Radar echoes from the surface of Venus are analyzed with a view to describing the mean behavior by suitable adjustment of available theories. By shortening the pulse width to give better resolution near the front portion of Venus, we find that a theory by Muhleman fits better than other theories. We show varia- bility of the echoes near normal incidence as the subradar point moves. We find that difficulty arises in fitting a spherically symmetric model to Venus because the echoes exhibit patchiness or structure which move as the planet rotates.
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Jurgens et al. (1970) studied this question.