# The effects of surface fossil magnetic fields on massive star evolution: I. Magnetic field evolution, mass-loss quenching and magnetic braking

## TL;DR

This study investigates how evolving surface fossil magnetic fields influence the evolution, mass loss, and rotation of massive stars, revealing that magnetic effects significantly alter surface chemical enrichment and rotational properties.

## Contribution

It introduces models of 15 solar mass stars with evolving magnetic fields, incorporating magnetic braking and mass-loss quenching, to explore their impact on stellar evolution.

## Key findings

- Magnetic fields weaken over time but remain observable in later stages.
- Magnetic braking enhances internal mixing and surface nitrogen enrichment.
- Magnetic models reproduce observed properties of slow rotators with high nitrogen abundance.

## Abstract

Surface magnetic fields have a strong impact on stellar mass loss and rotation and, as a consequence, on the evolution of massive stars. In this work we study the influence of an evolving dipolar surface fossil magnetic field with an initial field strength of 4 kG on the characteristics of 15 M$_{\odot}$ solar metallicity models using the Geneva stellar evolution code. Non-rotating and rotating models considering two different scenarios for internal angular momentum transport are computed, including magnetic field evolution, mass-loss quenching, and magnetic braking. Magnetic field evolution results in weakening the initially strong magnetic field, however, in our models an observable magnetic field is still maintained as the star evolves towards the red supergiant phase. At the given initial mass of the models, mass-loss quenching is modest. Magnetic braking greatly enhances chemical element mixing if radial differential rotation is allowed for, on the other hand, the inclusion of surface magnetic fields yields a lower surface enrichment in the case of near solid-body rotation. Models including surface magnetic fields show notably different trends on the Hunter diagram (plotting nitrogen abundance vs $v \sin i$) compared to those that do not. The magnetic models agree qualitatively with the anomalous `Group 2 stars', showing slow surface rotation and high surface nitrogen enhancement on the main sequence.