Magnetic Reconnection Phenomena In Interplanetary Space |
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Authors: | Wei Fengsi Hu Qiang Feng Xueshang Fan Quanlin |
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Institution: | (1) Laboratory for Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, P.O. Box 8701, Beijing, 100080, China |
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Abstract: | Interplanetary magnetic reconnection(IMR) phenomena are explored based on the observational data with various time resolutions
from Helios, IMP-8, ISEE3, Wind, etc. We discover that the observational evidence of the magnetic reconnection may be found
in the various solar wind structures, such as at the boundary of magnetic cloud, near the current sheet, and small-scale turbulence
structures, etc. We have developed a third order accuracy upwind compact difference scheme to numerically study the magnetic
reconnection phenomena with high-magnetic Reynolds number (R
M=2000–10000) in interplanetary space. The simulated results show that the magnetic reconnection process could occur under
the typical interplanetary conditions. These obtained magnetic reconnection processes own basic characteristics of the high
R
M reconnection in interplanetary space, including multiple X-line reconnection, vortex velocity structures, filament current
systems, splitting, collapse of plasma bulk, merging and evolving of magnetic islands, and lifetime in the range from minutes
to hours, etc. These results could be helpful for further understanding the interplanetary basic physical processes.
This revised version was published online in August 2006 with corrections to the Cover Date. |
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Keywords: | interplanetary magnetic reconnection observational evidence numerical simulation |
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