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，通电磁场的不稳定性，以及耀斑和物质抛射中自由能的快速释放。 日冕的磁能最终来自对流带的动能，但争论的焦点是磁场是否已经携带自由能，当它们从光球爆发形成活动区时，自由能从深对流带传播到日冕，或者场在爆发后受到光球足迹运动的应力。 研究人员将研究扭曲沿着非均匀通量管的传播。 特别是，他们将确定增长率和扭结不稳定性的特点，在一个水平的通量管躺在上面的光球。 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.