Slipping magnetic reconnection in coronal loops

被引:93
作者
Aulanier, Guillaume
Golub, Leon
DeLuca, Edward E.
Cirtain, Jonathan W.
Kano, Ryouhei
Lundquist, Loraine L.
Narukage, Noriyuki
Sakao, Taro
Weber, Mark A.
机构
[1] Univ Paris Diderot, UPMC, CNRS, Observ Paris,LESIA, F-92190 Meudon, France
[2] Harvard Smithsonian Ctr Astrophys, Cambridge, MA 02138 USA
[3] Natl Astron Observ Japan, Tokyo 1818588, Japan
[4] Kyoto Univ, Kwasan Observ, Kyoto 6078471, Japan
[5] Kyoto Univ, Hida Observ, Kyoto 6078471, Japan
[6] Japan Aerosp Explorat Agcy, Inst Space & Astronaut Sci, Sagamihara, Kanagawa 2298510, Japan
基金
英国科学技术设施理事会;
关键词
D O I
10.1126/science.1146143
中图分类号
O [数理科学和化学]; P [天文学、地球科学]; Q [生物科学]; N [自然科学总论];
学科分类号
07 ; 0710 ; 09 ;
摘要
The heating of the solar chromosphere and corona is a long-standing puzzle in solar physics. Hinode observations show the ubiquitous presence of chromospheric anemone jets outside sunspots in active regions. They are typically 3 to 7 arc seconds = 2000 to 5000 kilometers long and 0.2 to 0.4 arc second = 150 to 300 kilometers wide, and their velocity is 10 to 20 kilometers per second. These small jets have an inverted Y-shape, similar to the shape of x-ray anemone jets in the corona. These features imply that magnetic reconnection similar to that in the corona is occurring at a much smaller spatial scale throughout the chromosphere and suggest that the heating of the solar chromosphere and corona may be related to small-scale ubiquitous reconnection.
引用
收藏
页码:1588 / 1591
页数:4
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