Evolution of magnetic field structure and particle acceleration in solar flares

被引：7
|
作者：
Sakao, T
Kosugi, T
Masuda, S
Sato, J
机构：
[1] Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan
[2] Natl Astron Observ, Mitaka, Tokyo 1818588, Japan
[3] Nagoya Univ, Solar Terr Environm Lab, Toyokawa, Aichi 4428507, Japan
[4] Natl Astron Observ, Nobeyama Radio Observ, Minamisa Ku, Nagano 3841305, Japan
来源：
MAGNETIC RECONNECTION PROCESSES IN THE SOLAR ATMOSPHERE | 2000年 / 26卷 / 03期
关键词：
D O I：
10.1016/S0273-1177(99)01103-5
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
We present hard X-ray imaging observations of impulsive solar flares with Yohkoh HXT, focusing on the evolution of hard X-ray double footpoint sources seen in the energy range above 30 keV. In 7 out of the 14 events studied, the separation between the double sources increases (at the 30 confidence level) as the flare progresses, with the double sources moving nearly anti-parallel to each other in most cases. Implications of these results to the global magnetic field structure responsible for solar flare energy release / particle acceleration are discussed. (C) 2000 COSPAR. Published by Elsevier Science Ltd.
引用
收藏
页码：497 / 500
页数：4
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