从立体/Secchi图像重建立体极烟羽
Stereoscopic Polar Plume Reconstructions from Stereo/Secchi Images
摘要：
我们提出了立体重建的位置和倾斜的极地羽流的两个数据集的基础上的两个同时记录的图像由EUVI望远镜在SECCHI仪器包板载的\emph{STEREO (Solar TErrestrial RElations Observatory)}航天器。研究的十个羽流在三维冕洞中表现出超径向膨胀，这与二维结果一致。它们与当地子午面的偏差相当小，平均值为$6.47^{\circ}$。通过与轴沿太阳自转轴的偶极场重建的羽流进行比较，发现羽流比偶极场更倾向于水平方向。纬度越低，对偶极子场的偏离越大。羽流和亮点之间的关系已经被研究过了，它们并不总是相关的。对于第一个数据集，基于烟羽的3D高度和电子密度从SUMER/ \emph{SOHO} Si { \sc viii}线对，我们发现，电子密度沿烟羽随着高度以上的太阳表面上的减少。由密度标度高度获得的温度比由Mg { \sc ix}线比率获得的温度大1.6至1.8倍。我们把这种差异归因于电子和离子温度的偏差。最后，我们发现，在O { \sc vi}线上研究的羽流的流出速度由视线和羽流方向之间的角度校正是相当小的，最大值为10 $\mathrm{km s^{-1}}$。羽流不太可能是快速太阳风的主要贡献者。
英文摘要：
We present stereoscopic reconstructions of the location and inclination of polar plumes of two data sets based on the two simultaneously recorded images taken by the EUVI telescopes in the SECCHI instrument package onboard the \emph{STEREO (Solar TErrestrial RElations Observatory)} spacecraft. The ten plumes investigated show a superradial expansion in the coronal hole in 3D which is consistent with the 2D results. Their deviations from the local meridian planes are rather small with an average of $6.47^{\circ}$. By comparing the reconstructed plumes with a dipole field with its axis along the solar rotation axis, it is found that plumes are inclined more horizontally than the dipole field. The lower the latitude is, the larger is the deviation from the dipole field. The relationship between plumes and bright points has been investigated and they are not always associated. For the first data set, based on the 3D height of plumes and the electron density derived from SUMER/\emph{SOHO} Si {\sc viii} line pair, we found that electron densities along the plumes decrease with height above the solar surface. The temperature obtained from the density scale height is 1.6 to 1.8 times larger than the temperature obtained from Mg {\sc ix} line ratios. We attribute this discrepancy to a deviation of the electron and the ion temperatures. Finally, we have found that the outflow speeds studied in the O {\sc vi} line in the plumes corrected by the angle between the line of sight and the plume orientation are quite small with a maximum of 10 $\mathrm{km s^{-1}}$. It is unlikely that plumes are a dominant contributor to the fast solar wind.
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