NEW SOLAR TELESCOPE OBSERVATIONS OF MAGNETIC RECONNECTION OCCURRING IN THE CHROMOSPHERE OF THE QUIET SUN

被引：15

作者：

Chae, Jongchul ^{[1
,2
]}

Goode, P. R. ^{[2
]}

Ahn, K. ^{[1
,2
]}

Yurchysyn, V. ^{[2
]}

Abramenko, V. ^{[2
]}

Andic, A. ^{[2
]}

Cao, W. ^{[2
]}

Park, Y. D. ^{[3
]}

机构：

[1] Seoul Natl Univ, Dept Phys & Astron, Astron Program, Seoul 151747, South Korea

[2] Big Bear Solar Observ, Big Bear City, CA 92314 USA

[3] Korea Astron & Space Sci Inst, Taejon 305348, South Korea

来源：

ASTROPHYSICAL JOURNAL LETTERS | 2010年 / 713卷 / 01期

基金：

美国国家科学基金会; 新加坡国家研究基金会;

关键词：

magnetic reconnection; magnetohydrodynamics (MHD); Sun: chromosphere; Sun: magnetic topology; Sun: photosphere; FLUX CANCELLATION SITES; ACTIVE REGION; FIELD;

D O I：

10.1088/2041-8205/713/1/L6

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

Magnetic reconnection is a process in which field-line connectivity changes in a magnetized plasma. On the solar surface, it often occurs with the cancellation of two magnetic fragments of opposite polarity. Using the 1.6 m New Solar Telescope, we observed the morphology and dynamics of plasma visible in the Ha line, which is associated with a canceling magnetic feature (CMF) in the quiet Sun. The region can be divided into four magnetic domains: two pre-reconnection and two post-reconnection. In one post-reconnection domain, a small cloud erupted, with a plane-of-sky speed of 10 km s(-1), while in the other one, brightening began at points and then tiny bright loops appeared and subsequently shrank. These features support the notion that magnetic reconnection taking place in the chromosphere is responsible for CMFs.

引用

页码：L6 / L10

页数：5

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