Physics
Scientific paper
Aug 1997
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1997icar..128..474f&link_type=abstract
Icarus, Volume 128, Issue 2, pp. 474-479.
Physics
8
Scientific paper
The observed sulfur vapor abundance near Venus' surface is lower than the amount needed for pyrite to be stable. This conclusion is reached using either the observed S_3 abundance or the S_2 abundance calculated from the observations of S_3. Furthermore, the atmosphere is too oxidizing for pyrite to be stable. Pyrite is unstable at Venus' modal radius of 6051.4 km (1992. P. G. Ford and G. H. Pettengill, J. Geophys. Res. 97, 13,103-13,114) where T = 740K and P = 95.6 bar (1986. A. Seiff, J. T. Schofield, A. J. Kliore, F. W. Taylor, S. S. Limaye, H. E. Revercomb, L. A. Sromovsky, V. I. Kerzhanovich, V. I. Moroz, and M. Ya. Marov, In The Venus International Reference Atmosphere (A. J. Kliore, V. I. Moroz, and G. M. Keating, Eds.), pp. 3-58. Pergamon Press, Oxford). Pyrite is also unstable at 6056 km (T = 705 K, P = 71.2 bar), which is at 4.6 km altitude in the low radar emissivity region (Pettengill et al. 1996). Any pyrite on Venus' surface should decompose rapidly to iron oxides and sulfur vapor, as experimentally demonstrated by Fegley et al. (1995. B. Fegley Jr., K. Lodders, A. H. Treiman, and G. Klingelhofer. Icarus 115, 159-180).
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