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Probing the Distribution of Ozone on Mars

Author
Fast, K. E.
Published
[2008].
Physical Description
1 electronic document
Additional Creators
Lefevre, F., Hewagama, T., Delgado, J. D., Kostiuk, T., Livengood, T. A., and Annen, J.
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Summary
We present the application of infrared heterodyne line shapes of ozone on Mars to those produced by radiative transfer modeling of ozone profiles predicted by photochemistry-coupled general circulation models (GCM), and to contemporaneous column abundances measured by Mars Express SPICAM. Ozone is an important tracer of photochemistry in Mars' atmosphere, serving as an observable with which to test predictions of photochemical models. Infrared heterodyne measurements of ozone absorption features on Mars have been obtained at various Martian seasons from 1988 until present at the NASA Infrared Telescope Facility (IRTF) on Mauna Kea, Hawai'i [I]. The NASAiGoddard Space Flight Center spectrometers used were the Infrared Heterodyne Spectrometer (IRHS) [2, 3] and, since 2003, the Heterodyne Instrument for Planetary Wind and Composition (HIPWAC) [4]. A description the infrared heterodyne technique applied to ground-base observations of Martian ozone can be found in [I]. The most recent measurements on February 21-24 2008 UT at Ls=35deg were made by HIPWAC on or near the Mars Express orbital path with the goal of acquiring spectra that can be directly compared to nadir observations by SPICAM.
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Collection
NASA Technical Reports Server (NTRS) Collection.
Note
Document ID: 20080041580.
3rd International Workshop on the Mars Atmosphere: Modeling and Observations; 10-13 Nov. 2008; Williamsburg, VA; United States.
Terms of Use and Reproduction
Copyright, Distribution as joint owner in the copyright.
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