Magnetohydrostatic modeling of the solar atmosphere  

作　　者：ZHU XiaoShuai NEUKIRCH Thomas WIEGELMANN Thomas 

机构地区：[1]State Key Laboratory of Space Weather,National Space Science Center,Chinese Academy of Sciences,Beijing 100190,China [2]National Astronomical Observatories,Chinese Academy of Sciences,Beijing 100101,China [3]School of Mathematics and Statistics,University of St Andrews,St Andrews KY169SS,UK [4]Max-Planck-Institut f¨ur Sonnensystemforschung,G¨ottingen 37077,Germany

出　　处：《Science China(Technological Sciences)》2022年第8期1710-1726,共17页中国科学（技术科学英文版）

基　　金：the National Key R&D Program of China (Grant No. 2021YFA1600500) and mobility program (Grant No. M-0068) of the Sino-German Science Center;financial support by the UKs Science and Technology Facilities Council (STFC) (Grant Nos. ST/S000402/1 and ST/W001195/1) financial support by DLR-grant 50 OC 2101。

摘　　要：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.

关 键 词：magnetic field photosphere CHROMOSPHERE CORONA 

分 类 号：P353.7[天文地球—空间物理学]