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

页码：385 / +

页数：2

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