  Solid material in a protoplanetary nebula is subject to vigorous
redistribution processes relative to the nebula gas. Meter-sized particles
drift rapidly inwards near the nebula midplane, and material evaporates when
the particles cross a condensation/evaporation boundary. The material cannot be
removed as fast in its vapor form as it is being supplied in solid form, so its
concentration increases locally by a large factor (more than an order of
magnitude under nominal conditions). As time goes on, the vapor phase
enhancement propagates for long distances inside the evaporation boundary
(potentially all the way in to the star). Meanwhile, material is enhanced in
its solid form over a characteristic lengthscale outside the evaporation
boundary. This effect is applicable to any condensible (water, silicates, {\it
etc.}). Three distinct radial enhancement/depletion regimes can be discerned by
use of a simple model. Meteoritics applications include oxygen fugacity and
isotopic variations, as well as isotopic homogenization in silicates. Planetary
system applications include more robust enhancement of solids in Jupiter's core
formation region than previously suggested. Astrophysical applications include
differential, time-dependent enhancement of vapor phase CO and H$_2$O in the
terrestrial planet regions of actively accreting protoplanetary disks.
