Probing Ozone Vertical Distribution and Photochemistry on Mars with Infrared Heterodyne Spectroscopy

Details Probing Ozone Vertical Distribution and Photochemistry on Mars with Infrared Heterodyne Spectroscopy Probing Ozone Vertical Distribution and Photochemistry on Mars with Infrared Heterodyne Spectroscopy

Sep 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006dps....38.6011f&link_type=abstract

American Astronomical Society, DPS meeting #38, #60.11; Bulletin of the American Astronomical Society, Vol. 38, p.599

Astronomy and Astrophysics

Astronomy

Scientific paper

Ozone (O3) is an important tracer of photochemistry in the atmosphere of Mars. Increasingly complex photochemistry-coupled global circulation models require measurements of spatial, vertical, temporal and seasonal ozone variations in order to test their predictions and broaden the overall understanding of the chemistry and dynamics of the martian atmosphere. Infrared heterodyne spectroscopy at 9.7 μm with spectral resolving power >106 is the only technique that can directly measure fully-resolved line shapes of Martian atmospheric ozone features from the surface of the Earth. This and other techniques such oxygen dayglow measurements and space-based UV observations probe the ozone column differently, providing information on the vertical distribution of ozone. We present preliminary retrievals of ozone vertical distribution by combining different observing techniques. We also present recent IR heterodyne observations of ozone at the martian season of LS=10° not previously measured with this technique and compare those ozone abundances and previous retrievals to predictions of photochemistry.
This work was supported by the NASA Planetary Astronomy Program.

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