Atomic oxygen features at 1304 and 1356 ¿ detected by the Orbiting Ultraviolet Spectrometer (OUVS) on Pioneer Venus are compared to theoretical emission models. Limb scans from three orbits of the OI 1304 ¿ emission were analyzed using an improved model which removes the restrictive assumptions of complete frequency redistribution and isothermal multiple scattering. Data-model comparisons indicate the OI 1304 ¿ emission rates observed are consistent with an O density 40% of the BUS model. It is also found that the emission at 1356 ¿ is consistent with the sum of the CO fourth positive band at 1352 ¿ and the OI doublet at 1356, 1358 ¿, if an O density equal to 40% of the BUS model is used to calculate the OI emission rate.