脉冲星观测的日冕磁场
The Magnetic Field of the Solar Corona from Pulsar Observations
摘要：
我们提出了一个新的实验与独立测量的电子密度和太阳日冕的磁场的能力。我们实现这一点，通过测量的过量法拉第旋转由于传播的偏振发射从一些恒星通过太阳日冕的磁场。该方法通过脉冲信号和磁场的色散，通过法拉第旋转量，产生积分电子密度的独立测量。在原则上，这允许确定的综合磁场通过太阳日冕沿许多视线，而无需任何假设的电子密度分布。我们提出了一个检测的脉冲星J1801 $-$ 2304的旋转措施增加约160 \rad在0.95 $^\circ$从太阳盘中心的伸长率。这对应于沿着$> 393μ\mathrm{G}$的该视线的磁场强度的下限。积分电子密度测量的精确度不足限制了这一结果，但日冕等离子体模型的应用可以进一步将其限制在大约20 mG，沿着从太阳边缘经过2.5个太阳半径的路径。这与使用Wilcox太阳天文台发表的源表面模型的扩展获得的预测一致
英文摘要：
We present a novel experiment with the capacity to independently measure both the electron density and the magnetic field of the solar corona. We achieve this through measurement of the excess Faraday rotation due to propagation of the polarised emission from a number of pulsars through the magnetic field of the solar corona. This method yields independent measures of the integrated electron density, via dispersion of the pulsed signal and the magnetic field, via the amount of Faraday rotation. In principle this allows the determination of the integrated magnetic field through the solar corona along many lines of sight without any assumptions regarding the electron density distribution. We present a detection of an increase in the rotation measure of the pulsar J1801$-$2304 of approximately 160 \rad at an elongation of 0.95$^\circ$ from the centre of the solar disk. This corresponds to a lower limit of the magnetic field strength along this line of sight of $> 393μ\mathrm{G}$. The lack of precision in the integrated electron density measurement restricts this result to a limit, but application of coronal plasma models can further constrain this to approximately 20mG, along a path passing 2.5 solar radii from the solar limb. Which is consistent with predictions obtained using extensions to the Source Surface models published by Wilcox Solar Observatory
机构、总结、中文摘要均由AI分析而来，可能存在错误，请以论文正文为准。
