论文标题
太阳大气的磁液静态建模
Magnetohydrostatic Modeling of the Solar Atmosphere
论文作者
论文摘要
了解太阳多层的磁场和等离子体的结构和演变非常重要。由于低血浆$β$而导致的太阳电晕的准确近似的无力磁场已被广泛研究并用于对冠状磁性结构进行建模。尽管在太阳能电晕中可以很好地满足力的假设，但鉴于高血浆$β$，较低的大气并非没有力。因此，考虑到等离子体力（例如压力梯度和重力力），被认为更合适地描述较低大气的磁液压（MHS）平衡。本文根据MHS假设回顾了分析和数值外推法，用于从测得的磁图中计算太阳大气中的磁场和等离子体。
Understanding structures and evolutions of the magnetic fields and plasma in multiple layers on the Sun is very important. A force-free magnetic field which is an accurate approximation of the solar corona due to the low plasma $β$ has been widely studied and used to model the coronal magnetic structure. While the force-freeness assumption is well satisfied in the solar corona, the lower atmosphere is not force-free given the high plasma $β$. Therefore, a magnetohydrostatic (MHS) equilibrium which takes into account plasma forces, such as pressure gradient and gravitational force, is considered to be more appropriate to describe the lower atmosphere. This paper reviews both analytical and numerical extrapolation methods based on the MHS assumption for calculating the magnetic fields and plasma in the solar atmosphere from measured magnetograms.
