论文标题
通过极端粉状光谱法在恒星冠的基部的磁场测量值的正向建模
Forward Modeling of Magnetic-field Measurements at the Bases of Stellar Coronae through Extreme-Ultraviolet Spectroscopy
论文作者
论文摘要
恒星冠状磁场的测量对于理解恒星磁活动至关重要，但是测量非常困难。最近的研究提出了一种基于Fe〜 {\ sc {x}}离子的磁场诱导 - 转变（MIT）的新方法测量方法。在这里，我们构建了一系列恒星冠状动脉水动力学（MHD）模型，并在极端硫化物质波长处合成了几个Fe〜 {\ sc {x}}发射线，然后使用MIT技术诊断冠状动脉底部的磁场强度。我们的结果表明，该技术可以应用于一些磁场的恒星，其最大太阳能是太阳的三倍以上。此外，我们研究了由光子计数误差引起的衍生磁场强度的不确定性，并发现Fe〜 {\ sc {x}} 175Å〜线的信号噪声比为$ \ sim $ 50，以实现有效的恒星冠状磁场的测量。
Measurements of the stellar coronal magnetic field are of great importance in understanding the stellar magnetic activity, yet the measurements have been extremely difficult. Recent studies proposed a new method of magnetic field measurements based on the magnetic-field-induced-transition (MIT) of the Fe~{\sc{x}} ion. Here we construct a series of stellar coronal magnetohydrodynamics (MHD) models and synthesize several Fe~{\sc{x}} emission lines at extreme-ultraviolet wavelengths, and then diagnose the magnetic field strength at the bases of the coronae using the MIT technique. Our results show that the technique can be applied to some stars with magnetic fields more than three times higher than that of the Sun at solar maximum. Furthermore, we investigate the uncertainty of the derived magnetic field strength caused by photon counting error and find that a signal-noise ratio of $\sim$50 for the Fe~{\sc{x}} 175 Å~line is required to achieve effective measurements of the stellar coronal magnetic field.
