A review of the sources of analytical data for the chondritic meteorites is given, and the latest data, particularly for the minor elements, are tabulated. Though the composition of the chondrites is remarkably constant as compared with terrestrial rocks, important variations in the concentrations of certain major and minor constituents occur, which make it impossible to conclude that any one type of chondrite could have been produced from another by simple physical processes. This is true for the carbonaceous, enstatitic, and the high‐ and low‐iron‐group chondrites. The origin of these chondrites is discussed mostly with reference to the author’s suggestions about the origin of the solar system. Only very complicated processes can account for the detailed characteristics of these objects. The possibility that the carbonaceous chondrites and particularly Wiik's type 1 of this group are the primitive material from which the meteorites and planets originated is considered, and it is concluded that these objects as a group cannot be such material (a conclusion reached by the author some ten years ago). The case for the type 1 carbonaceous chondrites' being this material is better, but serious arguments against this conclusion can be advanced; it is concluded that even this material has undergone some extensive chemical pro