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Slipping Magnetic Reconnection in Coronal Loops
Guillaume Aulanier, Leon Golub, Edward E. DeLuca, Jonathan W. Cirtain, Ryouhei Kano, Loraine L. Lundquist, Noriyuki Narukage, Taro Sakao and Mark A. Weber
New Series, Vol. 318, No. 5856 (Dec. 7, 2007), pp. 1588-1591
Published by: American Association for the Advancement of Science
Stable URL: http://www.jstor.org/stable/20051754
Page Count: 4
You can always find the topics here!Topics: Magnetic fields, Magnets, Coronal loops, Astrophysical magnetism, Extreme ultraviolet radiation, Magnetic flux, X ray observatories, Solar observatories, Speed, Solar flares
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Magnetic reconnection of solar coronal loops is the main process that causes solar flares and possibly coronal heating. In the standard model, magnetic field lines break and reconnect instantaneously at places where the field mapping is discontinuous. However, another mode may operate where the magnetic field mapping is continuous but shows steep gradients: The field lines may slip across each other. Soft x-ray observations of fast bidirectional motions of coronal loops, observed by the Hinode spacecraft, support the existence of this slipping magnetic reconnection regime in the Sun's corona. This basic process should be considered when interpreting reconnection, both on the Sun and in laboratory-based plasma experiments.
Science © 2007 American Association for the Advancement of Science