Velocity structure of jets in a coronal hole

被引：52
作者：
Kamio, Suguru [1 ]
Hara, Hirohisa [1 ]
Watanabe, Tetsuya [1 ]
Matsuzaki, Keiichi [2 ]
Shibata, Kazunari [3 ]
Culhane, Len [4 ]
Warren, Harry P. [5 ]
机构：
[1] Natl Inst Nat Sci, Natl Astron Observ Japan, Solar Phys Div, Hinode Sci Ctr, Mitaka, Tokyo 1818588, Japan
[2] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan
[3] Kyoto Univ, Grad Sch Sci, Kwasan Observ, Yamashina Ku, Kyoto 6078471, Japan
[4] UCL, Mullard Space Sci Lab, Dept Space & Climate Phys, Dorking RH5 6NT, Surrey, England
[5] USN, Res Lab, Solar Terr Relationships Branch, Washington, DC 20375 USA
来源：
PUBLICATIONS OF THE ASTRONOMICAL SOCIETY OF JAPAN | 2007年 / 59卷 / sp3期
基金：
英国科学技术设施理事会;
关键词：
sun : atmospheric motions; sun : corona; sun : UV radiation;
D O I：
10.1093/pasj/59.sp3.S757
中图分类号：
P1 [天文学];
学科分类号：
0704 ;
摘要：
The velocity structures of jets in a coronal hole have been derived for the first time. Hinode observations revealed the existence of many bright points in coronal holes. They are loop-shaped and sometimes associated with coronal jets. Spectra obtained with the Extreme-ultraviolet Imaging Spectrometer aboard Hinode were analyzed to infer the Doppler velocity of bright loops and jets in a coronal hole of the north polar region. Elongated jets above bright loops are found to be blue-shifted by 30 km s(-1) at maximum, while foot points of bright loops are red-shifted. Blue-shifts detected in coronal jets are interpreted as being upflows produced by magnetic reconnection between emerging flux and the ambient field in the coronal hole.
引用
收藏
页码：S757 / S762
页数：6
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