Computer Modeling of Fast Collisionless Reconnection

  1. Edward W. Hones Jr.
  1. J. N. Leboeuf1,
  2. F. Brunel1,
  3. T. Tajima1,
  4. J. Sakai2,
  5. C. C. Wu3 and
  6. J. M. Dawson3

Published Online: 19 MAR 2013

DOI: 10.1029/GM030p0282

Magnetic Reconnection in Space and Laboratory Plasmas

Magnetic Reconnection in Space and Laboratory Plasmas

How to Cite

Leboeuf, J. N., Brunel, F., Tajima, T., Sakai, J., Wu, C. C. and Dawson, J. M. (2013) Computer Modeling of Fast Collisionless Reconnection, in Magnetic Reconnection in Space and Laboratory Plasmas (ed E. W. Hones), American Geophysical Union, Washington, D. C.. doi: 10.1029/GM030p0282

Author Information

  1. 1

    Institute for Fusion Studies, University of Texas, Austin, Texas 78712

  2. 2

    Department of Applied Mathematics and Physics, Faculty Of Engineering, Toyama University, Toyama 933, Japan

  3. 3

    Department of Physics, University Of California, Los Angeles, California 90024

Publication History

  1. Published Online: 19 MAR 2013
  2. Published Print: 1 JAN 1984

ISBN Information

Print ISBN: 9780875900582

Online ISBN: 9781118664223

SEARCH

Keywords:

  • Collisionless reconnection;
  • Computer model;
  • Magnetic configuration;
  • Magnetic reconnection;
  • Solar flares

Summary

Particle simulations of collisionless tearing, reconnection and coalescence of magnetic fields for a sheet-pinch configuration show that reconnection is Sweet-Parker like in the tearing and island formation phase. It is much faster, or even explosive, in the island coalescence stage. Island coalescence is the most energetic process and leads to large ion temperature increase and oscillations in the merged state. Similar phenomena have been observed in equivalent MHD simulations. Coalescence and its effects, as observed in our simulations, may explain many of the features of solar flares and coronal X-ray brightening.