Chromospheric Anemone Jets as Evidence of Ubiquitous Reconnection
Kazunari Shibata,(1) Tahei Nakamura,(1) Takuma Matsumoto,(1)
Kenichi Otsuji,(1) Takenori J. Okamoto,(1),(2) Naoto Nishizuka,(1)
Tomoko Kawate,(1) Hiroko Watanabe,(1) Shin'ichi Nagata,(1)
Satoru UeNo,(1) Reizaburo Kitai,(1) Satoshi Nozawa,(3)
Saku Tsuneta,(2) Yoshinori Suematsu,(2) Kiyoshi Ichimoto,(2)
Toshifumi Shimizu,(4) Yukio Katsukawa,(2)
Theodore D. Tarbell,(5) Thomas E. Berger,(5) Bruce W. Lites,(6)
Richard A. Shine,(5) Alan M. Title(5)
Abstract
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.
(1) Kwasan and Hida Observatories, Kyoto University, JAPAN
(2) National Astronomical Observatory, JAPAN
(3) Department of Science, Ibaraki University, JAPAN
(4) Institute of Space and Astronautical Science/Japan Aerospace
Exploration Agency, JAPAN
(5) Lockheed Martin Solar and Astrophysics Laboratory, USA
(6) High Altitude Observatory, USA
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