Journal article
The effects of surface fossil magnetic fields on massive star evolution – II. Implementation of magnetic braking in mesa and implications for the evolution of surface rotation in OB stars
- Keszthelyi, Z ORCID Department of Physics, Engineering Physics and Astronomy, Queen’s University, 99 University Avenue, Kingston, ON K7L 3N6, Canada
- Meynet, G Geneva Observatory, University of Geneva, Maillettes 51, CH-1290 Sauverny, Switzerland
- Shultz, M E Department of Physics and Astronomy, University of Delaware, 217 Sharp Lab, Newark, DE 19716, USA
- David-Uraz, A ORCID Department of Physics and Astronomy, University of Delaware, 217 Sharp Lab, Newark, DE 19716, USA
- ud-Doula, A Department of Physics, Penn State Scranton, 120 Ridge View Drive, Dunmore, PA 18512, USA
- Townsend, R H D ORCID Department of Astronomy, University of Wisconsin-Madison, 475 N Charter St, Madison, WI 53706, USA
- Wade, G A Department of Physics and Space Science, Royal Military College of Canada, PO Box 1700, Station Forces, Kingston, ON K7K 0C6, Canada
- Georgy, C Geneva Observatory, University of Geneva, Maillettes 51, CH-1290 Sauverny, Switzerland
- Petit, V ORCID Department of Physics and Astronomy, University of Delaware, 217 Sharp Lab, Newark, DE 19716, USA
- Owocki, S P Department of Physics and Astronomy, University of Delaware, 217 Sharp Lab, Newark, DE 19716, USA
- 2020-1-25
Published in:
- Monthly Notices of the Royal Astronomical Society. - Oxford University Press (OUP). - 2020, vol. 493, no. 1, p. 518-535
English
ABSTRACT
The time evolution of angular momentum and surface rotation of massive stars are strongly influenced by fossil magnetic fields via magnetic braking. We present a new module containing a simple, comprehensive implementation of such a field at the surface of a massive star within the Modules for Experiments in Stellar Astrophysics (mesa) software instrument. We test two limiting scenarios for magnetic braking: distributing the angular momentum loss throughout the star in the first case, and restricting the angular momentum loss to a surface reservoir in the second case. We perform a systematic investigation of the rotational evolution using a grid of OB star models with surface magnetic fields (M⋆ = 5–60 M⊙, Ω/Ωcrit = 0.2–1.0, Bp = 1–20 kG). We then employ a representative grid of B-type star models (M⋆ = 5, 10, 15 M⊙, Ω/Ωcrit = 0.2, 0.5, 0.8, Bp = 1, 3, 10, 30 kG) to compare to the results of a recent self-consistent analysis of the sample of known magnetic B-type stars. We infer that magnetic massive stars arrive at the zero-age main sequence (ZAMS) with a range of rotation rates, rather than with one common value. In particular, some stars are required to have close-to-critical rotation at the ZAMS. However, magnetic braking yields surface rotation rates converging to a common low value, making it difficult to infer the initial rotation rates of evolved, slowly rotating stars.
- Language
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- English
- Open access status
- hybrid
- Identifiers
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- DOI 10.1093/mnras/staa237
- ISSN 0035-8711
- Persistent URL
- https://sonar.ch/global/documents/252700
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