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The time evolution of angular momentum and surface rotation of massive starsis strongly influenced by fossil magnetic fields via magnetic braking. Wepresent a new module containing a simple, comprehensive implementation of sucha field at the surface of a massive star within the Modules for Experiments inStellar Astrophysics (MESA) software instrument. We test two limiting scenariosfor magnetic braking: distributing the angular momentum loss throughout thestar in the first case, and restricting the angular momentum loss to a surfacereservoir in the second case. We perform a systematic investigation of therotational evolution using a grid of OB star models with surface magneticfields ($M_\star=5-60$ M$_\odot$, $\Omega/\Omega_{\rm crit} =0.2-1.0$, $B_{\rmp} =1-20$ kG). We then employ a representative grid of B-type star models($M_\star=5, 10, 15$ M$_\odot$, $\Omega/\Omega_{\rm crit} =0.2 , 0.5, 0.8$,$B_{\rm p} = 1, 3 ,10, 30$ kG) to compare to the results of a recentself-consistent analysis of the sample of known magnetic B-type stars. We inferthat magnetic massive stars arrive at the zero age main sequence with a rangeof rotation rates, rather than with one common value. In particular, some starsare required to have close-to-critical rotation at the ZAMS. However, magneticbraking yields surface rotation rates converging to a common low value, makingit difficult to infer the initial rotation rates of evolved, slowly-rotatingstars.

monthly notices of the royal astronomical society

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