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Coronal Holes and Open Magnetic Flux

机译：冠状孔和开放磁通

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摘要

Coronal holes are low-density regions of the corona which appear dark in X-rays and which contain "open" magnetic flux, along which plasma escapes into the heliosphere. Like the rest of the Sun's large-scale field, the open flux originates in active regions but is subsequently redistributed over the solar surface by transport processes, eventually forming the polar coronal holes. The total open flux and radial interplanetary field component vary roughly as the Sun's total dipole strength, which tends to peak a few years after sunspot maximum. An inverse correlation exists between the rate of flux-tube expansion in coronal holes and the solar wind speed at 1 AU. In the rapidly diverging fields present at the polar hole boundaries and near active regions, the bulk of the heating occurs at low heights, leading to an increase in the mass flux density at the Sun and a decrease in the asymptotic wind speed. The quasi-rigid rotation of coronal holes is maintained by continual footpoint exchanges between open and closed field lines, with the reconnection taking place at the streamer cusps. At much lower heights within the hole interiors, "interchange reconnection" between small bipoles and the overlying open flux also gives rise to coronal jets and polar plumes.
机译：日冕孔是日冕的低密度区域，在X射线中看起来很暗，并且包含“开放”磁通量，等离子体沿着该磁通量逸出进入日光层。像其他太阳大尺度场一样，开放通量起源于活动区域，但随后通过传输过程重新分布在太阳表面，最终形成了极地冠冕孔。总的开放通量和径向行星际场分量随太阳的总偶极子强度而变化，太阳总偶极子强度往往在太阳黑子最大后的几年达到峰值。冠状孔中的通量管膨胀率与1 AU下的太阳风速成反比。在极孔边界和活动区域附近出现的快速发散场中，大部分加热发生在低高度，导致太阳处的质量通量密度增加，而渐近风速减小。冠状孔的准刚性旋转通过开放和闭合场线之间的连续脚点交换来保持，并且重新连接发生在拖缆的尖端。在孔内部的高度低得多时，小双极子与上面的开放通量之间的“互换重新连接”也会产生日冕射流和极羽。

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