Observations of Unresolved Photospheric Magnetic Fields in Solar Flares Using Fe i and Cr i Lines
Observations of Unresolved Photospheric Magnetic Fields in Solar Flares Using Fe i and Cr i Lines
复制标题
使用 Fe i 和 Cr i 线观测太阳耀斑中未解析的光球磁场
DOI：
--
复制
发表时间：
2014
期刊：
影响因子：
--
通讯作者：
V. Lozitsky
中科院分区：
文献类型：
--
作者：
M. Gordovskyy;V. Lozitsky
利用梯形光谱偏振观测研究了太阳耀斑期间光球磁场的结构。这项研究是基于在耀斑热相期间最亮的Hα发射对应的位置观测到的几条Fe-I和CrI-I线。分析是通过比较具有不同磁敏度的线的磁场值，以及检查I±V斯托克斯剖面分裂的精细结构来进行的。结果表明，磁场至少有两个分量，较强的未分辨磁通管嵌入较弱的环境磁场中。基于双分量磁场模型，我们比较了观测和合成的谱线轮廓，结果表明，小尺度通量管中的场强约为2 - 3 kg。此外，我们还发现小尺度的通量管与耀斑发射有关，这可能对耀斑现象的研究有一定的意义。
The structure of the photospheric magnetic field during solar flares is examined using echelle spectropolarimetric observations. The study is based on several Fe i and Cr i lines observed at locations corresponding to brightest Hα emission during thermal phase of flares. The analysis is performed by comparing magnetic-field values deduced from lines with different magnetic sensitivities, as well as by examining the fine structure of I±V Stokes-profiles’ splitting. It is shown that the field has at least two components, with stronger unresolved flux tubes embedded in weaker ambient field. Based on a two-component magnetic-field model, we compare observed and synthetic line profiles and show that the field strength in small-scale flux tubes is about 2 – 3 kG. Furthermore, we find that the small-scale flux tubes are associated with flare emission, which may have implications for flare phenomenology.