Abstract
The general theory of radar reflection from planetary surfaces that was described in an earlier publication is extended, and it is shown how the slope of the surface profile can be obtained from the autocorrelation function of the signal envelope. The theory is applied to lunar observations made at 440, 151, and 38.25 Mc/s, and a value of 14° is obtained for the rms slope. The angular power spectrum is found to be wavelength-dependent except at the short wavelength limit, where it depends only on the surface slope.
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