Origin of ureilite meteorites and implications for planetary accretion

The present analysis of the ureilite meteorites suggests that these are formed by well-understood processes, as indicated by such findings as their being partial melt residues rather than cumulates and their forming in a large chondritic body with heterogeneous O isotopic composition. Slow diffusion of the O in solid and molten silicates ensured that partial melting did not homogenize the O isotopes of the residues. These and other determinations furnish a plausible origin for ureilites as residues from the partial melting of isotopically heterogeneous chondritic material.