Gamma-Ray Imaging of the 2003 October/November Solar Flares
Gamma-Ray Imaging of the 2003 October/November Solar Flares
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2003 年 10 月/11 月太阳耀斑的伽马射线成像
DOI：
10.1086/505329
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发表时间：
2006
期刊：
影响因子：
--
通讯作者：
David M. Smith
中科院分区：
文献类型：
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作者：
G. Hurford;S. Krucker;R. Lin;Richard A. Schwartz;G. Share;David M. Smith
我们给出了2.223 MeV中子俘获伽马射线线上的三个耀斑(2003年10月28日、29日和11月2日)的RHESSI成像，角分辨率高达35‘’。对成象通量和空间积分通量的比较表明，在所有情况下，大多数(如果不是全部)辐射被限制在位于耀斑活动区内的规模为数十角秒或更小的致密源中。因此，产生伽马射线的离子似乎是由耀斑过程加速的，而不是由快速日冕物质抛射驱动的大范围激波。10月28日的事件产生了第一张显示双足点伽马射线线源的此类图像。这些脚点源横跨在耀斑环路拱廊上，但与相应的0.2-0.3 MeV电子-韧致辐射发射点相差14“”和17“±5”。与之前研究的2002年7月23日事件一样，这意味着耀斑加速的离子和电子之间在加速和/或传播方面存在空间差异。
We present RHESSI imaging of three flares (2003 October 28 and 29 and November 2) in the 2.223 MeV neutron-capture gamma-ray line with angular resolution as high as 35''. Comparisons of imaged and spatially integrated fluences show that in all cases most, if not all, of the emission was confined to compact sources with size scales of tens of arcseconds or smaller that are located within the flare active region. Thus, the gamma-ray-producing ions appear to be accelerated by the flare process and not by a widespread shock driven by a fast coronal mass ejection. The 28 October event yielded the first such image to show double-footpoint gamma-ray line sources. These footpoint sources straddled the flaring loop arcade but were displaced from the corresponding 0.2-0.3 MeV electron-bremsstrahlung emission footpoints by 14'' and 17'' ± 5''. As with the previously studied 2002 July 23 event, this implies spatial differences in acceleration and/or propagation between the flare-accelerated ions and electrons.