太阳黑子本影点的亮度、分布和演化
Brightness, distribution, and evolution of sunspot umbral dots
摘要：
我们提出了一个106分钟的TiO（705.7 nm）的时间序列的高空间和时间分辨率，其中包含数千个本影点（UD）在一个成熟的太阳黑子的活动区NOAA 10667在$μ$ =0.95。这些数据是由位于拉帕尔马的1米瑞典太阳望远镜获得的。借助多级跟踪算法（MLT）的帮助下，12836本影点的大小，亮度和轨迹被发现和分析。MLT允许可靠地识别对比度非常低的UD。在本影内部，我们确定UD填充因子为11%。UD寿命的直方图是单调的，即UD没有典型的寿命。四分之三的UD寿命不到150秒，没有或几乎没有运动。UD直径的直方图在225 km处显示出最大值，即大多数UD都是空间分辨的。UDs显示出典型的水平速度为420米/秒，典型的峰值强度为安静光球平均强度的51%，使它们平均比当地本影背景亮20%。几乎所有可移动的UD（大生灭距离）都出生在本影-半影边界附近，向本影中心移动，并且比平均亮度更亮。沿着一条突出的UD链也观察到了明显明亮和移动的UD，该UD链的两端位于本影-半影边界。他们的运动主要从链条的两端开始，沿着链条继续，并在链条的中心附近结束。我们观察到的分裂和合并的UD和时间的继承。这是第一次，一个典型的UD的亮度，大小和水平速度的演变可以确定在统计上显着的方式。中央和外围UD的演变之间存在相当大的差异，这表明起源的差异。
英文摘要：
We present a 106-minute TiO (705.7nm) time series of high spatial and temporal resolution that contains thousands of umbral dots (UDs) in a mature sunspot in the active region NOAA 10667 at $μ$=0.95. The data were acquired with the 1-m Swedish Solar Telescope on La Palma. With the help of a multilevel tracking (MLT) algorithm the sizes, brightnesses, and trajectories of 12836 umbral dots were found and analyzed. The MLT allows UDs with very low contrast to be reliably identified. Inside the umbra we determine a UD filling factor of 11%. The histogram of UD lifetimes is monotonic, i.e. a UD does not have a typical lifetime. Three quarters of the UDs lived for less than 150s and showed no or little motion. The histogram of the UD diameters exhibits a maximum at 225km, i.e. most of the UDs are spatially resolved. UDs display a typical horizontal velocity of 420m/s and a typical peak intensity of 51% of the mean intensity of the quiet photosphere, making them on average 20% brighter than the local umbral background. Almost all mobile UDs (large birth-death distance) were born close to the umbra-penumbra boundary, move towards the umbral center, and are brighter than average. Notably bright and mobile UDs were also observed along a prominent UD chain, both ends of which are located at the umbra-penumbra boundary. Their motion started primarily at either of the ends of the chain, continued along the chain, and ended near the chain's center. We observed the splitting and merging of UDs and the temporal succession of both. For the first time the evolution of brightness, size, and horizontal speed of a typical UD could be determined in a statistically significant way. Considerable differences between the evolution of central and peripheral UDs are found, which point to a difference in origin.
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