Transport of solar wind into Earth's magnetosphere through rolled-up Kelvin–Helmholtz vortices

H. Hasegawa (), M. Fujimoto, T.-D. Phan, H. Rème, A. Balogh, M. W. Dunlop, C. Hashimoto and R. TanDokoro
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H. Hasegawa: Dartmouth College
M. Fujimoto: Tokyo Institute of Technology
T.-D. Phan: University of California
H. Rème: Centre d'Etude Spatiale des Rayonnements
A. Balogh: Imperial College
M. W. Dunlop: Rutherford Appleton Laboratory
C. Hashimoto: Tokyo Institute of Technology
R. TanDokoro: Tokyo Institute of Technology

Nature, 2004, vol. 430, issue 7001, 755-758

Abstract: Abstract Establishing the mechanisms by which the solar wind enters Earth's magnetosphere is one of the biggest goals of magnetospheric physics, as it forms the basis of space weather phenomena such as magnetic storms and aurorae1. It is generally believed that magnetic reconnection is the dominant process, especially during southward solar-wind magnetic field conditions when the solar-wind and geomagnetic fields are antiparallel at the low-latitude magnetopause2. But the plasma content in the outer magnetosphere increases during northward solar-wind magnetic field conditions3,4, contrary to expectation if reconnection is dominant. Here we show that during northward solar-wind magnetic field conditions—in the absence of active reconnection at low latitudes—there is a solar-wind transport mechanism associated with the nonlinear phase of the Kelvin–Helmholtz instability5. This can supply plasma sources for various space weather phenomena.

Date: 2004
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DOI: 10.1038/nature02799

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