Atmospheric Imaging Results from the Mars Exploration Rovers: Spirit and Opportunity-Reference-Cited by-同舟云学术

Atmospheric Imaging Results from the Mars Exploration Rovers: Spirit and Opportunity

Published:2004-12-03 Issue:5702 Volume:306 Page:1753-1756
ISSN:0036-8075
Container-title:Science
language:en
Short-container-title:Science

Author:

Lemmon M. T.¹²³⁴⁵,Wolff M. J.¹²³⁴⁵,Smith M. D.¹²³⁴⁵,Clancy R. T.¹²³⁴⁵,Banfield D.¹²³⁴⁵,Landis G. A.¹²³⁴⁵,Ghosh A.¹²³⁴⁵,Smith P. H.¹²³⁴⁵,Spanovich N.¹²³⁴⁵,Whitney B.¹²³⁴⁵,Whelley P.¹²³⁴⁵,Greeley R.¹²³⁴⁵,Thompson S.¹²³⁴⁵,Bell J. F.¹²³⁴⁵,Squyres S. W.¹²³⁴⁵

Affiliation:

1. Texas A&M University, College Station, TX 77843, USA.

2. Space Science Institute, Boulder, CO 80301, USA.

3. NASA Goddard Space Flight Center, Greenbelt, MD 20771, USA.

4. Cornell University, Ithaca, NY 14853, USA.

5. NASA Glenn Research Center, Cleveland, OH 44135, USA.

Abstract

A visible atmospheric optical depth of 0.9 was measured by the Spirit rover at Gusev crater and by the Opportunity rover at Meridiani Planum. Optical depth decreased by about 0.6 to 0.7% per sol through both 90-sol primary missions. The vertical distribution of atmospheric dust at Gusev crater was consistent with uniform mixing, with a measured scale height of 11.56 ± 0.62 kilometers. The dust's cross section weighted mean radius was 1.47 ± 0.21 micrometers (μm) at Gusev and 1.52 ± 0.18 μ at Meridiani. Comparison of visible optical depths with 9-μ optical depths shows a visible-to-infrared optical depth ratio of 2.0 ± 0.2 for comparison with previous monitoring of infrared optical depths.

Publisher

American Association for the Advancement of Science (AAAS)

Subject

Multidisciplinary

Reference32 articles.

1. R. Kahnet al., in Mars, H. H. Kieffer et al., Eds. (Univ. Arizona Press, Tucson, 1992), pp. 1017–1053.

2. M. D. Smith, Icarus167, 148 (2003).

3. Localization and Physical Properties Experiments Conducted by Spirit at Gusev Crater

4. Localization and Physical Property Experiments Conducted by Opportunity at Meridiani Planum

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 this from a roughly 3% shorter solar day on Earth. Sol 1 was defined to begin at local solar midnight immediately before landing.

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