Solar wind origin in coronal funnels.
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.
Tu
Chuan-Yi
CY
Department of Geophysics, Peking University, Beijing 100871, China. cytu@public3.bta.net.cn
Zhou
Cheng
C
Marsch
Eckart
E
Xia
Li-Dong
LD
Zhao
Liang
L
Wang
Jing-Xiu
JX
Wilhelm
Klaus
K