Inertial-Range Reconnection in Magnetohydrodynamic Turbulence and in the Solar Wind.

@article{Lalescu2015InertialRangeRI,
  title={Inertial-Range Reconnection in Magnetohydrodynamic Turbulence and in the Solar Wind.},
  author={Cristian Constantin Lalescu and Yi-kang Shi and Gregory L. Eyink and Theodore D. Drivas and Ethan T. Vishniac and Alex Lazarian},
  journal={Physical review letters},
  year={2015},
  volume={115 2},
  pages={
          025001
        }
}
In situ spacecraft data on the solar wind show events identified as magnetic reconnection with wide outflows and extended "X lines," 10(3)-10(4) times ion scales. To understand the role of turbulence at these scales, we make a case study of an inertial-range reconnection event in a magnetohydrodynamic simulation. We observe stochastic wandering of field lines in space, breakdown of standard magnetic flux freezing due to Richardson dispersion, and a broadened reconnection zone containing many… 

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References

SHOWING 1-10 OF 18 REFERENCES

Magnetic Reconnection: MHD Theory and Applications

Preface 1. Introduction 2. Current-sheet formation 3. Magnetic annihilation 4. Steady reconnection: the classical solutions 5. Steady reconnection: new generation of fast regimes 6. Unsteady

Geophys

  • Res. Lett. 36, L09108
  • 2009

Phys

  • Rev. Lett. 112, 215002
  • 2014

Astrophys

  • J. 517, 700
  • 1999

Astrophys

  • J. 660, 863
  • 2007

Physica D 223

  • 82
  • 2006

Astrophys

  • J 700, 63
  • 2009

Astrophys

  • J. 743, 51
  • 2011

Astrophys

  • J. 726, 90
  • 2011

Eyink, ArXiv e-prints (2014), arXiv:1412.2254 [astro-ph.SR

  • 2014