THE AREA DISTRIBUTION OF SOLAR MAGNETIC BRIGHT POINTS
THE AREA DISTRIBUTION OF SOLAR MAGNETIC BRIGHT POINTS
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DOI：
10.1088/2041-8205/722/2/l188
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发表时间：
2010-09
期刊：
影响因子：
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通讯作者：
P. J. Crockett;M. Mathioudakis;D. Jess;S. Shelyag;F. Keenan;Damian J. Christian
中科院分区：
文献类型：
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作者：
P. J. Crockett;M. Mathioudakis;D. Jess;S. Shelyag;F. Keenan;Damian J. Christian
磁亮点（MBPs）是太阳光球层上最小的可观测物体之一。采用g波段观测和数值模拟相结合的方法确定了它们的面积分布。采用一维强度剖面的自动检测算法在观测和模拟数据集中识别这些结构。两种分布均在约45000 km2的面积处达到峰值，并向较小的面积急剧减少。分布符合对数正态统计量，表明通量碎片化优于通量收敛。辐射磁对流模拟表明，不同磁通密度的MBP面积分布具有独立性。最常见的亮点大小对应于颗粒间通道的典型宽度。
Magnetic bright points (MBPs) are among the smallest observable objects on the solar photosphere. A combination of G-band observations and numerical simulations is used to determine their area distribution. An automatic detection algorithm, employing one-dimensional intensity profiling, is utilized to identify these structures in the observed and simulated data sets. Both distributions peak at an area of ≈45,000 km2, with a sharp decrease toward smaller areas. The distributions conform with log-normal statistics, which suggests that flux fragmentation dominates over flux convergence. Radiative magneto-convection simulations indicate an independence in the MBP area distribution for differing magnetic flux densities. The most commonly occurring bright point size corresponds to the typical width of inter-granular lanes.