The Magnetic Topology of the Plasmoid Flux Rope in a MHD-Simulation of Magnetotail Reconnection

  1. C. T. Russell,
  2. E. R. Priest and
  3. L. C. Lee
  1. J. Birn and
  2. M. Hesse

Published Online: 21 MAR 2013

DOI: 10.1029/GM058p0655

Physics of Magnetic Flux Ropes

Physics of Magnetic Flux Ropes

How to Cite

Birn, J. and Hesse, M. (1990) The Magnetic Topology of the Plasmoid Flux Rope in a MHD-Simulation of Magnetotail Reconnection, in Physics of Magnetic Flux Ropes (eds C. T. Russell, E. R. Priest and L. C. Lee), American Geophysical Union, Washington, D. C.. doi: 10.1029/GM058p0655

Author Information

  1. University of California, Los Alamos National Laboratory, Los Alamos, NM 87545

Publication History

  1. Published Online: 21 MAR 2013
  2. Published Print: 1 JAN 1990

ISBN Information

Print ISBN: 9780875900261

Online ISBN: 9781118663868

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Keywords:

  • Solar photosphere;
  • Magnetic flux;
  • Astrophysics

Summary

On the basis of a three-dimensional MHD simulation we discuss the magnetic topology of a plasmoid that forms by a localized reconnection process in a magnetotail configuration including a net dawn-dusk magnetic field component ByN . As a consequence of ByN ≠ 0 the plasmoid assumes a helical flux rope structure rather than an isolated island or bubble structure. Initially all field lines of the plasmoid flux rope remain connected with the Earth, while at later times a gradually increasing amount of flux tubes becomes separated, connecting to either the distant boundary or to the flank boundaries. In this stage topologically different flux tubes become tangled and wrapped around each other, consistent with predictions on the basis of an ad-hoc plasmoid model.