Photochemistry of the Martian Atmosphere: Global Model and Seasonal, Latitudinal, and Diurnal Variations

Details Photochemistry of the Martian Atmosphere: Global Model and Seasonal, Latitudinal, and Diurnal Variations Photochemistry of the Martian Atmosphere: Global Model and Seasonal, Latitudinal, and Diurnal Variations

May 2005

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2005agusm.p21d..05k&link_type=abstract

American Geophysical Union, Spring Meeting 2005, abstract #P21D-05

Physics

5405 Atmospheres: Composition And Chemistry, 5409 Atmospheres: Structure And Dynamics, 5410 Composition, 6225 Mars

Scientific paper

Three types of models have been developed to study Mars' photochemistry. A steady-state model for global-mean conditions is the only way to calculate abundances of the long living species (H2, O2, and CO) and therefore to validate a chosen photochemistry. A steady-state model for local conditions adopts the known abundances of H2, O2, and CO and the photochemistry from the global-mean model to simulate the measured abundances of O3, O2(1Δ), and H2O2 and their variations with local conditions for a diurnal-mean insolation. A time-dependent model for local conditions is for the same purpose but accounts for the local-time variability. The local models were calculated at the conditions of the O3 (Espenak et al. 1991, Clancy et al. 1999), O2(1Δ) (Krasnopolsky 2003), and H2O2 (Clancy et al. 2004, Encrenaz et al. 2004) observations. Input data for the models (temperature profiles, H2O abundances, and dust opacities) are taken from the MGS/TES observations (Smith 2004), simultaneous or made at similar conditions. Comparison of results of the models with the observations favors an effective heterogeneous sink of odd hydrogen on the surface of water ice particles in the clouds and hazes on Mars. This sink reduces the strong anticorrelation between water vapor and ozone which follows from the pure gas-phase models. Results of the modeling and their implications will be discussed.

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