In the present paper, entry into the atmosphere of the planet Venus is considered. For direct entry, radiative heating is approximately equivalent to convective heating. Thus heating calculations must consider the radiative contribution in some detail, and such calculations require inputs of the radiative properties, not only of the inviscid layer species but also the major species of the ablation layer.nThe lower atmosphere of Venus is presently believed to consist almost entirely of carbon dioxide. Reference 1, for instance, concludes that carbon dioxide comprises about 97 percent or more by volume of the lower atmosphere, with nitrogen as the next most abundant gas. The radiation spectrum from the shock layer of a Venus probe would there
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