Solar coronal heating through magnetic reconnection

该项目的总体目标是通过研究磁通量管重联期间磁能释放的性质，帮助了解太阳耀斑如何释放能量和加速带电粒子。重点将放在释放存储的磁能通过合并的扭曲磁通量绳的配置。初步工作将集中在模拟测试粒子在2D强制重联，扩展以前的工作，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。这些结果将用于测试粒子模拟使用CGA代码，以确定太阳日冕中的一些粒子群加速到高能量的机制。基于先前在不稳定扭曲日冕环中的工作，将考虑更复杂的磁场配置，例如多线程和多环相互作用。也有范围扩展测试粒子动力学模型，以更自我一致的动力学模型，以及在可能的应用程序的建模融合等离子体。

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.