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Magnetic fields and internal mixing of main sequence B stars

Published online by Cambridge University Press:  23 January 2015

G. A. Wade ,
C. P. Folsom ,
J. Grunhut ,
J. D. Landstreet  and
V. Petit
G. A. Wade
Affiliation:
RMC, Canada
C. P. Folsom
Affiliation:
IRAP, France
J. Grunhut
Affiliation:
ESO, Germany
J. D. Landstreet
Affiliation:
UWO, Canada Armagh, U.K.
V. Petit
Affiliation:
U. Delaware, USA
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Abstract

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We have obtained high-quality magnetic field measurements of 19 sharp-lined B-type stars with precisely-measured N/C abundance ratios (Nieva & Przybilla 2012). Our primary goal is to test the idea (Meynet et al. 2011) that a magnetic field may explain extra drag (through the wind) on the surface rotation, thus producing more internal shear and mixing, and thus could provide an explanation for the appearance of slowly rotating N-rich main sequence B stars.

Keywords

stars: abundancesstars: early-typestars: evolutionstars: magnetic fields
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 9 , Issue S307: New windows on massive stars: asteroseismology, interferometry, and spectropolarimetry , June 2014 , pp. 401 - 403
Copyright
Copyright © International Astronomical Union 2015 

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