A giant quiescent solar filament observed with high-resolution spectroscopy
A giant quiescent solar filament observed with high-resolution spectroscopy
复制标题
用高分辨率光谱观察到的巨大静止太阳灯丝
DOI：
10.1051/0004-6361/201526636
复制
发表时间：
2016
期刊：
影响因子：
--
通讯作者：
C. Denker
中科院分区：
文献类型：
--
作者：
C. Kuckein;M. Verma;C. Denker
2011 年 11 月 15 日，在泰德天文台的真空塔望远镜中，用高分辨率阶梯光栅摄谱仪观察到了一条巨大的、安静的太阳细丝。在色球吸收线 H-alpha 和 Na I D2 中同时记录了一幅马赛克光谱（10 张 100" X 182" 的图）。灯丝等离子体的物理参数是使用云模型（CM）反演和线芯拟合得出的。光谱由色球望远镜 (ChroTel) 的全盘滤光图（He I 10830 A、H-alpha 和 Ca II K）和 HMI 的全盘磁图补充。该灯丝具有极大的线性尺寸 (817")，相当于太阳表面沿大圆的约 658 毫米。使用 CM 方法总共反演了 175119 个 H-alpha 对比度轮廓。推断的平均视线 (LOS) 速度、多普勒宽度和源函数与之前较小静态灯丝的工作类似。然而，导出的光学厚度更大。从 H-alpha 线推断的 LOS 速度趋势核配合比在细丝中检测到的逆流流特征一致，但较小。Na I D2 线核中最大的亮斑与 HMI 观察到的小尺度磁场吻合良好。基于 HMI 磁图的光球水平流计算揭示了大小为 5-8 毫米的流核。细丝末端的速度为 0.30-0.45 公里/秒，超大细丝的物理特性与较小的细丝类似，但我们的样品中发现的光学厚度更大，我们发现前一天喷发的部分细丝正在重建其初始配置。
A giant, quiet-Sun filament was observed with the high-resolution Echelle spectrograph at the Vacuum Tower Telescope at Observatorio del Teide on 2011 November 15. A mosaic of spectra (10 maps of 100" X 182") was recorded simultaneously in the chromospheric absorption lines H-alpha and Na I D2. Physical parameters of the filament plasma were derived using Cloud Model (CM) inversions and line core fits. The spectra were complemented with full-disk filtergrams (He I 10830 A, H-alpha, and Ca II K) of the Chromspheric Telescope (ChroTel) and full-disk magnetograms of HMI. The filament had extremely large linear dimensions (817"), which corresponds to about 658 Mm along a great circle on the solar surface. A total amount of 175119 H-alpha contrast profiles were inverted using the CM approach. The inferred mean line-of-sight (LOS) velocity, Doppler width, and source function were similar to previous works of smaller quiescent filaments. However, the derived optical thickness was larger. LOS velocity trends inferred from the H-alpha line core fits were in accord, but smaller, than the ones obtained with CM inversions. Signatures of counter-streaming flows were detected in the filament.The largest conglomerates of brightenings in the line core of Na I D2 coincided well with small-scale magnetic fields as seen by HMI. Mixed magnetic polarities were detected close to the ends of barbs. The computation of photospheric horizontal flows based on HMI magnetograms revealed flow kernels with a size of 5-8 Mm and velocities of 0.30-0.45 km/s at the ends of the filament. The physical properties of extremely large filaments are similar to their smaller counterparts, except for the optical thickness which in our sample was found to be larger. We found that a part of the filament, which erupted the day before, is in the process of reestablishing its initial configuration.
Ύ´ 点的近红外光谱偏振法
影响因子：
6.5
作者：
Balthasar;Denker
通讯作者：
Denker