Observational Aspects of Particle Acceleration in Large Solar Flares

被引：0
|
作者：
John C. Raymond
Säm Krucker
Robert P. Lin
Vahé Petrosian
机构：
[1] Center for Astrophysics,Space Sciences Laboratory
[2] University of California,Institute for 4D Technologies, School of Engineering
[3] University of Applied Sciences North Western Switzerland,School of Space Research
[4] Kyung Hee University,Department of Applied Physics
[5] Stanford University,undefined
来源：
Space Science Reviews | 2012年 / 173卷
关键词：
Solar physics: flares; Solar physics: magnetic reconnection;
D O I：
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中图分类号：
学科分类号：
摘要：
Solar flares efficiently accelerate electrons to several tens of MeV and ions to 10 GeV. The acceleration is usually thought to be associated with magnetic reconnection occurring high in the corona, though a shock produced by the Coronal Mass Ejection (CME) associated with a flare can also accelerate particles. Diagnostic information comes from emission at the acceleration site, direct observations of Solar Energetic Particles (SEPs), and emission at radio wavelengths by escaping particles, but mostly from emission from the chromosphere produced when the energetic particles bombard the footpoints magnetically connected to the acceleration region. This paper provides a review of observations that bear upon the acceleration mechanism.
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页码：197 / 221
页数：24
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