Climatology of Ozone on Mars from SPICAM/MEX UV/IR Nadir Measurements

Details Climatology of Ozone on Mars from SPICAM/MEX UV/IR Nadir Measurements Climatology of Ozone on Mars from SPICAM/MEX UV/IR Nadir Measurements

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006agufm.p14a..04p&link_type=abstract

American Geophysical Union, Fall Meeting 2006, abstract #P14A-04

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0317 Chemical Kinetic And Photochemical Properties, 1060 Planetary Geochemistry (5405, 5410, 5704, 5709, 6005, 6008), 6225 Mars

Scientific paper

The european mission Mars Express arrived at Mars in January 2004, during Mars's late northern winter. On board, the dual UV/IR spectrometer SPICAM is dedicated to monitor the martian atmosphere, and has recorded spectra for more than a full martian year. We analyse spectra of the backscattered solar light from SPICAM UV spectrometer in the [110--320] nm range. They were recorded on the day side in a nadir geometry (downward looking mode) where the surface of Mars is observed through the atmosphere. Some of these spectra show a strong absorption band around 250 nm, which is the spectral signature of ozone in the UV. The dataset coverage in season and latitude is variable, depending on observational and technical constrains. Strong spatial and temporal variations in the ozone column-density are observed. At high latitudes of both hemispheres, ozone seems to be present at fall, winter and early spring, to disappear during the spring, and to be totally absent during the summer. We discuss the comparison with predictions from the three-dimensional distribution of ozone computed by the General Circulation Model (GCM) described by Lefevre et al, 2004.Except in a few circumstances, the observed behaviour is well captured by the model, which will allow to calculate and predict other parameters not easy to measure. Even when ozone is found at its maximum value, it is still 200-300times less than on Earth, allowing harmful UV solar radiation to reach the ground. In the infrared, SPICAM is able to measure O2 emission at 1.27 μm and water vapor at 1.38 μm. We explore the correlation between H2O and ozone distributions and their implications on the martian photochemisty.

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