The strong magnetic field of the large-amplitude β Cephei pulsator V1449 Aquilae
The strong magnetic field of the large-amplitude β Cephei pulsator V1449 Aquilae
复制标题
大振幅β仙王波轮V1449 Aquilae的强磁场
DOI：
10.1051/0004-6361/201117261
复制
发表时间：
2011
影响因子：
6.5
通讯作者：
T. Morel
中科院分区：
文献类型：
--
作者：
S. Hubrig;I. Ilyin;M. Briquet;M. Briquet;M. Schöller;J. F. González;N. Nuñez;P. Cat;T. Morel
目标。只有极少数的仙王座β星在自转周期内的磁场行为被研究过。在过去的两年里，我们利用北欧光学望远镜的 SOFIN 获得了仙王座 β 星 V1449 Aql 的多历元极化光谱，以寻找旋转周期并约束磁场的几何形状。方法。平均纵向磁场是在 13 个不同历元测量的。新的测量结果与之前的 FORS 1 测量结果一起用于频率分析和磁场表征。结果。 V1449 Aql是迄今为止仙王座β星中最强的纵向磁场，高达700 G。生成的周期图显示了三个主峰，其中最高峰位于 f = 0.0720 d −1 处，对应于周期 P = 13. d 893。磁场几何形状很可能可以用极地磁场强度 Bd 约为 3 kG 且磁轴与旋转轴的倾斜角 β 为 76 ± 4 ° 的中心偶极子来描述。截至目前，最强的纵向磁场是在仙王座β星V1449 Aql和Σ 1 CMa中检测到的，具有较大的径向速度振幅。它们的峰峰值幅度分别达到~90 km s -1 和~33 km s -1 。最后，我们简单讨论一下目前已知的八颗磁性β仙王星的位置
Aims. Only for very few β Cephei stars has the behaviour of the magnetic field been studied over the rotation cycle. During the past two years we have obtained multi-epoch polarimetric spectra of the β Cephei star V1449 Aql with SOFIN at the Nordic Optical Telescope to search for a rotation period and to constrain the geometry of the magnetic field. Methods. The mean longitudinal magnetic field is measured at 13 different epochs. The new measurements, together with the previous FORS 1 measurements, have been used for the frequency analysis and the characterization of the magnetic field. Results. V1449 Aql so far possesses the strongest longitudinal magnetic field of up to 700 G among the β Cephei stars. The resulting periodogram displays three dominant peaks with the highest peak at f = 0.0720 d −1 corresponding to a period P = 13. d 893. The magnetic field geometry can likely be described by a centred dipole with a polar magnetic field strength Bd around 3 kG and an inclination angle β of the magnetic axis to the rotation axis of 76 ± 4 ◦ . As of today, the strongest longitudinal magnetic fields are detected in the β Cephei stars V1449 Aql and ξ 1 CMa with large radial velocity amplitudes. Their peak-to-peak amplitudes reach ∼90 km s −1 and ∼33 km s −1 , respectively. Concluding, we briefly discuss the position of the currently known eight magnetic β Cephei