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IMPLOSION IN A CORONAL ERUPTION

delete2009-04-13
delete50
PRE
AI
R
Rui Liu *
H
Haimin Wang
D
David Alexander
DOI：10.1088/0004-637X/696/1/121delete
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摘要

摘要

En 中文
我们介绍了在预热过程中覆盖在耀斑区域上的极紫外日冕环收缩的观察结果以及ges类C8.9耀斑的早期脉冲阶段。在相对较长的6分钟预热阶段中，较低能量 (低于25 keV) 的硬x射线 (HXR) 计数率以及软x射线通量逐渐增加，并且耀斑发射由温度为20-30 MK的热环顶源控制。脉冲HXR爆发后，耀斑光谱由17-20 MK的热分量 (对应于环顶发射) 和光谱指数伽马 = 3.5-4.5的非热分量 (对应于一对共轭脚点) 组成。上覆冠状环的收缩与共轭脚点的收敛运动和环顶源的向下运动有关。收缩后冠状环的膨胀与扩口区域中Ha排放的增加以及其北端靠近扩口区域的喷发细丝的加热有关。膨胀最终导致整个磁性结构的喷发和快速的日冕物质抛射。这是第一次记录到覆盖在扩口区域上的冠状环的如此大规模的收缩，这种收缩以类似于5 kms(-1) 的平均速度持续约10分钟。假设爆炸性色球蒸发在补偿燃烧区域的磁压降低中起着重要作用，我们建议以日冕热辐射为主的延长预热阶段是观察日冕内爆的必要条件。在预热阶段累积在电晕中的密集等离子体可以有效地抑制爆炸性色球蒸发，这解释了观察到的内爆持续到脉冲阶段的7分钟。
Keyword:
Sun: corona
Sun: filaments
Sun: flares
Sun: X-rays, gamma rays
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期刊

Astrophysical Journal 封面图
Astrophysical Journal
IF:
5.4
论文数:
8.3W
被引数:
32.0W

机构

R
Rice University
学者数:
1.4W
论文数: 1.2W
被引数: 2.6W
N
New Jersey Institute of Technology
学者数:
4.2K
论文数: 4.5K
被引数: 4.6K
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