The Three-Dimensional Collapse of a Rapidly Rotating 16 $M_{\odot}$ Star

TL;DR

This study presents the first 3D hydrodynamic simulations of a rapidly rotating 16 solar mass star's core-collapse, revealing how convective angular momentum transport influences the star's final collapse and remnant properties.

Contribution

It provides new insights into 3D angular momentum transport during core-collapse, highlighting its impact on stellar evolution and compact remnant characteristics.

Findings

Efficient 3D convective AM transport alters internal AM profiles.

AM distribution differences from 1D models affect neutron star/black hole spins.

3D simulations show significant impact on explosion outcomes.

Abstract

We report on the three-dimensional (3D) hydrodynamic evolution to iron core-collapse of a rapidly rotating 16 $M_{\odot}$ star. For the first time, we follow the 3D evolution of the angular momentum (AM) distribution in the iron core and convective shell burning regions for the final 10 minutes up to and including gravitational instability and core-collapse. In 3D, we find that convective regions show efficient AM transport that leads to an AM profile that differs in shape and magnitude from $\texttt{MESA}$ within a few shell convective turnover timescales. For different progenitor models, such as those with tightly coupled Si/O convective shells, efficient AM transport in 3D simulations could lead to a significantly different AM distribution in the stellar interior affecting estimates of the natal neutron star or black hole spin. Our results suggest that 3D AM transport in convective and rotating shell burning regions are critical components in models of massive stars and could qualitatively alter the explosion outcome and inferred compact remnant properties.