Experimental Simulation of Solar Flares

由于磁场释放的自由能，热的磁化等离子体结构往往表现出非常复杂的动力学行为。一个著名的例子是太阳双折射，在一个长时间的准稳定阶段之后，经常会导致壮观的爆发，如日冕物质抛射（CME），沿着着复杂的三维和时间依赖的磁场和接近阿尔文速度的等离子体流速。本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，将以协调一致的方式进行实验室等离子体放电和数值MHD模拟实验。这种结合的策略将开启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特性的影响的可能性，并反过来得出解释太阳观测的结论。

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.