Inhomogeneous stellar mixing in the final hours before the Cassiopeia A supernova

TL;DR

This paper presents observational evidence of a shell merger in a massive star's final hours before supernova, revealing rapid internal mixing that affects explosion asymmetry and remnant properties.

Contribution

It provides the first observational evidence that the last hours before a supernova involve inhomogeneous shell-merger mixing inside the star.

Findings

Detection of Ne-rich downflows and Si-rich upflows in the progenitor's interior.

Shell merger occurred within hours before collapse.

Final burning processes induce pre-supernova asymmetry.

Abstract

Understanding stars and their evolution is a key goal of astronomical research and has long been a focus of human interest. In recent years, theorists have paid much attention to the final interior processes within massive stars, as they can be essential for revealing neutrino-driven supernova mechanisms and other potential transients of massive star collapse. However, it is challenging to observe directly the last hours of a massive star before explosion, since it is the supernova event that triggers the start of intense observational study. Here we report evidence for a final phase of stellar activity known as a ``shell merger'', an intense shell burning in which the O-burning shell swallows its outer C-/Ne-burning shell, deep within the progenitor's interior moments before the supernova explosion. In the violent convective layer created by the shell merger, Ne, which is abundant in the stellar O-rich layer, is burned as it is pulled inward, and Si, which is synthesized inside, is transported outward. The remnant still preserves some traces of such Ne-rich downflows and Si-rich upflows in the O-rich layer, suggesting that inhomogeneous shell-merger mixing began just hours ($\lesssim 10^4$ s) before its gravitational collapse. Our results provide the first observational evidence that the final stellar burning process rapidly alters the internal structure, leaving a pre-supernova asymmetry. This breaking of spherical symmetry facilitates the explosion of massive stars and influences various supernova and remnant characteristics, including explosion asymmetries and the neutron star's kick and spin.