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Evolution of flux ropes in the magnetotail: A three-dimensional global hybrid simulation
Lu, S.; Lin, Y.; Lu, Q. M.; Wang, X. Y.; Wang, R. S.; Huang, C.; Wu, M. Y.; Wang, S.; Lu, QM (reprint author), Univ Sci & Technol China, Dept Geophys & Planetary Sci, CAS Key Lab Geospace Environm, Hefei 230026, Peoples R China.
Department空间科学部
Source PublicationPHYSICS OF PLASMAS
2015
Volume22Issue:5Pages:52901
ISSN1070-664X
Language英语
AbstractFlux ropes in the Earth's magnetotail are widely believed to play a crucial role in energy transport during substorms and the generation of energetic particles. Previous kinetic simulations are limited to the local-scale regime, and thus cannot be used to study the structure associated with the geomagnetic field and the global-scale evolution of the flux ropes. Here, the evolution of flux ropes in the magnetotail under a steady southward interplanetary magnetic field are studied with a newly developed three-dimensional global hybrid simulation model for dynamics ranging from the ion Larmor radius to the global convection time scales. Magnetic reconnection with multiple X-lines is found to take place in the near-tail current sheet at geocentric solar magneto-spheric distances x = -30R(E) similar to -15R(E) around the equatorial plane (z = 0). The magnetotail reconnection layer is turbulent, with a nonuniform structure and unsteady evolution, and exhibits properties of typical collisionless fast reconnection with the Hall effect. A number of small-scale flux ropes are generated through the multiple X-line reconnection. The diameter of the flux ropes is several R-E, and the spatial scale of the flux ropes in the dawn-dusk direction is on the order of several R-E and does not extend across the entire section of the magnetotail, contrary to previous models and MHD simulation results and showing the importance of the three-dimensional effects. The nonuniform and unsteady multiple X-line reconnection with particle kinetic effects leads to various kinds of flux rope evolution: The small-scale flux ropes propagate earthward or tailward after formation, and eventually merge into the near-Earth region or the mid-/distant-tail plasmoid, respectively. During the propagation, some of the flux ropes can be tilted in the geocentric solar magnetospheric (x, y) plane with respect to the y (dawn-dusk) axis. Coalescence between flux ropes is also observed. At the same time, the evolution of the flux ropes in the multiple X-line reconnection layer can also lead to the acceleration and heating of ions. (C) 2015 AIP Publishing LLC.
Indexed BySCI ; EI
Document Type期刊论文
Identifierhttp://ir.nssc.ac.cn/handle/122/4596
Collection空间科学部
Corresponding AuthorLu, QM (reprint author), Univ Sci & Technol China, Dept Geophys & Planetary Sci, CAS Key Lab Geospace Environm, Hefei 230026, Peoples R China.
Recommended Citation
GB/T 7714
Lu, S.,Lin, Y.,Lu, Q. M.,et al. Evolution of flux ropes in the magnetotail: A three-dimensional global hybrid simulation[J]. PHYSICS OF PLASMAS,2015,22(5):52901.
APA Lu, S..,Lin, Y..,Lu, Q. M..,Wang, X. Y..,Wang, R. S..,...&Lu, QM .(2015).Evolution of flux ropes in the magnetotail: A three-dimensional global hybrid simulation.PHYSICS OF PLASMAS,22(5),52901.
MLA Lu, S.,et al."Evolution of flux ropes in the magnetotail: A three-dimensional global hybrid simulation".PHYSICS OF PLASMAS 22.5(2015):52901.
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