Hard X-ray footpoint motions in solar flares: Comparing magnetic reconnection models with observations

被引：56

作者：

Krucker, S ^{[1
]}

Fivian, MD ^{[1
]}

Lin, RP ^{[1
]}

机构：

[1] Univ Calif Berkeley, Space Sci Lab, Berkeley, CA 94720 USA

来源：

ENERGY RELEASE AND PARTICLE ACCELERATION AT THE SUN AND IN THE HELIOSPHERE | 2005年 / 35卷 / 10期

关键词：

solar flares; solar X-ray emission; magnetic reconnection; particle acceleration;

D O I：

10.1016/j.asr.2005.05.054

中图分类号：

V [航空、航天];

学科分类号：

08 ; 0825 ;

摘要：

Hard X-ray observations from the Reuven Ramaty High Energy Solar Spectroscopic Imager (RHESSI) of the October 29, 2003 GOES X10 two-ribbon flare are used together with magnetic field observations from the Michelson Doppler Imager (MDI) onboard SoHO to compare footpoint motions with predictions from magnetic reconnection. models. The temporal variations of the velocity v of the hard X-ray footpoint motions and the photospheric magnetic field strength B in footpoints are investigated. The underlying photospheric magnetic field strength is generally higher (B similar to 700-1200 G) in the slower moving (v similar to 20-50 km s(-1)) western footpoint than in the faster (v similar to 20-100 km s(-1)) moving eastern source (similar to 100-600 G). Furthermore, a rough temporal correlation between the HXR flux and the product vB(2) is observed. (c) 2005 COSPAR. Published by Elsevier Ltd. All rights reserved.

引用

页码：1707 / 1711

页数：5

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