Following the previous work that described how the magnetic compression proceeded via dynamic loop-loop interaction, we constructed a quantitative model of this process in the solar magnetized atmosphere, which realized that it is a process of volume shrinkage with nonuniform acceleration caused by Lorentz force. When adjacent emerging magnetic loops locally have different thermal and dynamic properties, a significant discrepancy between their translational motions driven by means of Lorentz force may arise, leading to the dynamic interaction. We used numerical and analytic methods for examining magnetic piston-driven wave to evaluate how much a single event of the interaction could increase temperature in the upper chromosphere. The model showed a possibility that a chromospheric plasma is heated by the single event to have transition region temperature, which is typically several tens of times higher than chromospheric temperature. The model also provided an insight into the formation height of the transition region.
Reference
Magara, T.
Journal of the Korean Astronomical Society, 57, 239
*Plasma is essentially discontinous because it is composed of particles which are discrete objects. When these particles collide with each other well enough to make a continuum approximation valid, the plasma is treated as continuous matter. On the other hand, magnetic field is a kind of "field" which is essentially continuous.
For the derivation of this result, see this page.
