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The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities

Keszthelyi, Z; de Koter, A; Götberg, Y; Meynet, G; Brands, S A; Petit, V; Carrington, M; David-Uraz, A; Geen, S T; Georgy, C; Hirschi, R; Puls, J; Ramalatswa, K J; Shultz, M E; ud-Doula, A

The effects of surface fossil magnetic fields on massive star evolution: IV. Grids of models at Solar, LMC, and SMC metallicities Thumbnail


Z Keszthelyi

A de Koter

Y Götberg

G Meynet

S A Brands

V Petit

M Carrington

A David-Uraz

S T Geen

C Georgy

J Puls

K J Ramalatswa

M E Shultz

A ud-Doula


Magnetic fields can drastically change predictions of evolutionary models of massive stars via mass-loss quenching, magnetic braking, and efficient angular momentum transport, which we aim to quantify in this work. We use the MESA software instrument to compute an extensive main-sequence grid of stellar structure and evolution models, as well as isochrones, accounting for the effects attributed to a surface fossil magnetic field. The grid is densely populated in initial mass (3–60 M?), surface equatorial magnetic field strength (0–50 kG), and metallicity (representative of the Solar neighbourhood and the Magellanic Clouds). We use two magnetic braking and two chemical mixing schemes and compare the model predictions for slowly rotating, nitrogen-enriched (‘Group 2’) stars with observations in the Large Magellanic Cloud. We quantify a range of initial field strengths that allow for producing Group 2 stars and find that typical values (up to a few kG) lead to solutions. Between the subgrids, we find notable departures in surface abundances and evolutionary paths. In our magnetic models, chemical mixing is always less efficient compared to non-magnetic models due to the rapid spin-down. We identify that quasi-chemically homogeneous main sequence evolution by efficient mixing could be prevented by fossil magnetic fields. We recommend comparing this grid of evolutionary models with spectropolarimetric and spectroscopic observations with the goals of (i) revisiting the derived stellar parameters of known magnetic stars, and (ii) observationally constraining the uncertain magnetic braking and chemical mixing schemes.

Journal Article Type Article
Acceptance Date Sep 9, 2022
Online Publication Date Sep 15, 2022
Publication Date 2022-12
Publicly Available Date May 30, 2023
Journal Monthly Notices of the Royal Astronomical Society
Print ISSN 0035-8711
Publisher Oxford University Press
Peer Reviewed Peer Reviewed
Volume 517
Issue 2
Pages 2028 - 2055
Keywords stars: abundances, stars: evolution, stars: magnetic field, stars: massive, stars: rotation
Publisher URL


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