Small-scale magnetic flux tube diagnostics in a solar flare
Small-scale magnetic flux tube diagnostics in a solar flare
复制标题
太阳耀斑中的小型磁通管诊断
DOI：
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发表时间：
1994
期刊：
影响因子：
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通讯作者：
V. Lozitskij
中科院分区：
文献类型：
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作者：
N. Lozitska;V. Lozitskij
对1989年6月16日2B耀斑中的Fei 5247和5250线的I±V剖面进行了分析。太阳黑子外部耀斑的明亮结已被探索，其中 Hα 的中心强度达到峰值 1.4（相对于连续谱）。分析了飞 5250/飞 5247 磁力线比，该比基于这些线在耀斑五个演化阶段（包括耀斑开始、闪光阶段、峰值和峰值后 16 分钟）的 StokesV 峰间距。结果发现，Fei 5250 系的 StokesV 峰分离系统地大于 Fei 5247 系。这是在耀斑中存在具有 kG 场的小规模通量管的证据。通量管磁场强度在耀斑开始时和闪光阶段约为 1.1 kG，峰值期间为 1.55 kG，峰值后 16 分钟为 1.38 kG。填充因子 α 在耀斑期间似乎单调减少。
I ±V profiles of the Fei 5247 and 5250 lines in the 2B flare of June 16, 1989 have been analyzed. A bright knot of the flare outside the sunspot where the central intensity of Hα reached a peak value of 1.4 (relative to the continuum) has been explored. The Fei 5250/Fei 5247 magnetic line ratio based on the StokesV peak separations of these lines at five evolutionary phases of the flare (including the start of the flare, the flash phase, the peak and 16 min after the peak) has been analyzed. It was found that the StokesV peak separation for the Fei 5250 line was systematically larger than that of the Fei 5247 line. This is evidence for the presence in the flare of small-scale flux tubes with kG fields. The flux tube magnetic field strength was about 1.1 kG at the start of the flare and during the flash phase, 1.55 kG during the peak, and 1.38 kG 16 min after the peak. The filling factor,α, appears to decrease monotonically during the flare.