Molecular Oxygen in the Venus Middle Atmosphere

Details Molecular Oxygen in the Venus Middle Atmosphere Molecular Oxygen in the Venus Middle Atmosphere

Sep 1998

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1998dps....30.4803m&link_type=abstract

American Astronomical Society, DPS meeting #30, #48.03; Bulletin of the American Astronomical Society, Vol. 30, p.1105

Astronomy and Astrophysics

Astronomy

Scientific paper

The primary photochemical cycle of the Venus middle atmosphere is photolysis of CO_2 to form CO and O on the day side and the re-formation of CO_2 via catalytic cycles. Previous models (Krasnopolsky & Parshev [1983]; Yung & DeMore [1982]) qualitatively explained the stability of the atmosphere but could not quantitatively explain the low O_2 column abundance (< 0.3 x 10(18) molec cm(-2) [Trauger & Lunine 1983]) or the intense night side O_2 (a(1) Delta ) airglow [Crisp {et al. }1996]. Our one-dimensional, steady-state model (based on the latest laboratory data and observations) has been able to reproduce (within measurement uncertainty and temporal/spatial variability) the SO profile [Na et al. 1994], the SO_2 abundance and scale height at the cloud top [Na et al. 1994], the CO profile [Clancy & Muhleman 1991], and the ``global average'' O_2 (a(1) Delta ) airglow [Crisp {et al. }1996] using only gas-phase chemistry by adjusting selected reaction rates within their one-sigma uncertainties. If the stability of ClCO is increased by its assessed uncertainty, then radiative transfer model calculations indicate the predicted ``global average'' O_2 column abundance from the photochemical model is consistent with the observed 2 sigma upper limit. Calculations indicate horizontal transport is important in understanding the distribution of oxygen in the Venus atmosphere and suggest simultaneous, spatially-resolved retrievals of CO mixing ratios and temperatures are needed.

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