Experimental Simulation of Solar Flares

由于磁场释放的自由能，热的磁化等离子体构型通常表现出非常复杂的动力学行为。一个众所周知的例子是日冕，在经历了长时间的准静止阶段后，通常会导致壮观的喷发，如日冕物质抛射(CMES)，伴随着复杂的三维和随时间变化的磁场和接近阿尔芬速度的等离子体流速度。这个项目的目的是通过研究一类模型构型的稳定性和动力学行为来更好地理解这类事件。为此，实验室等离子体放电实验和MHD数值模拟将以一致的方式进行。这一组合策略将为研究初始磁场几何形状等参数对磁稳定性和由此产生的动力学性质的影响提供了可能性，并反过来为解释太阳观测得出结论。

Hot, magnetized plasma configurations often exhibit a very complex dynamical behavior due to free energy released from the magnetic field. One well-known example are Solar prominences which, after a long-lasting quasi-stationary phase, often result in spectacular eruptions like Coronal mass ejections (CMEs) that come along with intricate three-dimensional and time-dependent magnetic fields and plasma flow velocities close to the Alfvén velocity. The aim of this project is to achieve a better understanding of such events by studying the stability and dynamical behavior of a class of model configurations. To this end, experiments on a laboratory plasma discharge and numerical MHD simulations will be carried out in a concerted manner. This combined strategy will then open the possibility to investigate the influence of parameters like the initial magnetic field geometry on magnetic stability and on properties of the resulting dynamics, and, in turn, to draw conclusions for the interpretation of Solar observations.