arXiv 1202.20722012-02astro-ph.SR

在HELIO项目框架内实现长丝跟踪自动化

Automation of the filament tracking in the framework of the HELIO project

Xavier Bonnin, Jean Aboudarham, Nicolas Fuller, Andre Csillaghy, Robert D. Bentley

DOI：: 10.1007/10.1007/s11207-012-9985-9

摘要：

我们提出了一种新的方法来自动跟踪太阳盘面上的暗条。这些暗条首先在Meudon太阳分光照相Hα图像上被探测到，应用了Fuller、Aboudarham和Bentley开发的技术（Solar phys. 227，61，2005）。该技术结合了清洗过程、基于区域生长的图像分割和形态学参数提取，包括细丝骨架的确定。骨架像素的坐标，在日心系统中给出，然后转换到一个更合适的参考系，遵循太阳表面的旋转。在这样的框架中，同向旋转的细丝总是位于相同的位置周围，并且其骨架（从每个图像中提取）因此在空间上接近，形成一组相邻的特征。在第三步中，使用曲线匹配算法将每个骨架的形状与其邻居进行比较。这一步将允许我们定义概率[P ]，即在同向旋转框架中的两个接近的细丝实际上是在两个不同图像上观察到的同一个细丝。在结束时，对功能，其相应的概率大于阈值，使用跟踪识别indexs.On长丝的代表性样品相关联，自动和手动跟踪之间的良好的协议确认的可靠性的技术应用于大数据集。特别是，这一代码已经在太阳物理学综合观测台的框架内使用，以充实专门用于太阳和日光层特征的目录。这种方法还可以推广到其他暗条观测，并可能用于太阳黑子、光斑和冕洞的跟踪。

英文摘要：

We present a new method to automatically track filaments over the solar disk. The filaments are first detected on Meudon Spectroheliograph Hα images of the Sun, applying the technique developed by Fuller, Aboudarham, and Bentley (Solar phys. 227, 61, 2005). This technique combines cleaning processes, image segmentation based on region growing, and morphological parameter ex- traction, including the determination of filament skeletons. The coordinates of the skeleton pixels, given in a heliocentric system, are then converted to a more appropriate reference frame that follows the rotation of the Sun surface. In such a frame, a co-rotating filament is always located around the same position, and its skeletons (extracted from each image) are thus spatially close, forming a group of adjacent features. In a third step, the shape of each skeleton is compared with its neighbours using a curve-matching algorithm. This step will permit us to define the probability [P ] that two close filaments in the co-rotating frame are actually the same one observed on two different images. At the end, the pairs of features, for which the corresponding probability is greater than a threshold value, are associated using tracking identification indexes.On a representative sample of filaments, the good agreement between automated and manual tracking confirms the reliability of the technique to be applied on large data sets. Especially, this code is already used in the framework of the Heliophysics Integrated Observatory (HELIO) to populate a catalogue dedicated to solar and heliospheric features (HFC). An extension of this method to others filament observations, and possibly the sunspots, faculae, and coronal holes tracking can be also envisaged.

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