Journal
MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 493, Issue 1, Pages 518-535Publisher
OXFORD UNIV PRESS
DOI: 10.1093/mnras/staa237
Keywords
stars: evolution; stars: magnetic field; stars: massive; stars: rotation
Categories
Funding
- Swiss National Science Foundation [200020172505]
- Annie Jump Cannon Fellowship
- University of Delaware
- NASA through ChandraAward [TM7-18001X]
- NASA [NAS8-03060, NAS 5-26555]
- National Science Foundation [ACI-1663696, AST-1716436]
- Natural Science and Engineering Research Council (NSERC) of Canada
- National Aeronautics and Space Administration through Chandra Award [GO3-14017A]
- NASA through Space Telescope Science Institute [NAS803060, HST-GO-13734.011-A]
- NSERC
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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-circle dot, Omega/Omega(crit) = 0.2-1.0, B-p = 1-20 kG). We then employ a representative grid of B-type star models (M-* = 5, 10, 15 M-circle dot, Omega/Omega(crit) = 0.2, 0.5, 0.8, B-p = 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.
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