Extended magnetic reconnection at the Earth's magnetopause from detection of bi-directional jets

T. D. Phan (), L. M. Kistler, B. Klecker, G. Haerendel, G. Paschmann, B. U. Ö. Sonnerup, W. Baumjohann, M. B. Bavassano-Cattaneo, C. W. Carlson, A. M. DiLellis, K.-H. Fornacon, L. A. Frank, M. Fujimoto, E. Georgescu, S. Kokubun, E. Moebius, T. Mukai, M. Øieroset, W. R. Paterson and H. Reme
Additional contact information
T. D. Phan: Space Sciences Laboratory, University of California
L. M. Kistler: Space Science Center, University of New Hampshire
B. Klecker: Max-Planck-Institut für Extraterrestrische Physik
G. Haerendel: Max-Planck-Institut für Extraterrestrische Physik
G. Paschmann: Max-Planck-Institut für Extraterrestrische Physik
B. U. Ö. Sonnerup: Thayer School of Engineering, Dartmouth College
W. Baumjohann: Max-Planck-Institut für Extraterrestrische Physik
C. W. Carlson: Space Sciences Laboratory, University of California
A. M. DiLellis: IFSI-CNR
K.-H. Fornacon: Technische Universität Braunschweig
L. A. Frank: University of Iowa
M. Fujimoto: Tokyo Institute of Technology
E. Georgescu: Max-Planck-Institut für Extraterrestrische Physik
S. Kokubun: Solar-Terrestrial Environment Laboratory, Nagoya University
E. Moebius: Space Science Center, University of New Hampshire
T. Mukai: The Institute of Space and Astronautical Science
M. Øieroset: Space Sciences Laboratory, University of California
W. R. Paterson: University of Iowa
H. Reme: Centre d'Etude Spatiale des Rayonnements, Université Paul Sabatier

Nature, 2000, vol. 404, issue 6780, 848-850

Abstract: Abstract Magnetic reconnection is a process that converts magnetic energy into bi-directional plasma jets; it is believed to be the dominant process by which solar-wind energy enters the Earth's magnetosphere1,2. This energy is subsequently dissipated by magnetic storms and aurorae3,4. Previous single-spacecraft observations5,6,7 revealed only single jets at the magnetopause—while the existence of a counter-streaming jet was implicitly assumed, no experimental confirmation was available. Here we report in situ two-spacecraft observations of bi-directional jets at the magnetopause, finding evidence for a stable and extended reconnection line; the latter implies substantial entry of the solar wind into the magnetosphere. We conclude that reconnection is determined by large-scale interactions between the solar wind and the magnetosphere, rather than by local conditions at the magnetopause.

Date: 2000
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DOI: 10.1038/35009050

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