Magnetic fields and internal mixing of main sequence B stars

被引：1
|
作者：
Wade, G. A. [1 ]
Folsom, C. P. [2 ]
Grunhut, J. [3 ]
Landstreet, J. D. [4 ]
Petit, V [5 ]
机构：
[1] RMC, Kingston, ON, Canada
[2] IRAP, Toulouse, France
[3] ESO, Garching, Germany
[4] Univ Western Ontario, London, ON, Canada
[5] Univ Delaware, Newark, DE 19716 USA
来源：
NEW WINDOWS ON MASSIVE STARS: ASTEROSEISMOLOGY, INTERFEROMETRY AND SPECTROPOLARIMETRY | 2014年 / 307卷
关键词：
stars: abundances; stars: early-type; stars: evolution; stars: magnetic fields; NITROGEN;
D O I：
10.1017/S1743921314007273
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
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.
引用
收藏
页码：401 / 403
页数：3
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