Why Pyrite Is Unstable on the Surface of Venus

✍ Scribed by Bruce Fegley Jr.

• Publisher: Elsevier Science
• Year: 1997
• Tongue: English
• Weight: 335 KB
• Volume: 128
• Category: Article
• ISSN: 0019-1035
• DOI: 10.1006/icar.1997.5744

✦ Synopsis

Thus, the experimental pyrite decomposition rates are relevant to Venus where the S 2 pressure is lower than in the experiments of Fegley et al.

The observed sulfur vapor abundance near Venus' surface (1995a). I then consider in situ observations of Venus' lower atmosphere is lower than the amount needed for pyrite to be stable. This and use the observed S 3 partial pressure and thermodynamic data from conclusion is reached using either the observed S 3 abundance the literature to calculate the S 2 pressure in Venus' lower atmosphere. or the S 2 abundance calculated from the observations of S 3 . Finally, I show that (1) both the observed S 3 pressure and the calculated Furthermore, the atmosphere is too oxidizing for pyrite to be S 2 pressure in Venus' near-surface atmosphere are lower than the amount needed for pyrite stability, and (2) that Venus' atmosphere is too oxidizing stable. Pyrite is unstable at Venus' modal radius of 6051.4 km for pyrite to be stable.