论文标题
主序列B Star HD 43317中近核磁场强度的小催化性推断
Asteroseismic inference of the near-core magnetic field strength in the main sequence B star HD 43317
论文作者
论文摘要
观察到大约10％的中间和高质量矮人恒星在其表面上占有强大的大规模磁场，被认为是化石场的起源。但是，关于恒星深处内部内部磁场强度和几何形状的推断很少。考虑到巨大的恒星具有对流核心，而在主序列上，重力（G）模式的Asterosesology能够在其核心质量上提供约束，但到目前为止，它尚未用于探测其内部磁场的强度。在这里，我们基于磁场的预期相互作用及其G模式，在这里使用Asterosology来限制脉动和磁性B星HD 43317的近核区域的上限。我们发现订单的磁场强度$ 5 \ times 10^5 $ g足以抑制高radial阶G模式并重现仅包含高频G模式的HD 43317的观察到的频谱。该结果是主序列内磁场强度的首次推断。
About 10 per cent of intermediate- and high-mass dwarf stars are observed to host a strong large-scale magnetic field at their surface, which is thought to be of fossil field origin. However, there are few inferences as to the magnetic field strength and geometry within the deep interiors of stars. Considering that massive stars harbour a convective core whilst on the main sequence, asteroseismology of gravity (g) modes is able to provide constraints on their core masses, yet it has so far not been used to probe the strength of their interior magnetic fields. Here we use asteroseismology to constrain an upper limit for the magnetic field strength in the near-core region of the pulsating and magnetic B star HD 43317, based on the expected interaction of a magnetic field and its g modes. We find a magnetic field strength of order $5 \times 10^5$ G is sufficient to suppress high-radial order g modes and reproduce the observed frequency spectrum of HD 43317, which contains only high-frequency g modes. This result is the first inference of the magnetic field strength inside a main-sequence star.
