Remnant masses and explodability of core-collapse supernovae at different metallicities: a theoretical model to predict explosion properties

The explodability of core-collapse supernovae is still a highly debated topic. Determining which stars explode and which ones do not requires reliable simulations and a model to connect the pre-supernova stellar structure to the explosion dynamics. In this talk, I will show the explodability of stars with a ZAMS mass of 9-120 solar masses at three different metallicities, and compare their remnant masses and explosion energies to observations. I will then present a robust model to predict both the explodability and the remnant masses of massive stars, based on the pre-supernova stellar structure. This model depends on the magnitude of the density jump at the Si/O interface. I will quantitatively explain why this interface plays such an important role by interpreting its accretion through the shock using a semi-analytical model.