Fog phenomena on Mars

Fog phenomena on Mars Mars Express High Resolution Stereo Camera (HRSC) images show impressive morning fog features in Valles Marineris and other regions of the surface of Mars. Temperatures have been determined, simultaneously to the imaging, by Mars Express Planetary Fourier Spectrometer (PFS). This identifies water ice rather than frozen CO 2 as the cause of the fog observations in Valles Marineris. Numerical estimates of the water vapor pressure, and the related atmospheric water content, at the frost-point (temperature of freezing or “re-sublimation” of water vapor) by a 1-dimensional planetary boundary layer model indicate that conditions in the planetary boundary layer can indeed temporarily favor the formation of ice particles. A systematic registration of sites of fog observations shows preferred regions and seasons on Mars for fog phenomena. In the first instance, the fog phenomena seem to be induced or supported by orographic effects but not directly by the distribution pattern of the atmospheric vapor or by the regional subsurface water content. This paper documents and thermodynamically verifies the existence of fog of water ice particles in the near-surface atmosphere of Mars. http://www.deepdyve.com/assets/images/DeepDyve-Logo-lg.png Planetary and Space Science Elsevier

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Publisher
Elsevier
Copyright
Copyright © 2009 Elsevier Ltd
ISSN
0032-0633
eISSN
1873-5088
D.O.I.
10.1016/j.pss.2009.08.003
Publisher site
See Article on Publisher Site

Abstract

Mars Express High Resolution Stereo Camera (HRSC) images show impressive morning fog features in Valles Marineris and other regions of the surface of Mars. Temperatures have been determined, simultaneously to the imaging, by Mars Express Planetary Fourier Spectrometer (PFS). This identifies water ice rather than frozen CO 2 as the cause of the fog observations in Valles Marineris. Numerical estimates of the water vapor pressure, and the related atmospheric water content, at the frost-point (temperature of freezing or “re-sublimation” of water vapor) by a 1-dimensional planetary boundary layer model indicate that conditions in the planetary boundary layer can indeed temporarily favor the formation of ice particles. A systematic registration of sites of fog observations shows preferred regions and seasons on Mars for fog phenomena. In the first instance, the fog phenomena seem to be induced or supported by orographic effects but not directly by the distribution pattern of the atmospheric vapor or by the regional subsurface water content. This paper documents and thermodynamically verifies the existence of fog of water ice particles in the near-surface atmosphere of Mars.

Journal

Planetary and Space ScienceElsevier

Published: Dec 1, 2009

References

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