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Recent accurate abundance analyses of B-type main sequence stars in the solarvicinity has shown that abundances derived from these stellar objects are morehomogeneous and metal-rich than previously thought. We investigate whether theinhomogeneity of abundances previously found in B-type stars in the Ori OB1association is real (hence a signature of enrichment of the newly formed starsin an induced star formation scenario) or a consequence of intrinsic errorsinduced by the use of photometric indices to establish the stellar parametersprior to the abundance analysis. We obtained a new (improved) spectroscopicdata set comprising 13 B-type stars in the various Ori OB1 associations, andperformed a detailed, self-consistent spectroscopic abundance analysis by meansof the modern stellar atmosphere code FASTWIND. We detect systematic errors inthe stellar parameters determined previously which affect the derivedabundances. Once these errors are accounted for, we find a high degree ofhomogeneity in the O and Si abundances for stars in the four Ori OB1 subgroups.The derived abundances are in very good agreement with recent determinations inother B-type stars in the solar vicinity. We also compare our results withthose obtained for the Sun during the epoch of the "solar crisis", and theOrion nebula.

The chemical composition of the Orion star forming region: I. Homogeneity of O and Si abundances in B-type stars