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We present a comprehensive evolutionary model of the Sun's protoplanetarydisk, constructed to resolve the "CAI Storage" problem of meteoritics. Wepredict the abundances of calcium-rich, aluminum-rich inclusions (CAIs) andrefractory lithophile elements under the central assumption that Jupiter's$\sim 30 \, M_{\oplus}$ core forms at about 3 AU at around 0.6 Myr and opened agap CAIs are trapped in the pressure maximum beyond Jupiter; carbonaceouschondrites formed there. Inside Jupiter's orbit, CAIs were depleted byaerodynamic drag; ordinary and enstatite chondrites formed there. For 16chondrites and achondrites, we review meteoritic data on their CAI andrefractory abundances and their times of formation, constrained by radiometricdating and thermal models. We predict their formation locations, findingexcellent consistency with other location information (water content, asteroidspectra and parent bodies). We predict the size of particle concentrated byturbulence for each chondrite, finding excellent matches to each chondrites'smean chondrule diameter. These consistencies imply meteorite parent bodiesassembled quickly from local materials concentrated by turbulence, and usuallydid not migrate far. We predict CI chondrites are depleted in refractorylithophile elements relative to the Sun, by about 12% (0.06 dex). We constrainthe variation of turbulence parameter $\alpha$ in the disk, and find a limitedrole for magnetorotational instability, favoring hydrodynamical instabilitiesin the outer disk, plus magnetic disk winds in the inner disk. Between 3 and 4Myr at least, gas persisted outside Jupiter but was depleted inside it, and thesolar nebula was a transition disk.

The Effect of Jupiter's Formation on the Distribution of Refractory Elements and Inclusions in Meteorites