Solar Wind Origin in Coronal Funnels
Solar Wind Origin in Coronal Funnels
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DOI：
10.1126/science.1109447
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发表时间：
2005-04
期刊：
影响因子：
56.9
通讯作者：
C. Tu;Cheng Zhou;E. Marsch;L. Xia;Liang Zhao;Jingxiu Wang;K. Wilhelm
中科院分区：
文献类型：
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作者：
C. Tu;Cheng Zhou;E. Marsch;L. Xia;Liang Zhao;Jingxiu Wang;K. Wilhelm
日冕洞中太阳风的起源一直不清楚。我们确定，太阳风在光球层上方5到20百万米的高度开始以磁漏斗的形式流出日冕。这一结果是通过各种离子发射的谱线的多普勒速度和辐射率图与从光球磁图外推到不同高度的无力磁场的相关性得到的。具体来说，我们发现Ne7+离子主要辐射约20兆米，其中它们的流出速度约为每秒10公里，而没有平均流速的C3+离子主要辐射约5兆米。在此基础上，提出了一个认识太阳风起源的模型。
The origin of the solar wind in solar coronal holes has long been unclear. We establish that the solar wind starts flowing out of the corona at heights above the photosphere between 5 megameters and 20 megameters in magnetic funnels. This result is obtained by a correlation of the Doppler-velocity and radiance maps of spectral lines emitted by various ions with the force-free magnetic field as extrapolated from photospheric magnetograms to different altitudes. Specifically, we find that Ne7+ ions mostly radiate around 20 megameters, where they have outflow speeds of about 10 kilometers per second, whereas C3+ ions with no average flow speed mainly radiate around 5 megameters. Based on these results, a model for understanding the solar wind origin is suggested.