The rotational shear in pre-collapse cores of massive stars

TL;DR

This study models the rotational profiles of massive star cores before collapse, revealing large shear zones that could amplify magnetic fields and influence supernova explosion mechanisms.

Contribution

It provides detailed rotational profiles of pre-collapse cores considering various initial conditions, highlighting the potential for magnetic amplification and jet-driven explosions.

Findings

Large rotational shear zones near convective regions.

Inner core rotation insufficient for Keplerian disk formation.

Outer core and envelope retain significant angular momentum.

Abstract

We evolve stellar models to study the rotational profiles of the pre-explosion cores of single massive stars that are progenitors of core collapse supernovae (CCSNe), and find large rotational shear above the iron core that might play an important role in the jet feedback explosion mechanism by amplifying magnetic fields before and after collapse. Initial masses of 15 Mo and 30 Mo and various values of the initial rotation velocity are considered, as well as a reduced mass-loss rate along the evolution and the effect of core-envelope coupling through magnetic fields. We find that the rotation profiles just before core collapse differ between models, but share the following properties. (1) There are narrow zones of very large rotational shear adjacent to convective zones. (2) The rotation rate of the inner core is slower than required to form a Keplerian accretion disk. (3) The outer part of the core and the envelope have non-negligible specific angular momentum compared to the last stable orbit around a black hole (BH). Our results suggest the feasibility of magnetic field amplification which might aid a jet-driven explosion leaving behind a neutron star. Alternatively, if the inner core fails in exploding the star, an accretion disk from the outer parts of the core might form and lead to a jet-driven CCSN which leaves behind a BH.