A magnetic reconnection X-line extending more than 390 Earth radii in the solar wind

T. D. Phan (), J. T. Gosling, M. S. Davis, R. M. Skoug, M. Øieroset, R. P. Lin, R. P. Lepping, D. J. McComas, C. W. Smith, H. Reme and A. Balogh
Additional contact information
T. D. Phan: University of California
J. T. Gosling: University of Colorado
M. S. Davis: University of California
R. M. Skoug: Los Alamos National Laboratory, MS D466
M. Øieroset: University of California
R. P. Lin: University of California
R. P. Lepping: NASA/Goddard Space Flight Center
D. J. McComas: Southwest Research Institute
C. W. Smith: University of New Hampshire
H. Reme: Centre d'Etude Spatiale des Rayonnements
A. Balogh: Imperial College

Nature, 2006, vol. 439, issue 7073, 175-178

Abstract: Feel the Force Magnetic reconnection is a process in which pairs of magnetic field lines merge to convert magnetic energy into particle energy. Kinks formed in the merged field lines produce a slingshot effect that accelerates high-speed plasma jets away from the merger site. The process supplies energy to solar flares and the space storms near Earth that interfere with electric power grids and telecommunications. Space physicists have long debated whether reconnection occurs over great distances, or randomly in localized patches. On 2 February 2002, the Cluster, ACE and Wind spacecraft, widely separated in interplanetary space, all detected similar plasma jets within the same passing current sheet. It was direct evidence of a 2.5-million-kilometre reconnection region, confirming that magnetic reconnection can occur on a very large scale over long periods. On the cover, kinked magnetic field lines accelerate a pair of particle jets.

Date: 2006
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DOI: 10.1038/nature04393

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