Abstract
Due to the presence of opaque clouds at high altitudes, it is difficult to survey the surface of Venus in the optical spectral range. At the same time, in the under-cloud layer, there are transparency windows at the wavelengths λ = 1.08, 0.85, and 0.65 μm. At these wavelengths, the gaseous absorption (in the whole atmosphere rather than only in the under-cloud layer) is weaker, and the atmospheric transparency is mainly determined by the scattering on molecules. The paper presents the results of the Monte-Carlo computer modeling of the imaging of the surface from a balloon or a lander. It has been shown that the imaging from the lower boundary of the clouds is possible.
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