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The size distribution of magnetic bright points derived from Hinode/SOT observations

机译:从Hinode / SOT观测资料得出的磁性亮点的大小分布

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Context. Magnetic bright points (MBPs) are small-scale magnetic features in the solar photosphere. They may be a possible source of coronal heating by rapid footpoint motions that cause magnetohydrodynamical waves. The number and size distribution are of vital importance in estimating the small scale-magnetic-field energy. Aims. The size distribution of MBPs is derived for G-band images acquired by the Hinode/SOT instrument. Methods. For identification purposes, a new automated segmentation and identification algorithm was developed. Results. For a sampling of 0.108 arcsec/pixel, we derived a mean diameter of km for the MBPs. For the full resolved data set with a sampling of 0.054 arcsec/pixel, the size distribution shifted to a mean diameter of km. The determined diameters are consistent with earlier published values. The shift is most probably due to the different spatial sampling. Conclusions. We conclude that the smallest magnetic elements in the solar photosphere cannot yet be resolved by G-band observations. The influence of discretisation effects (sampling) has also not yet been investigated sufficiently. Key words: Sun: photosphere - magnetic fields - techniques: image processing
机译:上下文。磁亮点(MBP)是太阳光球中的小尺度磁特征。它们可能是通过引起磁流体动力学波的快速脚步运动而引起冠状动脉发热的来源。数量和尺寸分布对于估算小规模的磁场能量至关重要。目的MBP的大小分布是针对由Hinode / SOT仪器获取的G波段图像得出的。方法。为了识别,开发了一种新的自动分割和识别算法。结果。对于0.108 arcsec /像素的采样,我们得出了MBP的平均直径km。对于具有0.054 arcsec /像素采样的完整解析数据集,大小分布转移到km的平均直径。所确定的直径与先前公开的值一致。这种变化很可能是由于不同的空间采样所致。结论。我们得出结论,太阳光球中最小的磁性元素尚无法通过G波段观测得到解决。离散化影响(采样)的影响也尚未得到充分研究。关键词:太阳:光球-磁场-技术:图像处理

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