  Infrared observations provide the dust composition in the protoplanetary
discs surface layers, but can not probe the dust chemistry in the midplane,
where planet formation occurs. Meteorites show that dynamics was important in
determining the dust distribution in the Solar Nebula and needs to be
considered if we are to understand the global chemistry in discs. 1D radial
condensation sequences can only simulate one disc layer at a time and cannot
describe the global chemistry or the complexity of meteorites. To address these
limitations, we compute for the first time the two dimensional distribution of
condensates in the inner Solar Nebula using a thermodynamic equilibrium model,
and derive timescales for vertical settling and radial migration of dust.
  We find two enstatite-rich zones within 1 AU from the young Sun: a band ~0.1
AU thick in the upper optically-thin layer of the disc interior to 0.8 AU, and
in the optically-thick disc midplane out to ~0.4 AU. The two enstatite-rich
zones support recent evidence that Mercury and enstatite chondrites shared a
bulk material with similar composition. Our results are also consistent with
infrared observation of protoplanetary disc which show emission of
enstatite-rich dust in the inner surface of discs.
  The resulting chemistry and dynamics suggests that the formation of the bulk
material of enstatite chondrites occurred in the inner surface layer of the
disc, within 0.4~AU. We also propose a simple alternative scenario in which gas
fractionation and vertical settling of the condensates lead to an
enstatite-chondritic bulk material.
