Solar coronal heating through magnetic reconnection

该项目的总体目标是通过研究磁通管重连过程中磁能释放的本质，帮助了解太阳耀斑如何释放能量并加速带电粒子。重点将放在通过扭曲磁通绳合并释放存储磁能的配置上。最初的工作将集中在模拟2D强制重连接中的测试粒子，扩展之前的工作，包括岛（通量绳）合并。为了实现这一目标，将使用磁流体动力学模拟来研究日冕中强制磁重联事件期间磁场的演变。这些结果将用于使用CGA代码的测试粒子模拟，以确定太阳日冕中某些粒子群加速到高能的机制。在先前不稳定的扭曲日冕环工作的基础上，将考虑更复杂的磁场结构，如多线程和多环路相互作用。此外，还可以将测试粒子动力学模型扩展到更自洽的动力学模型，并研究将该模型应用于聚变等离子体的可能性。

The overall aim of the project is to contribute to understanding how the solar flares release energy and accelerate charged particles, by studying the nature of magnetic energy release during magnetic flux tube reconnection. The focus will be on configurations which release stored magnetic energy trhough merger of twisted magnetic flux ropes. Initial work will focus on modelling test partices in 2D forced reconnection, extending previous work to include island (flux rope) merger. In order to achieve this, the evolution of the magnetic field during forced magnetic reconnection events in the corona will be investigated using magnetohydrodynamic simulations. These results will be used in test-particle simulations using the CGA code to determine the mechanisms by which some particle populations in the solar corona are accelerated to high energies. Building on previous work in unstable twisted coronal loops, more complex magnetic field configurations will then be considered, such as multi-thread and multi-loop interactions. There is also scope to extend the test-particle kinetic model to more self consistent kinetic models, as well as looking at possible applications of the modelling to fusion plasmas.