Photochemistry of the martian atmosphere: Seasonal, latitudinal, and diurnal variations

• Published in: Icarus (New York, N.Y. 1962) N.Y. 1962), 2006-11, Vol.185 (1), p.153-170
• Main Author: Krasnopolsky, Vladimir A.
• Format: Article
• Language: English
• Subjects: Abundances; Astronomy; atmosphere; Atmospheres; composition; Earth, ocean, space; Exact sciences and technology; Mars; Photochemistry; Solar system
• ISSN: 0019-1035; 1090-2643
• DOI: 10.1016/j.icarus.2006.06.003

There is a significant progress in the observational data relevant to Mars photochemistry in the current decade. These data are not covered by and sometimes disagree with the published models. Therefore we consider three types of models for Mars photochemistry. A steady-state model for global-mean conditions is currently the only way to calculate the abundances of long living species (H 2, O 2, and CO). However, our model does not fit the observed CO abundance using gas-phase chemistry and reasonable values of heterogeneous loss of odd hydrogen on the water ice aerosol. The second type of the calculated models is steady-state models for local conditions. The MGS/TES data on temperature profiles, H 2O, and dust are input parameters for these models. The calculations have been made for nine seasonal points spread over the martian year and for twelve latitudes with a step of 10° for each season. The only adopted heterogeneous reaction is a weak loss of H 2O 2 on water ice with probability of 5 × 10 −4 . The results are in good agreement with the recent observations of the O 2 dayglow at 1.27 μm and the O 3 and H 2O 2 abundances. Global maps of the seasonal and latitudinal behavior of these species have been made. The third type of models is a time-dependent model for local conditions. These models show that odd hydrogen quickly converts to H 2O 2 at the nighttime and the chemistry is switched off while the association of O, the heterogeneous loss of H 2O 2, and eddy diffusion continue. This requires significant changes in the global-mean and local steady-state models discussed above, and these changes have been properly done. The calculated diurnal variations of Mars photochemistry are discussed. The martian photochemistry at low and middle latitudes is significantly different in the aphelion period at L S = 10 ° – 130 ° from that in the remaining part of the year.