Chromospheric Anemone Jets as Evidence of Ubiquitous Reconnection
Kazunari Shibata, Tahei Nakamura, Takuma Matsumoto, Kenichi Otsuji,
Takenori J. Okamoto, Naoto Nishizuka, Tomoko Kawate, Hiroko Watanabe,
Shin'ichi Nagata, Satoru UeNo, Reizaburo Kitai, Satoshi Nozawa, Saku
Tsuneta, Yoshinori Suematsu, Kiyoshi Ichimoto, Toshifumi Shimizu, Yukio
Katsukawa, Theodore D. Tarbell, Thomas E. Berger, Bruce W. Lites,
Richard A. Shine, and Alan M. Title
Supporting Online Material
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Movie S1
Movie S1
Movies of CaII H images taken with Hinode/SOT for 1 hour from 20:00:37
UT to 20:59:18 UT. Images were taken 56-s intervals. Note the numerous jets with bright
footpoints that have a cusp- or inverted Y-shape. These morphologies are similar to those
of x-ray anemone jets observed by Yohkoh/SXT. Hence, these Ca jets are called
chromospheric anemone jets. The anemone shape of the jets provides indirect evidence of
magnetic reconnection as a mechanism for the formation of these jets. The jets are 2000
to 5000 km long and have velocities of 10 to 20 km/s. Note also the presence of
numerous jets without clear bright footpoints, which are not called anemone jets but show
properties (length, width, velocity) similar to those of chromospheric anemone jets.
Hinode observations show that the entire chromosphere is covered by jets, either
anemone or non-anemone.
To view these movies, download a QuickTime viewer.
