Magnetohydrostatic modeling of the solar atmosphere

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 beta 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 beta. 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.

Automated summary

Understanding the structure and evolution of magnetic fields and plasma in different layers of the Sun is crucial. While force-free magnetic fields are widely used for modeling the solar corona, a magnetohydrostatic equilibrium is more appropriate for the lower atmosphere due to the high plasma beta. This paper reviews analytical and numerical methods based on the magnetohydrostatic assumption for calculating magnetic fields and plasma in the solar atmosphere from measured magnetograms.