  We present a comprehensive evolutionary model of the Sun's protoplanetary
disk, constructed to resolve the "CAI Storage" problem of meteoritics. We
predict the abundances of calcium-rich, aluminum-rich inclusions (CAIs) and
refractory 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 a
gap CAIs are trapped in the pressure maximum beyond Jupiter; carbonaceous
chondrites formed there. Inside Jupiter's orbit, CAIs were depleted by
aerodynamic drag; ordinary and enstatite chondrites formed there. For 16
chondrites and achondrites, we review meteoritic data on their CAI and
refractory abundances and their times of formation, constrained by radiometric
dating and thermal models. We predict their formation locations, finding
excellent consistency with other location information (water content, asteroid
spectra and parent bodies). We predict the size of particle concentrated by
turbulence for each chondrite, finding excellent matches to each chondrites's
mean chondrule diameter. These consistencies imply meteorite parent bodies
assembled quickly from local materials concentrated by turbulence, and usually
did not migrate far. We predict CI chondrites are depleted in refractory
lithophile elements relative to the Sun, by about 12% (0.06 dex). We constrain
the variation of turbulence parameter $\alpha$ in the disk, and find a limited
role for magnetorotational instability, favoring hydrodynamical instabilities
in the outer disk, plus magnetic disk winds in the inner disk. Between 3 and 4
Myr at least, gas persisted outside Jupiter but was depleted inside it, and the
solar nebula was a transition disk.
