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It has been recently proposed that the shocked surface layers of explodingO-Ne-Mg cores provide the conditions for r-process nucleosynthesis, becausetheir rapid expansion and high entropies enable heavy r-process isotopes toform even in an environment with very low initial neutron excess of the matter.We show here that the most sophisticated available hydrodynamic simulations (inspherical and axial symmetry) do not support this new r-process scenariobecause they fail to provide the necessary conditions of temperature, entropy,and expansion timescale by significant factors. This suggests that, either theformation of r-process elements works differently than suggested by Ning et al.(2007, NQM07), or that some essential core properties with influence on theexplosion dynamics might be different from those predicted by Nomoto'sprogenitor model.

Dynamics of shock propagation and nucleosynthesis conditions in O-Ne-Mg core supernovae