Recent accurate abundance analyses of B-type main sequence stars in the solar vicinity has show that abundances derived from these stellar objects are more homogeneous and metal-rich than previously thought.

We investigate wether the inhomogeneity of abundances previously found in B-type stars in the Ori OB1 association is real (and hence a signature of
enrichment of the newly formed stars in an induced star formation scenario) or a consequence of intrinsic errors induced by the use of photometric indices to establish the stellar parameters prior to the abundance analysis.

We obtain a new (improved) spectroscopic data-set comprising 13 B-type stars in the various Ori OB1 associations, and perform a detailed self-consistent spectroscopic abundance analysis by means of the modern stellar atmosphere code FASTWIND.

We detect systematic errors in the stellar parameters previously determined which affect the derived abundances. Once these errors are accounted for, we find a high degree of homogeneity of O and Si abundances for stars in the four Ori OB1 subgroups. The derived abundances are in very good agreement with recent determinations in other B-type stars in the solar vicinity. We also compare our results with those obtained for the Sun during the epoch of the "solar crisis", and the Orion nebula.