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

Author

Listed:
  • 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)

  • M. B. Bavassano-Cattaneo
  • 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
    Institute of Space Sciences)

  • 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)

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.

Suggested Citation

  • 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, 2000. "Extended magnetic reconnection at the Earth's magnetopause from detection of bi-directional jets," Nature, Nature, vol. 404(6780), pages 848-850, April.
    • Handle: RePEc:nat:nature:v:404:y:2000:i:6780:d:10.1038_35009050
    DOI: 10.1038/35009050
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