Is the wind of the Oe star HD 155806 magnetically confined?

被引：0
|
作者：
Petit, Veronique [1 ]
Fullerton, A. W. [2 ]
Bagnulo, S. [3 ]
Wade, G. A. [4 ]
机构：
[1] Univ Laval, Dept Phys, Quebec City, PQ G1K 7P4, Canada
[2] Space Telescope Sci Inst, Baltimore, MD USA
[3] Armagh Observ, Armagh, North Ireland
[4] Royal Mil Coll Canada, Dept Phys, Kingston, ON, Canada
来源：
COSMIC MAGNETIC FIELDS: FROM PLANETS, TO STARS AND GALAXIES | 2009年 / 259期
关键词：
Stars: magnetic fields; stars: mass loss; stars: early-type; stars: emission-line; MASSIVE STARS; FIELD;
D O I：
10.1017/S1743921309030786
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Oe stars are a subset of the O-type stars that exhibit emission lilies from a circumstellar disk. The recent; detection of magnetic fields in some O-type stars suggests a possible explanation for the stability of disk-like structures around Oe stars. According to this hypothesis, the wind of the star is channeled by a, dipolar magnetic field producing a disc in the magnetic equatorial plane. As a test, of this model, we have obtained spectropolarimetric observations of the hottest Galactic Oe star HD 155806. Here we discuss its results and implications.
引用
收藏
页码：385 / +
页数：2
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