An explanation of the SO2 profile on Venus from the Vega 1 and 2 UV spectrometers

Details An explanation of the SO2 profile on Venus from the Vega 1 and 2 UV spectrometers An explanation of the SO2 profile on Venus from the Vega 1 and 2 UV spectrometers

May 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003dps....35.3703f&link_type=abstract

American Astronomical Society, DPS meeting #35, #37.03; Bulletin of the American Astronomical Society, Vol. 35, p.983

Astronomy and Astrophysics

Astronomy

Scientific paper

We use chemical equilibrium calculations to model the SO2 gradient from the UV spectrometers on Vega 1 and 2. They found SO2 decreases from ˜125 ppmv to ˜25 ppmv with decreasing altitude. We can match the gradient by varying the oxygen elemental abundance with altitude. Variations range from +47 (cloud base) to -186 ppm (near surface) of the total oxygen elemental abundance. Figure 1 compares our results to the reported SO2 profile. We reproduce many features of gas chemistry in Venus' lower atmosphere including: (1) increases in SO3 and H2SO4 near the cloud base, (2) decreases in H2O upward from the cloud base, (3) decreases in OCS above ˜22 km, and (4) increases in OCS below ˜22 km. However CO increases towards Venus' surface.
Supported by NASA NAG5-11037.

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