Chromospheric Anemone Jets as Evidence of Ubiquitous Reconnection
Chromospheric Anemone Jets as Evidence of Ubiquitous Reconnection
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DOI：
10.1126/science.1146708
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发表时间：
2007-12
期刊：
影响因子：
56.9
通讯作者：
K. Shibata;Tahei Nakamura;Takuma Matsumoto;Ken Otsuji;T. Okamoto;N. Nishizuka;T. Kawate;H. Watanabe-H
中科院分区：
文献类型：
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作者：
K. Shibata;Tahei Nakamura;Takuma Matsumoto;Ken Otsuji;T. Okamoto;N. Nishizuka;T. Kawate;H. Watanabe-H
太阳色球层和日冕的加热是太阳物理学中一个长期存在的难题。日出观测表明，在活动区的太阳黑子外，色球海葵喷流无处不在。它们通常长3至7弧秒= 2000至5000公里，宽0.2至0.4弧秒= 150至300公里，速度为每秒10至20公里。这些小喷流呈倒Y形，类似于日冕中X射线海葵喷流的形状。这些特征意味着类似于日冕中的磁场重联发生在整个色球层中一个小得多的空间尺度上，并表明太阳色球层和日冕的加热可能与小尺度无处不在的重联有关。
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.