  We present non-LTE oxygen abundances for a sample of B stars in the Orion
association. The abundance calculations included non-LTE line formation and
used fully blanketed non-LTE model atmospheres. The stellar parameters were the
same as adopted in the previous study by Cunha & Lambert (1994). We find that
the young Orion stars in this sample of 10 stars are described by a single
oxygen abundance with an average value of A(O)=8.78 and a small dispersion of
+/- 0.05 dex, which is of the order of the uncertainties in the analysis. This
average oxygen abundance compares well with the average oxygen abundance
obtained previously in Cunha & Lambert (1994): A(O) = 8.72 +/- 0.13 although
this earlier study, based upon non-blanketed model atmospheres in LTE,
displayed larger scatter. Small scatter of chemical abundances in Orion B stars
had also been found in our previous studies for neon and argon; all based on
the same effective temperature scale. The derived oxygen abundance distribution
for the Orion association compares well with other results for the oxygen
abundance in the solar neighborhood.
