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Observation of Reconnection Inflow of a Solar Flare

Published online by Cambridge University Press:  13 May 2016

T. Yokoyama ,
K. Akita ,
T. Morimoto ,
K. Inoue  and
J. Newmark
T. Yokoyama
Affiliation:
National Astronomical Observatory of Japan, Nobeyama Radio Observatory, Minamimaki, Minamisaku, 384-1305, Japan
K. Akita
Affiliation:
Osaka Gakuin Univ., Suita, Osaka, 564-8511, Japan
T. Morimoto
Affiliation:
Kyoto Univ., Kyoto, 606-8502, Japan
K. Inoue
Affiliation:
Kyoto Univ., Kyoto, 606-8502, Japan
J. Newmark
Affiliation:
Emergent Information Technologies-East, GSFC/NASA, Greenbelt, MD20771, USA

Abstract

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We find an important piece of evidence for magnetic reconnection inflow in a flare on March 18, 1999. The flare occurred on the north-east limb, displaying a nice cusp-shaped soft X-ray loop and a plasmoid ejection typical for the long-duration-events. As the plasmoid is ejected, magnetic reconnection occurs at the disconnecting point. A clear ingoing pattern toward the magnetic X-point is seen. The velocity of this apparent motion is about 5 km sec−1, which is an upper limit on reconnection inflow speed. Based on this observation, we derive the reconnection rate as MA = 0.001 − 0.03, where MA is a Alfvén Mach number of the inflow.

Type
Session III: Active Region Structure and Dynamics
Information
Symposium - International Astronomical Union , Volume 203: Recent Insights into the Physics of the Sun and Heliosphere: Highlights from Soho and Other Space Missions , 2001 , pp. 344 - 346
Copyright
Copyright © Astronomical Society of the Pacific 2001 

References

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