Abstract
The new observational [O/Fe] vs [Fe/H] relationship in halo dwarfs is analyzed in terms of a model of chemical evolution for the solar neighbourhood. The role of nucleosynthesis prescriptions for SN II and SN I (both Ia and Ib) is analyzed. We show that by adopting iron yields for SN II according to the observations of SN 1987A and by assuming double degenerate systems to be the progenitors of SN Ia and Wolf-Rayet stars to be the progenitors of SN Ib, it is possible to reproduce quite well the behaviour of the [O/Fe] ratio for halo and disk stars. Nevertheless, best agreement is obtained when introducing in addition a variable IMF during the halo evolution.
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