Astronomy and Astrophysics – Astronomy
Scientific paper
Sep 2008
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2008dps....40.6205y&link_type=abstract
American Astronomical Society, DPS meeting #40, #62.05; Bulletin of the American Astronomical Society, Vol. 40, p.513
Astronomy and Astrophysics
Astronomy
Scientific paper
The chemical and dynamical processes in the atmosphere of Venus are poorly known. The recently obtained profiles of CO and OCS provide a new constraint on these processes. The two species are intimately coupled. CO2 photolysis occurring in the upper atmosphere above the cloud tops provides the major source of CO, which will be transported to the lower atmosphere. The ultimate sink is to react with sulfur and oxygen compounds by either thermochemistry or heterogeneous chemistry or a combination of both to recycle back to CO2 or to form OCS. The latter is then transported to a higher region of the atmosphere and get photolyzed. We have shown recently that the observed meridional distribution of OCS at 33 km can well be explained by current knowledge of dynamics and photochemistry, assuming a uniform mixing ratio (37 ppmv) of OCS at the surface. Venus Express (VIRTIS-M) obtained profiles of CO at 36 km and found that the mixing ratio increased by about 50% from the equator to latitude of 60S. The increase feature is expected as the air mass ascends at low latitudes and descends at mid to high latitudes (Hadley cell). In this presentation, we will adopt the current knowledge of dynamics and chemistry away from the surface and vary the lower boundary condition of CO and OCS. New chemistry for constraining the required boundary condition will be proposed, tested, and discussed.
Liang Manlai
Yung Yuk
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