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Effect of a Dipole Magnetic Field on Stellar Mass-Loss

Published online by Cambridge University Press:  28 July 2017

Chris Bard  and
Richard Townsend
Chris Bard
Affiliation:
NPP Fellow, NASA Goddard Space Flight Center 8800 Greenbelt Rd., Greenbelt, MD, USA email: [email protected]
Richard Townsend
Affiliation:
Dept. of Astronomy, University of Wisconsin-Madison, 475 N. Charter St., Madison, WI, USA email: [email protected]
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Abstract

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Massive star winds greatly influence the evolution of both their host star and local environment though their mass-loss rates, but current radiative line-driven wind models do not incorporate any magnetic effects. Recent surveys of O and B stars have found that about ten percent have large-scale, organized magnetic fields. These massive-star magnetic fields, which are thousands of times stronger than the Sun’s, affect the inherent properties of their own winds by changing the mass-loss rate. To quantify this, we present a simple surface mass-flux scaling over the stellar surface which can be easily integrated to get an estimate of the mass-loss rate for a magnetic massive star. The overall mass-loss rate is found to decrease by factors of 2-5 relative to the non-magnetic CAK mass-loss rate.

Keywords

stars: magnetic fieldsstars: winds, outflowsstars: mass-lossstars: early-type
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 12 , Symposium S329: The Lives and Death-Throes of Massive Stars , November 2016 , pp. 242 - 245
Copyright
Copyright © International Astronomical Union 2017 

References

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