Detection of a centrifugal magnetosphere in one of the most massive stars in the ρOph star-forming cloud

被引：1
|
作者：
Hubrig, S. [1 ]
Schoeller, M. [2 ]
Jaervinen, S. P. [1 ]
Kueker, M. [1 ]
Kholtygin, A. F. [3 ]
Steinbrunner, P. [4 ]
机构：
[1] Leibniz Inst Astrophys Potsdam AIP, Sternwarte 16, D-14482 Potsdam, Germany
[2] European Southern Observ, Garching, Germany
[3] St Petersburg State Univ, Astron Inst, St Petersburg, Russia
[4] Free Univ Berlin, Berlin, Germany
来源：
ASTRONOMISCHE NACHRICHTEN | 2018年 / 339卷 / 01期
关键词：
stars: early-type; stars: formation; stars: individual: Oph A; stars: magnetic field; stars: variables: general; stars: X-rays; DRIVEN STELLAR WINDS; X-RAY-EMISSION; DYNAMICAL SIMULATIONS; MAGNETIC-FIELDS; ROAP STARS; O-STARS; OPHIUCHI; VARIABILITY; FORS-1; MODEL;
D O I：
10.1002/asna.201713457
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
Recent XMM-Newton observations of the B2 type star Oph A indicated a periodicity of 1.205 day, which was ascribed to rotational modulation. Since variability of X-ray emission in massive stars is frequently the signature of a magnetic field, we investigated whether the presence of a magnetic field can indeed be invoked to explain the observed X-ray peculiarity. Two FORS 2 spectropolarimetric observations in different rotation phases revealed the presence of a negative (B-zall = - 419 +/- 101 G) and positive (B-zall = 538 +/- 69 G) longitudinal magnetic field, respectively. We estimate a lower limit for the dipole strength as B-d = 1.9 +/- 0.2 kG. Our calculations of the Kepler and Alfven radii imply the presence of a centrifugally supported, magnetically confined plasma around Oph A. The study of the spectral variability indicates a behavior similar to that observed in typical magnetic early-type Bp stars.
引用
收藏
页码：72 / 77
页数：6
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