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

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.

[1]  J. Pollack,et al.  Scattering by nonspherical particles of size comparable to wavelength - A new semi-empirical theory and its application to tropospheric aerosols , 1980 .

[2]  R. M. Haberle,et al.  Diurnal variations in optical depth at Mars , 1989 .

[3]  James B. Pollack,et al.  Viking Lander image analysis of Martian atmospheric dust , 1995 .

[4]  Nicolas Thomas,et al.  Optical properties of the Martian aerosols as derived from Imager for Mars Pathfinder midday sky brightness data , 1999 .

[5]  F. Ferri,et al.  Dust devils as observed by Mars Pathfinder , 1999 .

[6]  Mark T. Lemmon,et al.  Properties of dust in the Martian atmosphere from the Imager on Mars Pathfinder , 1999 .

[7]  M. Lemmon,et al.  Opacity of the Martian atmosphere measured by the Imager for Mars Pathfinder , 1999 .

[8]  R. Todd Clancy,et al.  Hubble Space Telescope observations of the Martian aphelion cloud belt prior to the Pathfinder mission: Seasonal and interannual variations , 1999 .

[9]  John Scott Drilling,et al.  in Allen''''s Astrophysical Quantities , 2000 .

[10]  A. Cox,et al.  Allen's astrophysical quantities , 2000 .

[11]  R. Todd Clancy,et al.  Mars aerosol studies with the MGS TES emission phase function observations: Optical depths, particle sizes, and ice cloud types versus latitude and solar longitude , 2003 .

[12]  William M. Drennan,et al.  Constraining the inertial dissipation method using the vertical velocity variance , 2003 .

[13]  S. T. Elliot,et al.  Mars Exploration Rover Athena Panoramic Camera (Pancam) investigation , 2003 .

[14]  M. Klimesh,et al.  Mars Exploration Rover engineering cameras , 2003 .

[15]  H. Graber,et al.  Impact of flow distortion corrections on turbulent fluxes estimated by the inertial dissipation method during the FETCH experiment on R/V L'Atalante , 2003 .

[16]  C. Vera.  Interannual and interdecadal variability of atmospheric synoptic‐scale activity in the Southern Hemisphere , 2003 .

[17]  R. Greeley,et al.  Mars: Dust devil track survey in Argyre Planitia and Hellas Basin , 2003 .

[18]  Mark T. Lemmon,et al.  Dust deposition at the Mars Pathfinder landing site: observations and modeling of visible/near-infrared spectra , 2003 .

[19]  Thomas E. Wolverton,et al.  Miniature Thermal Emission Spectrometer for the Mars Exploration Rovers , 2003 .

[20]  K Davis,et al.  Localization and Physical Property Experiments Conducted by Opportunity at Meridiani Planum , 2004, Science.

[21]  R J Sullivan,et al.  Wind-Related Processes Detected by the Spirit Rover at Gusev Crater, Mars , 2004, Science.

[22]  Amitabha Ghosh,et al.  First Atmospheric Science Results from the Mars Exploration Rovers Mini-TES , 2004, Science.

[23]  D. Ming,et al.  Localization and Physical Properties Experiments Conducted by Spirit at Gusev Crater , 2004, Science.

[24]  D. Ming,et al.  Pancam Multispectral Imaging Results from the Opportunity Rover at Meridiani Planum , 2004, Science.

[25]  Michael D. Smith.  Interannual variability in TES atmospheric observations of Mars during 1999–2003 , 2004 .

[26]  D. Ming,et al.  Pancam Multispectral Imaging Results from the Spirit Rover at Gusev Crater , 2004, Science.