Charged Particle Acceleration in Solar Eruptive Events

了解在太阳耀斑中观测到的大量非热加速粒子的产生机制是目前太阳物理学中最有趣的未解决问题之一。为太阳爆发事件提供动力的能量基本上来自日冕磁场，其释放涉及磁重联。磁重联过程中存在多种粒子加速机制。虽然磁重联过程中产生的平行电场是粒子加速的一个明显的潜在机制，但由于非理想重联区域的大小非常有限，它是否能解释观测到的高能粒子的数量存在一些疑问。与重联流出区有关的机制已经研究了几十年，到目前为止，在宏观尺度上的加速结果有些不确定，但最近在较小尺度上的操作得到了更多的关注。在这个博士项目中，将探索重连流出区粒子加速机制的各种以前未研究的方面。特别是，计划该项目将重点关注2D和3D模型之间的差异。该项目将主要使用测试粒子计算作为工具。该项目本质上主要是理论性的，但在可能的情况下，将与观测结果进行比较。

Understanding the mechanisms for the generation of the large number of non-thermal accelerated particles observed in solar flares is currently one of the most interesting unsolved problems in solar physics. The energy for powering solar eruptive events fundamentally comes from the coronal magnetic field and its release involves magnetic reconnection. A variety of particle acceleration mechanisms have been associated with the process of magnetic reconnection. While the parallel electric field generated during magnetic reconnection is an obvious potential mechanism for particle acceleration, there is some doubt whether it can account for the number of high-energy particles observed due to the very limited size of the non-ideal reconnection regions. Mechanisms linked to the reconnection outflow region have been studied for a couple of decades, so far with somewhat inconclusive results for acceleration on macroscopic scales, but have recently have gained more attention for operating on smaller scales. In this PhD project various previously unstudied aspects of particle acceleration mechanisms in reconnection outflow regions will be explored. In particular, it is planned that the project will focus on the differences between 2D and 3D models. The project will mainly use test particle calculations as a tool. The project is mainly theoretical in nature, but where possible comparison with observations will be made.