Speaker
Description
Predicting whether a core-collapse supernova (CCSN) will successfully explode remains a central challenge in astrophysics. While many physical parameters influence the explosion outcome, recent studies have highlighted the structure of the silicon-oxygen (Si/O) interface as a potentially decisive factor in shock revival. In this work, I investigate the role of the Si/O interface by systematically modifying a set of progenitor models to produce a broad range of density gradients at the interface, while keeping all other physical properties fixed. This controlled approach allows us to isolate and better understand the influence of the interface's steepness and structure on the explosion dynamics. By analyzing the outcomes of these modified progenitors in numerical simulations, we aim to determine whether the Si/O interface is indeed a critical ingredient in triggering successful CCSN explosions.
