论文标题
黑子penubrae的水平运动
Horizontal motions in sunspot penubrae
论文作者
论文摘要
需要对半肿的水平运动进行高分辨率观察，以补充从光谱极化获得的半阴茎的概念。分析了G带和红色连续体中使用瑞典太阳能望远镜获得的AR 10634中大黑子的强度图像。两个同时的时间序列持续六个小时五分钟。半半晶粒（PGS）的水平运动，细丝的暗体中的结构，外半月边界和G波段明亮点以时间切片为覆盖整个PENUMBRA和相邻颗粒的时间切片。空间和时间分辨率分别为90 km和20.1 s。在内部半月，PGS的平均速度为-0.7 km S -1。运动方向在大约60％的半宽宽度上从向内变为向外，平均速度在外部阴茎中逐渐增加，接近0.5 km/s。这种速度也是通常在持续一个小时且随后进行快速收缩的时期内膨胀的速度。大多数G波段的明亮点远离黑子，典型的速度为0.6 km/s。在半丝丝的黑色体中，平均观察到高外向速度，平均为3.6 km/s。根据半丝细丝的模型，建议在细丝的黑色体中检测到的速度与Evershed Flow相关，并且内部和外部PG的PG运动的相反方向可以通过丝状头部中上升的质量的相互作用与周围含有磁场不同的磁场相互作用。
High-resolution observations of horizontal motions in the penumbra are needed to complement the concept of penumbrae obtained from spectropolarimetry. Time series of intensity images of a large sunspot in AR 10634 acquired with the Swedish Solar Telescope in the G band and red continuum are analysed. The two simultaneous time series last six hours and five minutes. Horizontal motions of penumbral grains (PGs), structures in dark bodies of filaments, the outer penumbral border, and G-band bright points are measured in time slices that cover the whole width of the penumbra and the neighbouring granulation. The spatial and temporal resolutions are 90 km and 20.1 s, respectively. In the inner penumbra, PGs move toward the umbra (inwards) with a mean speed of -0.7 km s-1. The direction of motion changes from inwards to outwards at approximately 60% of the penumbral width and the mean speed increases gradually in the outer penumbra, approaching 0.5 km/s. This speed is also typical of an expansion of the penumbra-granulation border during periods that typically last one hour and are followed by a fast contraction. The majority of the G-band bright points moves away from the sunspot, with a typical speed of 0.6 km/s. High outward speeds, 3.6 km/s on average, are observed in dark bodies of penumbral filaments. According to the model of penumbral filaments, it is suggested that the speeds detected in the dark bodies of filaments are associated with the Evershed flow and that the opposite directions of PG motions in the inner and outer penumbrae may be explained by the interaction of rising plasma in filament heads with a surrounding, differently inclined magnetic field.
