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The lunar radar echo is divided into specular and Lambert scatter components, the specular component being derived from a statistical model of the lunar surface. The theoretical impulse response is compared with experimental data from Trexler, and the theoretical frequency response is compared with some preliminary Goldstone moonbounce experimental data. The theory indicates that the Lambert component will be visible at high power levels and would probably become apparent about 1000 μsec after the leading edge of the echo. A value for reflectivity of 0.01 found from the level of the scatter component is used to derive an estimate of some of the average properties of the lunar surface.
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W. E. Brown (1960) studied this question.
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