Flare ribbon expansion and energy release rate
Flare ribbon expansion and energy release rate
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DOI：
10.1086/422159
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发表时间：
2004-08-10
影响因子：
4.9
通讯作者：
Shibata, K
中科院分区：
文献类型：
--
作者：
Asai, A;Yokoyama, T;Shibata, K
我们研究了发生在2001年4月10日的一次太阳耀斑中，Halpha耀斑带的演化与释放的磁能之间的关系。在磁重联模型的基础上，利用光球磁场强度和Halpha耀斑带前缘的分离速度定量计算了释放能量。我们将释放能量的变化与在硬x射线和微波中观测到的非热辐射的时空波动进行了比较。这些非热辐射源表明了大能量释放发生的时间和地点。我们还估计了耀斑期间释放的磁能。估计的与硬x射线源相关的Halpha核的能量释放率在局部大到足以解释Halpha核与硬x射线源的空间分布之间的差异。我们还利用估算的能量释放率重建了非热辐射峰。
We have examined the relation between the evolution of the Halpha flare ribbons and the released magnetic energy in a solar flare that occurred on 2001 April 10. Based on the magnetic reconnection model, the released energy was quantitatively calculated by using the photospheric magnetic field strengths and separation speeds of the fronts of the Halpha flare ribbons. We compared the variation of the released energy with the temporal and spatial fluctuations in the nonthermal radiation observed in hard X-rays and microwaves. These nonthermal radiation sources indicate when and where large energy releases occur. We also estimated the magnetic energy released during the flare. The estimated energy release rates in the Halpha kernels associated with the hard X-ray sources are locally large enough to explain the difference between the spatial distributions of the Halpha kernels and the hard X-ray sources. We also reconstructed the peaks in the nonthermal emission by using the estimated energy release rates.