A Three-Dimensional MHD Simulation of the Multiple X Line Reconnection Process

  1. C. T. Russell,
  2. E. R. Priest and
  3. L. C. Lee
  1. Z. F. Fu1,
  2. L. C. Lee2 and
  3. Y. Shi2

Published Online: 21 MAR 2013

DOI: 10.1029/GM058p0515

Physics of Magnetic Flux Ropes

Physics of Magnetic Flux Ropes

How to Cite

Fu, Z. F., Lee, L. C. and Shi, Y. (1990) A Three-Dimensional MHD Simulation of the Multiple X Line Reconnection Process, 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/GM058p0515

Author Information

  1. 1

    Center for Space Science and Applied Research, Academia Sinica, P.O. Box 8701, Beijing, China

  2. 2

    Geophysical Institute and Department of Physics, University of Alaska, Fairbanks, AK 99775

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

The multiple X line reconnection (MXR) process is studied through a 3-dimensional incompressible MHD simulation. The simulation is conducted in a local rectangular box for which a constant plasma flow and magnetic inflow flux are maintained on the two plasma incoming boundaries. Reconnection takes place under such driven boundary conditions.

Magnetic reconnections at multiple sites are observed. As the reconnections proceed, several magnetic flux tubes are formed and convected outward after growing to a large size. Tube-aligned plasma flows are observed inside the moving magnetic flux tubes. As reconnection proceeds, the active reconnection regions shift towards the ends of the reconnection lines. Of the most importance is the field line topology revealed at the two ends of the flux tube. The simulation shows that the magnetic ropes usually have “frayed” ends.