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Cambridge University Press (CUP), Proceedings of the International Astronomical Union, S307(9), p. 401-403, 2014

DOI: 10.1017/s1743921314007273

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Magnetic fields and internal mixing of main sequence B stars

Journal article published in 2014 by G. A. Wade, C. P. Folsom, J. Grunhut, J. D. Landstreet ORCID, V. Petit
This paper was not found in any repository, but could be made available legally by the author.
This paper was not found in any repository, but could be made available legally by the author.

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Abstract

AbstractWe 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 (Meynetet 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.

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