The Atmosphere of Venus

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Figure 8. Mixing ratios assumed in the baseline models of Grinspoon and Bullock (2001) shown as a function of altitude. Dotted line shows SO 2 mixing ratio as a function of altitude derived by Bertaux et al. (1996) from VEGA 1 and 2 entry probe data.!
Thermochemical equilibrium of atmospheric SO 2 with Venus surface minerals. The temperature/pressure curve for the Venus atmosphere is shown by the dashed line on the right, with the globally averaged surface temperature indicated by the diamond. SO 2 equilibrium with calcite is shown by the solid line on the left, SO 2 equilibrium with pyrite is shown by the solid line on the right. SO 2 is more than two orders more abundant on Venus than required for equilibrium with calcite, but it is close to equilibrium with pyrite and magnetite. However, for either of these reactions to be in equilibrium the reactants must exist at the surface. While there are no unequivocal data for the existence of either of these phases, CaCO 3 is a possible interpretation of the Venera XRF data for Ca. FeS 2 has been shown in laboratory experiments to have a lifetime of ~100 days at Venus surface conditions (Fegley et al. 1995), so it is unlikely to exist for geologically relevant timescales.
Page 1 and 2: The Atmosphere of Venus! David Grin
Page 4 and 5: New York Times 2/26/1963
Page 6 and 7: The heavens … …now are seen to
Page 8 and 9: A luxuriant garden… ! ! !… of s
Page 10: Radiative Processes
Page 13 and 14: Cloud Particles: Chemical Propertie
Page 15 and 16: Fast Atmospheric S Cycle CO 2 CO +
Page 17 and 18: Geologic Sulfur Cycle 2H 2 S + 3O 2
Page 19 and 20: Large Impacts, Steam Atmospheres, H
Page 21: The Faint Young Sun and Early Venus
Page 24 and 25: Venus vs. Earth. Extreme desiccatio
Page 26: Role of Water in Plate Tectonics
Page 30 and 31: CO 2 Atmosphere-Mineral Equilibrium
Page 32 and 33: Radiative Transfer Model Non-grey,
Page 34 and 35: Climate Evolution • Radiative- Co
Page 36 and 37: SO 2 variations & cloud brightening
Page 38 and 39: Globally synchronous formation of w
Page 42 and 43: Did Venus experience one great tran
Page 44 and 45: History of Venus: A Unified Scenari
Page 46 and 47: (D/H) VENUS = 120 ± 40 x (D/H) EAR
Page 48 and 49: Presently, the problem is underdete
Page 50 and 51: ASPERA! Escape of H+ occurs mostly
Page 52: Determination of wind fields from V
Page 55 and 56: Polar vortex dynamics Virtis data @
Page 58 and 59: UV UV 50 km NIR

The Atmosphere of Venus

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