A Brief Review on Particle Acceleration in Multi-island Magnetic Reconnection

被引：7

作者：

Che, H. ^{[1
,2
]}

Zank, G. P.

机构：

[1] Univ Maryland, College Pk, MD 20742 USA

[2] NASA, Goddard Space Flight Ctr, Greenbelt, MD 20771 USA

来源：

18TH ANNUAL INTERNATIONAL ASTROPHYSICS CONFERENCE | 2019年 / 1332卷

关键词：

ELECTRON ACCELERATION; SOLAR-FLARES; COSMIC-RAYS; COALESCENCE; SPECTRA; SUBSTORMS; FIELD; MODEL; FLUX;

D O I：

10.1088/1742-6596/1332/1/012003

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

The basic physics and recent progresses in theoretical and particle-in-cell (PIC) simulation studies of particle acceleration in multi-island magnetic reconnection are briefly reviewed. Particle acceleration in multi-island magnetic reconnection is considered a plausible mechanism for the acceleration of energetic particles in solar flares and the solar wind. Theoretical studies have demonstrated that such a mechanism can produce the observed power-law energy distribution of energetic particles if the particle motion is sufficiently randomized in the reconnection event. However, PIC simulations seem to suggest that the first-order Fermi acceleration mechanism is unable to produce a power-law particle energy distribution function in mildly relativistic multi-island magnetic reconnections. On the other hand, while simulations of highly relativistic reconnections appear to be able to produce a power-law energy spectra, the spectral indices obtained are generally harder than the soft power-law spectra with indices similar to -5 commonly observed in the solar wind and solar flare events. In addition, the plasma heating due to kinetic instabilities in 3D magnetic reconnection may "thermalize" the power-law particles, making it even more difficult for multi-island reconnections to generate a power-law spectrum. We discuss the possible reasons that may lead to these problems.

引用

页数：11

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