Exchange of atmospheric water vapour with the regolith of the Martian surface: Phobos-2 infrared spectrometer (ISM) data reanalysed using improved topography data (MOLA/MGS)

Details Exchange of atmospheric water vapour with the regolith of the Martian surface: Phobos-2 infrared spectrometer (ISM) data reanalysed using improved topography data (MOLA/MGS) Exchange of atmospheric water vapour with the regolith of the Martian surface: Phobos-2 infrared spectrometer (ISM) data reanalysed using improved topography data (MOLA/MGS)

Apr 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003eaeja.....6821w&link_type=abstract

EGS - AGU - EUG Joint Assembly, Abstracts from the meeting held in Nice, France, 6 - 11 April 2003, abstract #6821

Computer Science

Scientific paper

The water vapour content of the Martian atmosphere is one of the main topics in the research on this planet. Water vapour is the minor constituent of the Martian atmosphere with the highest variability. Its seasonal and latitudional variations reach a factor of 10. In addition, diurnal variations and variations correlated with the properties of the Martian surface are observed. Also the vertical distribution of this gas is variable. These variations are caused by sublimation and condensation of the polar caps and surface frost, adsorption to and desorption from the surface regolith, and advective transport of the gas due to the global circulation. Both, seasonal changes and diurnal and spatial variations imply that exchange of water vapour between atmosphere and the regolith of the Martian surface plays a major rôle in explaining the variations of atmospheric water vapour. Measurements of the Martian atmosphere's water vapour content have been made by ground-based observations as well as by observations from spacecrafts in orbits around Mars. The observations by the Vikings were followed by measurements by the Phobos-2 spacecraft in the year 1989. Its imaging infrared spectrometer (ISM) provided spectra in the wavelength range of 0.8-3.5 μm. Very high signal-to-noise ratio allows one to study variations of weak spectral features of atmospheric H_2O. Unfortunately, they overlap with the spectral bands of the dominant constituent of the Martian atmosphere, carbon dioxide. So, appropiate column density data are needed to correct for the contribution of CO_2. Using high resolution data of the Martian surface's topography provided by the Mars Orbiter Laser Altimeter (MOLA, Mars Global Surveyor) to calculate the CO_2 column density the ISM spectral data are reanalysed. First results of this investigation will be presented. The main goal of this investigation is to study spatial variability of the atmospheric water vapour abundance and its correlation with topography and surface properties. This would provide a clue to the mechanism of H_2O exchange between atmosphere and regolith. As an example data observed above the Tharsis volcanoes are compared to data measured above the surrounding planes.

Affiliated with

Also associated with

No associations

Rating

Exchange of atmospheric water vapour with the regolith of the Martian surface: Phobos-2 infrared spectrometer (ISM) data reanalysed using improved topography data (MOLA/MGS) does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with Exchange of atmospheric water vapour with the regolith of the Martian surface: Phobos-2 infrared spectrometer (ISM) data reanalysed using improved topography data (MOLA/MGS), we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and Exchange of atmospheric water vapour with the regolith of the Martian surface: Phobos-2 infrared spectrometer (ISM) data reanalysed using improved topography data (MOLA/MGS) will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-843563