论文标题
太阳能活动区域移动小规模强度增强的分类模型
Categorization model of moving small-scale intensity enhancements in solar active regions
论文作者
论文摘要
在太阳能活动区的极端紫外线图像中远程观察到的小尺度移动强度增强，我们称之为活动区域移动篝火（ARMC）与局部血浆温度和/或密度增强有关。它们的动态是由整个冠状血浆中的物理过程驱动的。我们先前对ARMC的研究表明它们在背景速度附近具有特征性速度。我们工作的主要目的是对两个观察任务SDO/AIA和HI-C 2.1的EUV图像进行同时分析。对SDO/AIA和HI-C 2.1进行的交叉验证分析的目的是揭示观察到的移动特征如何分布在研究的活性区域AR12712上，测试具有不同物理特征的不同组ARMC的存在。我们使用以前论文中开发的强度质心收敛和跟踪的统计模型。此外，详细阐述了观察到的移动ARMC复合物的高斯混合模型拟合，以揭示不同ARMC组的存在并研究这些不同基团的物理特征。在SDO/AIA的171Å，193Å和211Å通道的数据中，我们确定了几组ARMC，既相关斑点强度和速度曲线。通过HI-C 2.1的172Å数据集的交叉验证证实了此类组的存在。本文研究的ARMC在冠状环中的典型音速范围内具有特征性的速度。因此，这些运动物体与磁性重新连接位点的众所周知的快速alfvénic速度喷气机不同。 ARMC沿活动区域磁性结构（股线）传播的事实也证明了这一点。尚不清楚发现ARMC事件的统计分组的性质。
The small-scale moving intensity enhancements remotely observed in the extreme ultraviolet images of the solar active regions, which we refer to as active region moving campfires (ARMCs), are related to local plasma temperature and/or density enhancements. Their dynamics is driven by the physical processes in the entire coronal plasma. Our previous study of ARMCs indicates that they have characteristic velocities at around the background sound speed. The main goal of our work is to carry out a simultaneous analysis of EUV images from two observational missions, SDO/AIA and Hi-C 2.1. The aims of the performed cross-validating analysis of both SDO/AIA and Hi-C 2.1 data were to reveal how the observed moving features are distributed over the studied active region, AR12712, test the existence of different groups of ARMCs with distinct physical characteristics. We use the statistical model of intensity centroid convergence and tracking that was developed in our previous paper. Furthermore, a Gaussian mixture model fit of the observed complex of moving ARMCs is elaborated to reveal the existence of distinct ARMC groups and to study the physical characteristics of these different groups. In data from the 171Å, 193Å and 211Å channels of SDO/AIA, we identified several groups of ARMCs with respect to both blob intensity and velocity profiles. The existence of such groups is confirmed by the cross-validation of the 172Å data sets from Hi-C 2.1. The ARMCs studied in this paper have characteristic velocities in the range of the typical sound speeds in coronal loops. Hence, these moving objects differ from the well-known rapid Alfvénic velocity jets from magnetic reconnection sites. This is also proven by the fact that ARMCs propagate along the active region magnetic structure (strands). The nature of the discovered statistical grouping of the ARMC events is not known.
