Tu Chuan-Yi, Zhou Cheng, Marsch Eckart, Xia Li-Dong, Zhao Liang, Wang Jing-Xiu, Wilhelm Klaus
Department of Geophysics, Peking University, Beijing 100871, China.
Science. 2005 Apr 22;308(5721):519-23. doi: 10.1126/science.1109447.
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.
长期以来，日冕洞中的太阳风起源一直不明。我们确定，太阳风在光球层上方5兆米至20兆米高度的磁漏斗中开始从日冕流出。这一结果是通过将不同离子发射的光谱线的多普勒速度图和辐射度图与从光球磁图外推到不同高度的无力磁场相关联而获得的。具体而言，我们发现Ne7+离子大多在约20兆米处辐射，在那里它们的流出速度约为每秒10公里，而平均流速为零的C3+离子主要在约5兆米处辐射。基于这些结果，提出了一个理解太阳风起源的模型。
