Magnetic Energy Release during the 2002 September 9 Solar Flare
Magnetic Energy Release during the 2002 September 9 Solar Flare
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2002 年 9 月 9 日太阳耀斑期间的磁能释放
DOI：
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发表时间：
2006
期刊：
影响因子：
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通讯作者：
G. Choe
中科院分区：
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作者：
Jeongwoo Lee;D. Gary;G. Choe
我们利用大熊太阳天文台的高频率(40ms)H-α滤光片，结合鲁文·拉马蒂高能太阳光谱成像仪和欧文斯谷太阳阵列的硬X射线和微波数据，研究了2002年9月9日耀斑期间的磁能释放。我们采用标准二维电流片(RCS)的Pointing矢量法，但提出了一种新的技术来推断RCS的面积，以便完全用观测量来完成磁能计算。我们发现了五个脉冲磁能释放峰，集中在10-30个S周期内，它们与硬X射线光曲线的峰是周期性的。每个峰的最大释放量达到~2.6×1030ergs S-1，由RHESSI谱得到的电子能量沉积率落在磁能释放率的10%-80%范围内。我们将这一结果与迄今为理解太阳耀斑中的磁重联而进行的其他研究相比较，并提出脉动电流片模型是对我们的结果最合理的解释。
We study the magnetic energy release during the 2002 September 9 flare using the high-cadence (40 ms) Hα filtergram at Big Bear Solar Observatory (BBSO), along with hard X-ray and microwave data from the Reuven Ramaty High-Energy Solar Spectroscopic Imager (RHESSI) and the Owens Valley Solar Array (OVSA), respectively. We take the Poynting vector approach with the standard two-dimensional geometry of the reconnecting current sheet (RCS) but suggest a new technique to infer the area of the RCS, in order to complete the magnetic energy calculation entirely with observed quantities. We found five peaks of impulsive magnetic energy release, concentrated within 10-30 s periods, that are episodic with the peaks of the hard X-ray light curve. The maximum amount of energy released per peak reaches ~2.6 × 1030 ergs s-1, and the electron energy deposition rate derived from the RHESSI spectra falls into the range of 10%-80% of the magnetic energy release rate. We briefly discuss this result in comparison with other studies thus far made toward understanding of the magnetic reconnection in solar flares and suggest the pulsating current sheet model as the most plausible interpretation of our result.