Signatures of magnetic reconnection in solar radio observations?

被引：4

作者：

Aurass, Henry ^{[1
]}

机构：

[1] Astrophys Inst Postsdam, D-14482 Potsdam, Germany

来源：

ADVANCES IN SPACE RESEARCH | 2007年 / 39卷 / 09期

关键词：

solar radio emission; magnetic fields; flares; CMEs;

D O I：

10.1016/j.asr.2007.01.058

中图分类号：

V [航空、航天];

学科分类号：

08 ; 0825 ;

摘要：

Magnetic reconnection occurs during eruptive processes (flares, CMEs) in the solar corona. This leads to a change of magnetic connectivity. Nonthermal electrons propagate along the coronal magnetic field thereby exciting dm- and m-wave radio burst emission after acceleration during reconnection or other energy release processes in heights of some Mm to >= 700 Mm. We summarize the results of some case studies which can be interpreted as radio evidence of magnetic reconnection: under certain conditions, simple spectral structures (pulsation pulses, reverse drift bursts) are formed by simultaneously acting but widely spaced radio sources. Narrowband spikes are emitted as a side-effect during large-scale coronal loop collisions. In dynamic radio spectra, the lower fast mode shock formed in the reconnection outflow appears as type II burst-like but nondrifting emission lane. It has been several times observed at the harmonic mode of the local plasma frequency between 250 and 500 MHz and at heights of approximate to 200 Mm. (C) 2007 COSPAR. Published by Elsevier Ltd. All rights reserved.

引用

页码：1407 / 1414

页数：8

共 37 条

[1]

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[2]

Aschwanden M J, 2002, Particle Acceleration and Kinematics in Solar Flares

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