TY - JOUR
T1 - 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
AU - Keszthelyi, Z.
AU - Meynet, G.
AU - Shultz, M. E.
AU - David-Uraz, A.
AU - Ud-Doula, A.
AU - Townsend, R. H.D.
AU - Wade, G. A.
AU - Georgy, C.
AU - Petit, V.
AU - Owocki, S. P.
N1 - Funding Information:
We thank the anonymous referee for providing uswith a constructive and helpful report, which has led to improving the paper. We appreciate discussions with K. Augustson and P. Marchant. We are grateful for B. Paxton and the MESA developers for making their code publicly available. GM and CG acknowledge support from the Swiss National Science Foundation (project number 200020-172505). MES acknowledges support from the Annie Jump Cannon Fellowship, which supported by the University of Delaware and is endowed by the Mount Cuba Astronomical Observatory. AuD acknowledges support fromNASA through ChandraAward number TM7-18001X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. RHDT acknowledges support from National Science Foundation grants ACI-1663696 and AST-1716436. GAW acknowledges support in the form of a Discovery Grant from the Natural Science and Engineering Research Council (NSERC) of Canada. VP acknowledges support provided by (i) the National Aeronautics and Space Administration through Chandra Award Number GO3-14017A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060, and (ii) program HST-GO-13734.011-A that was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. ADU acknowledges support from NSERC.
Funding Information:
We thank the anonymous referee for providing us with a constructive and helpful report, which has led to improving the paper. We appreciate discussions with K. Augustson and P. Marchant. We are grateful for B. Paxton and the MESA developers for making their code publicly available. GM and CG acknowledge support from the Swiss National Science Foundation (project number 200020-172505). MES acknowledges support from the Annie Jump Cannon Fellowship, which supported by the University of Delaware and is endowed by the Mount Cuba Astronomical Observatory. AuD acknowledges support from NASA through Chandra Award number TM7-18001X issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of NASA under contract NAS8-03060. RHDT acknowledges support from National Science Foundation grants ACI-1663696 and AST-1716436. GAW acknowledges support in the form of a Discovery Grant from the Natural Science and Engineering Research Council (NSERC) of Canada. VP acknowledges support provided by (i) the National Aeronautics and Space Administration through Chandra Award Number GO3-14017A issued by the Chandra X-ray Observatory Center, which is operated by the Smithsonian Astrophysical Observatory for and on behalf of the National Aeronautics Space Administration under contract NAS8-03060, and (ii) program HST-GO-13734.011-A that was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-26555. ADU acknowledges support from NSERC.
Publisher Copyright:
© 2020 The Author(s).
PY - 2020/3/1
Y1 - 2020/3/1
N2 - The time evolution of angular momentum and surface rotation of massive stars are strongly influenced by fossilmagnetic fields viamagnetic braking.We present a new module containing a simple, comprehensive implementation of such a field at the surface of a massive star within theModules 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.
AB - The time evolution of angular momentum and surface rotation of massive stars are strongly influenced by fossilmagnetic fields viamagnetic braking.We present a new module containing a simple, comprehensive implementation of such a field at the surface of a massive star within theModules 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.
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U2 - 10.1093/mnras/staa237
DO - 10.1093/mnras/staa237
M3 - Article
AN - SCOPUS:85089568167
VL - 493
SP - 518
EP - 535
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
SN - 0035-8711
IS - 1
ER -