Ion clusters and the Venus ultraviolet haze layer.

Abstract

The daytime ionosphere of Venus is observed between 100 and 500 km altitude. Below 100 km ion clustering processes combine with the low temperature at the mesopause to form coagulates, giving rise to the UV haze layer which has frequently been observed. Ion ratios involving carbon dioxide are considered, taking into consideration also the possibility of a presence of nitrogen and oxygen in the Venus atmosphere.