Electron Acceleration during Macroscale Magnetic Reconnection
Electron Acceleration during Macroscale Magnetic Reconnection
复制标题
宏观磁重联过程中的电子加速
DOI：
10.1103/physrevlett.126.135101
复制
发表时间：
2021-03-30
影响因子：
8.6
通讯作者：
Shen, C.
中科院分区：
文献类型：
--
作者：
Arnold, H.;Drake, J. F.;Shen, C.
首次对宏观系统中磁重联过程中的电子加速进行了自洽模拟。与太阳耀斑的观测结果一致，高能电子的光谱呈幂律形式，其能量范围超过20年。这些非热电子的驱动机制是在增长和合并磁通绳费米反射。强的引导场通过削弱费米驱动机制来抑制非热电子的产生。对于弱的引导场，非热电子的总能量含量占主导地位的热热电子，即使他们的数量密度仍然很小。我们的结果以2017年9月10日X8.2级太阳耀斑的硬X射线，无线电和极紫外线观测为基准。
The first self-consistent simulations of electron acceleration during magnetic reconnection in a macroscale system are presented. Consistent with solar flare observations, the spectra of energetic electrons take the form of power laws that extend more than two decades in energy. The drive mechanism for these nonthermal electrons is Fermi reflection in growing and merging magnetic flux ropes. A strong guide field suppresses the production of nonthermal electrons by weakening the Fermi drive mechanism. For a weak guide field the total energy content of nonthermal electrons dominates that of the hot thermal electrons even though their number density remains small. Our results arc benchmarked with the hard x-ray, radio, and extreme ultraviolet observations of the X8.2-class solar flare on September 10, 2017.