Extremely Microwave-Rich Solar Flare Observed with Nobeyama Radioheliograph
Extremely Microwave-Rich Solar Flare Observed with Nobeyama Radioheliograph
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野边山射电日光仪观测到极其富含微波的太阳耀斑
DOI：
10.1093/pasj/65.sp1.s1
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发表时间：
2013
影响因子：
2.3
通讯作者：
S. Ishikawa and M. Ohno
中科院分区：
文献类型：
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作者：
S. Masuda;M. Shimojo;T. Kawate;S. Ishikawa and M. Ohno
2011年3月10日，野边山射电日像仪（NoRH）在西翼稍后观测到一个紧凑型耀斑。在17和34 GHz的微波峰值通量值分别为约210和133 sfu。从17 GHz峰值通量和GOES 1-8的软X射线峰值通量之间的相关性，M1.5级预计为这个微波通量。然而，在耀斑期间，在GOES 1-8的软X射线光变曲线中，在C1级背景上只检测到B1级增强。除了微波外，朱雀号还探测到了硬X射线辐射，甚至在100 keV以上的能量范围内。很明显，在这次耀斑中有效地产生了高能电子，而热辐射非常弱。为什么这枚耀斑会有这样的特点？考虑以下两种情况。一种情况是，电子的磁阱有效地工作，每个电子在其相对较长的寿命内继续发射微波。另一个是环顶区域周围的磁场很强，相对大量的低能电子发射微波。考虑到观测事实，如短持续时间和小耀斑环，后一种情况更合理。
A compact flare was observed with Nobeyama Radioheliograph (NoRH) slightly behind the west limb on 2011 March 10. The microwave peak flux values at 17 and 34 GHz were about 210 and 133 sfu, respectively. From the correlation between the 17 GHz peak flux and the GOES 1-8 Å soft X-ray peak flux, M1.5-class is expected for this microwave flux. However, only the B1-level enhancement was detected in the GOES 1-8 Å soft X-ray light curve on the C1-level background during the flare period. In addition to microwaves, Suzaku detected hard X-ray emissions, even in the energy range above 100 keV. It is clear that high-energy electrons were effectively produced in this flare, while the thermal emission was very weak. Why did this flare have this unique feature? The following two cases are considered. One is the case that a magnetic trap for electrons works effectively, and that each electron continues to emit microwaves in its relatively long lifetime. The other is that the magnetic field around the looptop region is intense, and relatively a large number of lower-energy electrons emit microwaves. Considering the observational facts, such as the short duration and the small flare loop, the latter case is more plausible.