Core-collapse supernovae simulations with reduced nucleosynthesis networks

We present core-collapse supernovae simulations including nuclear reaction networks which impact explosion dynamics and nucleosynthesis. The different composition treatment can lead to changes in the neutrino heating in the vicinity of the shock, by modifying the amount of nucleons and thus the $\mathrm{\nu}$-opacity of the region. This reduces the ram pressure outside the shock and allows an easier expansion. The energy released by the nuclear reactions during collapse also slows down the accretion, and aids the shock expansion. In addition, nuclear energy generation in the post-shocked matter produces more energetic explosions, up to $20\,\%$. Nucleosynthesis is affected due to the different dynamic evolution of the explosion. Our results indicate that the energy generation from nuclear reactions helps to sustain late outflows from the vicinity of the proto-neutron star (PNS), synthesizing more neutron-rich species. Furthermore, we show that there are systematic discrepancies between the ejecta calculated with in-situ and ex-situ reaction networks. The mass fractions of some Ca, Ti, Cr, and Fe isotopes are consistently under-produced in post-processing calculations, leading to different nucleosynthesis paths. Therefore, large in-situ nuclear reaction networks are needed for a more accurate nucleosynthesis.