Effect of the nuclear Equation of State on the Core-Collapse Supernovae explosion

Massive stars end their lives when their core collapses under the influence of gravity. In some cases, the collapse results in a bright and spectacular event forming a core-collapse supernova (CCSN). At other times the star fails to explode and eventually becomes a black hole. The equation of state (EOS) of dense nuclear matter plays an important role in determining the final fate of the star. We can see differences in the neutrino luminosities produced in a CCSN event for different EOS. Here, we investigate the impact of different EOS on the explosion properties and the nucleosynthesis yields. We model the simulation using the parametrized spherically symmetric explosion method PUSH which includes general-relativistic hydrodynamics and neutrino transport. We use eight different supernovae EOS and study the variation in explosion properties and nucleosynthesis yields for stars with different masses and metallicities. We find that the explosion outcome changes drastically depending on the EOS. In this talk, I will discuss the reasons for such alteration in the explosion outcome. I will also discuss how the nuclear EOS impacts nucleosynthesis yields and the remnant mass distribution.