  We explore heavy element nucleosynthesis in the explosion of massive stars
which are triggered by a quark-hadron phase transition during the early post
bounce phase of core-collapse supernovae. The present study is based on general
relativistic radiation hydrodynamics simulations with three-flavor Boltzmann
neutrino transport in spherical symmetry, which utilize a quark-hadron hybrid
equation of state based on the MIT bag model for strange quark matter. The
quark-hadron phase transition inside the stellar core forms a shock wave
propagating towards the surface of the proto-neutron star. The shock wave
results in an explosion and ejects neutron-rich matter which is piled up or
accreting on the proto-neutron star. Later, during the cooling phase, the
proto-neutron star develops a proton-rich neutrino-driven wind. We present a
detailed analysis of the nucleosynthesis outcome in both neutron-rich and
proton-rich ejecta and compare our integrated nucleosynthesis with observations
of metal poor stars.
