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Galactic cosmic-ray source compositions, (Z/H)GCRS from H to Pb and ~10^8 -10^14 eV, differ from solar-local interstellar, (Z/H)SS or (Z/H)ISM by~20-200x. Both are mostly just mixes of core collapse (CCSN) and thermonuclear(SN Ia) supernova ejecta. The (Z/H)ISM come from steady unbiased accumulationover Gyrs. But the cosmic ray mass mixing ratio, universal ISM/CCSN ~4:1 ofswept-up ISM and ~10x metallicity ejecta show that (Z/H)GCRS come from basicSedov-Taylor bulk mixing of homologous, expanding CCSN in their OB clusterself-generated superbubbles, further enriched by highly biased grain-sputteringinjection during diffusive shock acceleration (DSA). Moreover, this mixingratio now reveals that the cosmic rays are primarily accelerated as theirevolving reverse shock radius and energy passes through their maxima.Refractories and volatiles, first deposited in fast ejecta and ISM grains infreely expanding ejecta, are simultaneously Coulomb-sputtered FCS by turbulentH and He as suprathermal ions into DSA that carries them to cosmic-rayenergies. This bulk mixing selectively increases source mix abundancies (Z/H)SM/ (Z/H)SS by ~2-10; and injection by grain condensation and implantationfractions FGC, by another ~6, while Z^0.67 Coulomb grain sputtering enrichmentsFCS give an added ~4-20. Applying these basic processes of mixing and injectionto solar system (Z/H)SS produces grain-injected, source-mix (Z/H)SMGI thatmatch major cosmic ray abundances (Z/H)GCRS to within 35 % with no freeparameters. Independently confirming grain injection, (Z/H)GCRS shows nodetectable contribution of Fe from SN Ia, although producing ~1/2 Fe in ISM,but there is also no dust in SN Ia remnants, unlike CCSN.

The Origin of Cosmic Rays: How Their Composition Defines Their Sources and Sites, and the Processes of Their Mixing, Injection and Acceleration