# Rotation and Magnetism of Massive Stellar Cores

## TL;DR

This paper investigates the internal rotation and magnetic field evolution of massive stars, linking core dynamics to neutron star and black hole properties, with implications for magnetic field strength and binary interactions.

## Contribution

It presents new models of stellar core rotation and magnetism, highlighting the impact of convective layers and binary interactions on remnant spin and magnetic fields.

## Key findings

- Neutron star spin periods vary from 0.1 to 2 ms depending on stellar mass.
- Stronger inward angular momentum pumping occurs in more massive stars.
- Binary interactions can significantly spin up black hole remnants.

## Abstract

The internal rotation and magnetism of evolved massive stars are considered in response to i) the inward pumping of angular momentum through deep and slowly rotating convective layers; and ii) the winding up of a helical magnetic field in radiative layers. Field winding can transport angular momentum effectively even when the toroidal field is limited by kinking. Magnetic helicity is pumped into a growing radiative layer from an adjacent convective envelope (or core). The receding convective envelope that forms during the early accretion phase of a massive star is the dominant source of helicity in its core, yielding a $\sim 10^{13}$ G polar magnetic field in a collapsed neutron star (NS) remnant. Using MESA models of various masses, we find that the NS rotation varies significantly, from $P_{\rm NS} \sim 0.1-1$ s in a 13$\,M_\odot$ model to $P_{\rm NS} \sim 2$ ms in a $25\,M_\odot$ model with an extended core. Stronger inward pumping of angular momentum is found in more massive stars, due to the growing thickness of the convective shells that form during the later stages of thermonuclear burning. On the other hand, stars that lose enough mass to form blue supergiants in isolation end up as very slow rotators. The tidal spin-up of a 40$\,M_\odot$ star by a massive binary companion is found to dramatically increase the spin of the remnant black hole, allowing a rotationally supported torus to form during the collapse. The implications for post-collapse decay or amplification of the magnetic field are also considered.