Other
Scientific paper
Dec 2006
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p23a0040d&link_type=abstract
American Geophysical Union, Fall Meeting 2006, abstract #P23A-0040
Other
0360 Radiation: Transmission And Scattering, 0394 Instruments And Techniques, 5210 Planetary Atmospheres, Clouds, And Hazes (0343), 5405 Atmospheres (0343, 1060), 5464 Remote Sensing
Scientific paper
Very high resolution optical spectroscopy (where the profiles and shifts of emission/absorption lines are used to infer atmospheric properties) has been successfully applied to the terrestrial atmosphere for measurements of wind and temperature. The application of these techniques to other planets (and to a certain extent, Earth) is complicated by the presence of optically thick aerosols. In particular, it is important to account for Doppler shifts in what would otherwise be considered monochromatic scattering. We describe here a radiative transfer model that accurately and efficiently calculates line profiles and shifts considering both multiple scattering and Doppler shifting. The model itself is based on the well documented and thoroughly tested Discrete Ordinate method. We use this model to construct a method of retrieving wind on Mars. We propose here an observation scenario using a combination of limb emission line observations for the middle and upper atmosphere of Mars and downward looking (sub-limb) measurements of carbon dioxide absorption lines to cover the first few scale heights of the atmosphere where the dust makes limb viewing difficult. Above 35 kilometers or so, the emission line techniques are very similar to those used in the past for terrestrial observations. The limb measurements below this, and the sub-limb measurements, have no tested terrestrial analog. We describe methods for constructing wind retrievals for these observations here. Our model and retrieval methods can be generalized to other atmospheres where remote optical wind measurements are complicated by multiple scattering. These methods are particularly useful where multiple scattering occurs in the presence of a strong molecular absorber such as carbon dioxide. Thus, the techniques described here can be used to study the atmosphere of Venus as well as the terrestrial lower atmosphere.
DeMajistre Robert
Morgan Molly
Talaat Elsayed
Yee J.
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