Ozone on Mars: The effects of clouds and airborne dust

Mars Ozone: Mariner 9 Revisited

“…Using a constant mixing ratio for 63 (e.g., Wehrbein, 1979;Lindner, 1988) and no chemical or radiative interaction between 03 and clouds/dust, Fig. 3 shows that when typical amounts of dust and cloud are present that significant underestimation of Os abundance occurs.…”

“…03 absorption cross-sections from 2000 A to 3200 A are included (Daumont et al, 1983;Freeman et al, 1984). Ultraviolet absorption cross-sections for CO2, O2, H2O, HC»2 and HI&I are negligible (e.g., Lindner, 1988;1991;1993b). The Rayleigh scattering optical depth is computed as in Hansen and Travis (1974), using parameters appropriate for Mars.…”

“…Atmospheric composition is taken as 95% CO2 (Owen et al, 1977). The altitude dependence of 03 is based on model results (Lindner, 1988).…”

“…Over 20 photochemical models of the martian atmosphere have been published, and 03 is often used as a benchmark for these models (e.g., Lindner, 1988;Shimazaki, 1989;Krasnopolsky, 1993). 03 abundance has been inferred from instrumentation on several spacecraft, with the most complete coverage provided by Mariner 9 (Barth et al, 1973;Lane et al, 1973;Wehrbein et al, 1979).…”

“…The only atmospheric absorption in the 2000 to 3000 A wavelength region was previously assumed to come from the Hartley band system of ozone (Barth et al, 1973;Lane et al 1973), which has an opacity of order unity at winter polar latitudes (Lindner, 1988). Therefore the amount of ozone was inferred by fitting this absorption feature with laboratory data of ozone absorption, as shown in Fig.…”