Providing constant concentration of SO2, COS and CO below altitudes of
measurements (12-26 km), the chemical composition of the near-surface
atmosphere of Venus appears to be in agreement with a model of thermo
chemical gaseous equilibrium in the C-O-S system at the condition of t
he modal planetary radius. The thermochemical equilibrium between CO2,
SO2, COS and CO at the level of modal radius indicated an oxygen fuga
city logf(O2)==-21.3 +/- 0.2 bar. That value appears to be quite near
with the condition of hematite-magnetite buffer providing non-unity ac
tivities of those solid phases. Besides, that value of oxygen fugacity
is consistent with the result of the ''Contrast'' experiment on the V
enera-13,14 landers as well as with the reflectance properties of soil
at the Venera-9,10 landing sites. The presented model of thermochemic
al equilibrium predicts concentration gradients for gases in the thin
(1-2 km) layer in the near-surface atmosphere, Oxygen fugacity within
the equilibrium layer seems to be governed by CO2, SO2 and COS and dec
reases with increase of elevation. That situation should result in the
growth of hematite stability from lowlands to more elevated levels. T
he,model of thermochemical equilibrium between gases could not apply f
or the Venus highlands. Lack of the thermochemical equilibrium between
gases al highland condition does not allow to estimate oxygen fugacit
y in the frame of methods of equilibrium chemical thermodynamics.