WHAT DO IRIS OBSERVATIONS OF Mg II k TELL US ABOUT THE SOLAR PLAGE CHROMOSPHERE?
WHAT DO IRIS OBSERVATIONS OF Mg II k TELL US ABOUT THE SOLAR PLAGE CHROMOSPHERE?
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Mg II k 的虹膜观测告诉我们有关太阳斑色球层的哪些信息？
DOI：
10.1088/2041-8205/809/2/l30
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发表时间：
2015
期刊：
影响因子：
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通讯作者：
B. Pontieu
中科院分区：
文献类型：
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作者：
M. Carlsson;J. Leenaarts;B. Pontieu
我们分析了观测的界面区域成像光谱仪的Mg二k线，Mg二紫外线的附属线，和O i 135.6 nm？>线，以更好地了解太阳plage色球层。我们还比较了瑞典1米太阳望远镜的Hα线，Ca ii 8542线和太阳动力学天文台/大气成像组件的日冕19.3 nm观测。线为了了解观察到的Mg ii分布，我们将这些观察结果与数值实验的结果进行了比较。在谱斑中发现的单峰或平顶的Mg ii k分布意味着在高柱质量和约6500 K的热而致密的色球层处存在一个过渡区。这种情况是支持所观察到的苔藓亮度和填充的配置文件很少或没有自我逆转之间的大规模相关性。在斑中发现的大的翼宽也意味着一个热而致密的色球层，色球层温度急剧上升。Mg Ⅱ次级谱线的不发射限制了色球温度和温度上升的高度，而O Ⅰ的宽度为135.6 nm？线将非热速度限制在7 km s-1左右。
We analyze observations from the Interface Region Imaging Spectrograph of the Mg ii k line, the Mg ii UV subordinate lines, and the O i 135.6 nm ?> line to better understand the solar plage chromosphere. We also make comparisons with observations from the Swedish 1-m Solar Telescope of the Hα line, the Ca ii 8542 line, and Solar Dynamics Observatory/Atmospheric Imaging Assembly observations of the coronal 19.3 nm ?> line. To understand the observed Mg ii profiles, we compare these observations to the results of numerical experiments. The single-peaked or flat-topped Mg ii k profiles found in plage imply a transition region at a high column mass and a hot and dense chromosphere of about 6500 K. This scenario is supported by the observed large-scale correlation between moss brightness and filled-in profiles with very little or absent self-reversal. The large wing width found in plage also implies a hot and dense chromosphere with a steep chromospheric temperature rise. The absence of emission in the Mg ii subordinate lines constrain the chromospheric temperature and the height of the temperature rise while the width of the O i 135.6 nm ?> line sets a limit to the non-thermal velocities to around 7 km s−1.