日冕磁环漏斗状腿中的上升流
Upflows in funnel-like legs of coronal magnetic loops
摘要：
Ne viii的显著蓝移与平静太阳中磁网络的连接点有关，这一点仍然没有得到很好的理解。通过比较的日冕磁场结构所获得的位场重建与显着的蓝移补丁的多普勒频移Ne VIII在赤道安静的太阳区域观察到的，我们发现，大多数地区具有显着的上升流与漏斗状的腿的磁环和共空间的线宽的增量。这些准定常上升流可被视为日冕环物质供应的特征。通过使用线强度的平方根作为等离子体密度的代理，可以估计每个漏斗中的上升流的质量通量。我们发现，质量通量是反相关的漏斗的膨胀因子确定从外推的磁场。其中一个环系统与一个日冕亮点有关，它被几种仪器观测到，在不同的波长和观察方向上表现出各种形态。一个显着的协议之间的磁性结构和相关的EUV发射模式被发现，表明一个几乎势场性质的日冕磁场。我们还报告了直接检测的小规模虹吸流的STEREO卫星。然而，这种瞬态虹吸流发生在一个弱的混合极性场区域，这是外相邻的磁漏斗，因此，它可能是不相关的漏斗中的等离子体上升流。基于这些观测结果，我们认为，在上TR温度的主导流在安静的太阳日冕环是持久的上升流，而不是虹吸流。我们还讨论了日冕加热和未解决的磁结构的影响。
英文摘要：
The prominent blue shifts of Ne viii associated with the junctions of the magnetic network in the quiet Sun are still not well understood. By comparing the coronal magnetic-field structures as obtained by a potential-field reconstruction with the conspicuous blue-shift patches on the dopplergram of Ne viii as observed in an equatorial quiet-Sun region, we find that most of the regions with significant upflow are associated with the funnel-like legs of magnetic loops and co-spatial with increments of the line width. These quasi-steady upflows can be regarded as the signatures of mass supply to coronal loops. By using the square-root of the line intensity as a proxy for the plasma density, the mass flux of the upflow in each funnel can be estimated. We find that the mass flux is anti-correlated with the funnel's expansion factor as determined from the extrapolated magnetic field. One of the loop systems is associated with a coronal bright point, which was observed by several instruments and exhibited various morphologies in different wavelengths and viewing directions. A remarkable agreement between its magnetic structure and the associated EUV emission pattern was found, suggesting an almost potential-field nature of the coronal magnetic field. We also report the direct detection of a small-scale siphon flow by both STEREO satellites. However, this transient siphon flow occurred in a weak mixed-polarity-field region, which was outside the adjacent magnetic funnel, and thus it is perhaps not related to plasma upflow in the funnel. Based on these observations, we suggest that at upper-TR temperatures the dominant flows in quiet-Sun coronal loops are long-lasting upflows rather than siphon flows. We also discuss the implications for coronal heating and unresolved magnetic structures.
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