The considerable differences in bulk composition of the moon and the earth have led most investigators to favor the capture hypothesis of lunar origin. However, upon closer examination all forms of the hypothesis still seem much less plausible dynamically than formation by accretion,. i.e., acquisition of the moon in many small pieces rather than as predominantly one body. Models of accretion do suggest that the proto-lunar matter had a significantly different history from the proto-earth matter. A better understanding of collisions is needed to infer the compositional consequences of this history. Recent work on the acceleration of the moon's orbit exacerbates the time scale problem of orbital evolution. However, it now is much clearer that the locus of tidal dissipation is in the oceans and hence that the solution to the time scale problem lies in differing oceanic configurations in the past. This review is an updating of an article by Kauta [1971]. statistics of the most ancient craters indicate the mass Since then there has been a considerable sharpening of the distribution of forming planetesimals, as was suggested by compositional constraints, based mainly on data generated by Baldwin [1974]. the Apollo project. There also has been some work on the Geophysical data pertaining to the lunar interior also place more general problem of solar system origin, which is constraints on origin circumstances. The slight attenuation of necessarily the context for origin of the moon. seismic waves indicates a lithosphere 1000 km thick surround-The long-standing problem of the low density of the moon ing an asthenosphere that is only 10% of the moon's mass relative to that of the earth has been firmly resolved as being [Toks;Sz et at., 1974]. Within this asthenosphere a denser core caused by a deficiency in iron. Indeed, the permeability of the of 400-km radius has been inferred [Nakamura et at., 1974], moon inferred from magnetometry [Dyat et at., 1974] and the close to the upper limit allowed by the moment of inertia indication that the lunar mantle is olivine from seismic wave [Kauta et at., 1974]. Reasonably consistent with these findings velocity models [Nakamura et at., 1974] imply an iron content are internal temperatures inferred from a combination of lunar of only 6%, compared to 30% in the earth and meteorites. If interaction with the solar wind [Dyat et at., 1974] and the mantle is assumed to be pyroxene, the lunar iron content laboratory measurement of the temperature dependence of becomes 13% [Dyat et at., 1974]. ' electrical conductivity [Duba et at., 1974]. It appears that Additional major constraints generated by the Apollo radioactive heat sources have been removed from the outerchemical data are that the moon as a whole is severely depleted most 1000 km, only the central asthenosphere now being in volatiles and considerably enriched in refractory silicates. heated to partial melting. Because of the need for a crust thick enough to compensate 6km mare-terra height differences isostatically [Kauta et at., ...