Magnetic Instability and Energy Release in Solar Active Regions

该项目旨在了解日冕中自由能的积累、带电磁场的不稳定以及耀斑和物质抛射中自由能的快速释放。日冕磁能最终来自对流带的动能，但争论的焦点是，当磁场从光球喷发形成活动区时，磁场是否已经携带了自由能，自由能是从深对流区传播到日冕，还是喷发后光球足迹的运动对磁场产生了压力。研究人员将研究扭转沿非均匀通量管的传播。特别是，他们将确定位于光球层上方的水平通量管中扭结不稳定性的增长速度和特征。此外，他们还将研究电流片形成后磁能的释放。

This project aims to understand the accumulation of free energy in the solar corona, the destabilization of energized magnetic field, and the rapid release of free energy in flares and mass ejections. Coronal magnetic energy ultimately arises from kinetic energy of the convection zone, but the controversy is whether the magnetic fields already carry free energy when they erupt from the photosphere to form active regions, free energy propagates into the corona from the deep convection zone, or the fields are stressed by motions of their photospheric footprints after eruption. The investigators will examine the propagation of twist along a nonuniform flux tube. In particular, they will determine the growth rate and characteristics of the kink instability in a horizontal flux tube lying above the photosphere. In addition, they will investigate the release of magnetic energy subsequent to the formation of current sheets.