Photochemical Distribution of Venusian Sulfur and Halogen Species

Details Photochemical Distribution of Venusian Sulfur and Halogen Species Photochemical Distribution of Venusian Sulfur and Halogen Species

Oct 2010

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2010dps....42.1004p&link_type=abstract

American Astronomical Society, DPS meeting #42, #10.04; Bulletin of the American Astronomical Society, Vol. 42, p.994

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The photochemistry of Venus’ atmosphere from the cloudtops to 110 km has been modeled using an updated/expanded chemical scheme, with the view to improving our understanding of the vertical distributions of sulfur and halogen species. We mainly follow Yung and DeMore (1982), Mills (1998), Pernice et al. (2004), and Krasnopolsky (2009) in our choice of chemical reactions, chemical rate constants, and boundary conditions for several key species. We examine two models, with HCl mixing ratios of 10-7 and 4 x 10-7, respectively. The former corresponds to Venus Express observations made at high northern latitudes and the latter to the mid- to low-latitude value Young (1972) determined based on infrared measurements by Connes et al (1967). Both models agree satisfactorily with stratospheric observations of key species such as CO, O2 and SO2, but we hope to better quantify the implications of the different HCl mixing ratios observed. Additionally, we perform sensitivity tests where water is set to 31 ppm at 40 km, but vary the SO2 mixing ratio at the lower boundary about a nominal value of 25 ppm. We also consider a range of eddy diffusion profiles and other sensitivity studies. For most cases, K = Ko (n(z)/n_ref)-a, where Ko is the eddy diffusion coefficient at some reference altitude, n is the number density, z is altitude, and a is the variable parameter (<1). Our modeling suggests lower HCl abundances result in greater abundances of SO2, SO, and SO3 generally lower O2 abundances, and greater ClO abundances. Also, the effects on sulfur compounds seems more evident/pronounced for lower mixing ratios of SO2 at the lower boundary as well as higher up in the atmosphere i.e. above 58 km. We consider both SO2 observations of Bertaux et al (2009) and Sandor and Clancy (2010) in our analysis of results.

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