抚仙湖太阳观测和研究基地知识库

太阳磁场结构在日面上具有各种不同的空间尺度。我国最大口径的地基太阳观测设备NVST (新真空太阳望远镜) 在光球波段上的衍射极限接近太阳磁元的尺度范围，标志着太阳低层大气的成像观测迈入了优于0.2′′ 的高分辨率时代。NVST 已获取海量的光球观测数据，扎根于米粒暗径里的超精细磁结构能够有效地分辨出来。光球亮点的观测特征和物理机制的研究是太阳物理领域中普遍关注且高度重视的前沿课题。采用图像处理技术来识别和提取出光球亮点并运用数值分析手段获取光球亮点的统计参数，是十分重要的方法。提出了一种拉普拉斯变换和形态学膨胀相结合的图像处理算法，可用来高效准确地识别出光球亮点，并得到其典型直径、面积分布、形状演化和强度变化等特征参数。最后讨论了光球亮点的物理参数对于理解磁场能量从光球传输到日冕并对高层大气进行加热的科学意义。

Solar magnetic structures in the lower atmosphere exhibit a wealth of different spatial and temporal scales. Presently, solar magnetic element is believed to be the ultra-fine magnetic structure of the Sun, and the diffraction limit of the best solar telescope (New Vacuum Solar Telescope; NVST) of China is close to the spatial scale of magnetic element. This implies that solar observations have entered the era of high resolution better than 0:2′′. Since the year of 2011, the NVST has successfully established and obtained huge observational data. Moreover, the ultra-fine magnetic structures rooted in the dark inter-graunlar lanes can be easily observed. Studies on the observational characteristics and physical mechanism of photospheric bright points (PBPs) are the most important and hottest aspects in solar physics, so it is very important to obtain the statistical parameters of PBPs with the feature extraction techniques and numerical analysis approaches. For identifying the PBPs, an automatically and effectively detection algorithm employed the Laplacian transform and the morphological dilation technique is proposed. Then, the statistical parameters such as the typical diameter, the area distribution, the eccentricity, and the intensity contrast are obtained. And finally, the scientific meaning of studying the physical parameters of PBPs is discussed, especially for understanding the physical processes of solar magnetic energy transferred from the photosphere to the corona.