. P. Gorevan et al., J. Geophys. Res. 108, 10.1029/ 2003JE002061 (2003).
34. S. R. C. Rafkin, T. I. Michaels, J. Geophys. Res. 108, 10.1029/2002JE002027 (2003).
35. D. Toigo, M. I. Richardson, J. Geophys. Res. 108, 10.1029/2003JE002064 (2003).
36. R. Greeley et al., J. Geophys. Res. 108, 10.1029/ 2002JE002006 (2003).
37. M. T. Mellon, B. M. Jakosky, H. H. Kieffer, P. R. Christensen, Icarus 148, 437 (2000).
38. R. Greeley, J. Geophys. Res. 84, 6248 (1979).
39. Our work was supported by NASA by contracts through the Jet Propulsion Laboratory.