Abstract
Oxygen abundances are presented from LTE and non-LTE analyses of O II lines in spectra of 18 B mainsequence stars of the four subgroups comprising the Orion association. The lowest abundances are found in the oldest subgroups (Ia and Ib). The youngest subgroup Id, the Trapezium cluster, and some stars of the slightly older Ic subgroup seem to have an abundance that is up to about 40% higher. It is suggested that this enrichment resulted from the mixing of supernovae ejecta from the Ic subgroup with those adjacent portions of the dense molecular cloud that subsequently collapsed to form the Trapezium cluster
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