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New Evidence for Magnetic Reconnection in the Tail of Interplanetary Magnetic Cloud |
| ZHONG Ding-Kun1,2;WEI Feng-Si1;FENG Xue-Shang1;YANG Fang1,2 |
| 1Key Laboratory of Space Weather, Center for Space Science and Applied Research, Chinese Academy of Sciences, Beijing 100080
2Graduate School of the Chinese Academy of Sciences, Beijing 100080 |
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| Cite this article: |
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ZHONG Ding-Kun, WEI Feng-Si, FENG Xue-Shang et al 2005 Chin. Phys. Lett. 22 3225-3228 |
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Abstract We analyse the WIND data of an interplanetary magnetic cloud (MC) on 2 November 2001, and find new evidences for magnetic reconnection in the tail of this MC. In the MC tail, the largely dip and the large change of the orientation of the magnetic field occurred simultaneously, Δθ approx 45°, and ΔФ changed from 90° to 320°. Correspondingly, the number density of ions increased, and the superthermal electrons were heated and accelerated, however its number density decreased. Meanwhile, inverse jets and Hall term were observed. The pitch-angle distributions of the electrons with lower energy and higher energy showed strong turbulence and bi-direction flow, respectively. The plasma wave activity enhanced near the electron plasma frequency, fpe and 2fpe. These important physical characteristics are new evidences for magnetic reconnection existing in interplanetary space.
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| Keywords:
96.50.Bh
96.50.Ci
96.50.Ry
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Published: 01 December 2005
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| PACS: |
96.50.Bh
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(Interplanetary magnetic fields)
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96.50.Ci
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(Solar wind plasma; sources of solar wind)
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96.50.Ry
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(Discontinuities)
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