On the Distribution of the Solar Magnetic Fields
On the Distribution of the Solar Magnetic Fields
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DOI：
10.1086/175800
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发表时间：
1995-06
期刊：
影响因子：
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通讯作者：
Haosheng Lin
中科院分区：
文献类型：
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作者：
Haosheng Lin
我们使用了两条磁敏红外FeI线，研究了太阳磁场的分布。我们使用了两条磁敏红外FeI线，分别位于15648.5？和15652.9？我们发现，网内元素的平均场强约为500高斯。此外，太阳表面磁场分布可以用二分量模型来描述。第一个分量是强场分量。它包括太阳黑子、黑子和宁静区域网络中的磁性元素，平均场强为1400高斯。第二个组件是主要由网内网元组成的弱场组件。我们还发现，弱场元素的平均直径约为70公里。我们认为，强场和弱场分量的明显区别意味着，强场代表着由太阳等离子体热压支撑的大尺度、根深蒂固的太阳周场；弱场分量可能由太阳对流带的湍流速度产生，并受到太阳对流运动的湍流压力的支持。
We use the two magnetically sensitive infrared Fe I lines at We use the two magnetically sensitive infrared Fe I lines at 15648.5 Åand 15652.9 Å to study the distribution of the solar magnetic fields. We found that the intra-network elements have an average field strength of about 500 gauss. Furthermore the solar surface magnetic field distribution can be described by a 2-component mode. The first component is the strong-field component. It includes the magnetic elements found in sunspots, plages, and quiet region network, and has an average field strength of 1400 gauss. The second component is the weak-field component comprised mostly of the intra-network elements. We also found that the average size of the weak-field elements is approximately 70 km in diameter.We suggest that the clear distinction between the strong-and weak-field components imply that the strong-field represent the large-scale, deeply rooted solar-cycle field supported by the thermal pressure of the solar plasma; the weak-field component may be generated by the turbulent velocity of the solar convection zone, and is supported by the turbulent pressure of the solar convective motion.