Particle acceleration in solar flares: observations versus numerical simulations

被引：9

作者：

Benz, A. O. ^{[1
]}

Grigis, P. C. ^{[1
]}

Battaglia, M. ^{[1
]}

机构：

[1] ETH, Inst Astron, CH-8092 Zurich, Switzerland

来源：

PLASMA PHYSICS AND CONTROLLED FUSION | 2006年 / 48卷 / 12B期

关键词：

D O I：

10.1088/0741-3335/48/12B/S12

中图分类号：

O35 [流体力学]; O53 [等离子体物理学];

学科分类号：

070204 ; 080103 ; 080704 ;

摘要：

Solar flares are generally agreed to be impulsive releases of magnetic energy. Reconnection in dilute plasma is the suggested trigger for the coronal phenomenon. It releases up to 10(26) J, accelerates up to 10(38) electrons and ions and must involve a volume that greatly exceeds the current sheet dimension. The Ramaty High-Energy Solar Spectroscopic Imager satellite can image a source in the corona that appears to contain the acceleration region and can separate it from other x-ray emissions. The new observations constrain the acceleration process by a quantitative relation between spectral index and flux. We present recent observational results and compare them with theoretical modelling by a stochastic process assuming transit-time damping of fast-mode waves, escape and replenishment. The observations can only be fitted if additional assumptions on trapping by an electric potential and

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收藏

页码：B115 / B121

页数：7

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