\begin{center}{\Large\bf 
The evolution of magnetic hot massive stars: Implementation of the quantitative influence of surface magnetic fields in modern models of stellar evolution}\end{center} 

\centerline{\bf Zsolt Keszthelyi [1,2], Gregg A. Wade [1], Veronique Petit [3,4]
}{\footnotesize [1] Royal Military College of Canada
[2] Queen's University 
[3] Florida Institute of Technology
[4] University of Delaware
}
 
Large-scale dipolar surface magnetic fields have been detected in a fraction of OB stars, however only few stellar evolution models of massive stars have considered the impact of these fossil fields. We are performing 1D hydrodynamical model calculations taking into account evolutionary consequences of the magnetospheric-wind interactions in a simplified parametric way. Two effects are considered: i) the global mass-loss rates are reduced due to mass-loss quenching, and ii) the surface angular momentum loss is enhanced due to magnetic braking. As a result of the magnetic mass-loss quenching, the mass of magnetic massive stars remains close to their initial masses. Thus magnetic massive stars - even at Galactic metallicity - have the potential to be progenitors of `heavy' stellar mass black holes. Similarly, at Galactic metallicity, the formation of pair instability supernovae is plausible with a magnetic progenitor.

{\bf Reference: to appear in Proceedings of IAUS 329} \\{\it Status:} Conference proceedings
 \\ {\it Comments:} 

{\it On the web at:} {\tt https://arxiv.org/abs/1702.04460} 

{\it Preprints from:} {\tt  zsolt.keszthelyi@rmc.ca} 
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