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Annales Geophysicae An interactive open-access journal of the European Geosciences Union
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Volume 27, issue 2 | Copyright
Ann. Geophys., 27, 807-822, 2009
https://doi.org/10.5194/angeo-27-807-2009
© Author(s) 2009. This work is distributed under
the Creative Commons Attribution 3.0 License.

  18 Feb 2009

18 Feb 2009

Reconstruction of a large-scale reconnection exhaust structure in the solar wind

W.-L. Teh1, B. U. Ö. Sonnerup1, Q. Hu2, and C. J. Farrugia3 W.-L. Teh et al.
  • 1Thayer School of Engineering, Dartmouth College, NH, USA
  • 2Institute of Geophysics and Planetary Physics, UCR, CA, USA
  • 3Institute for the Study of Earth, Ocean, and Space, UNH, NH, USA

Abstract. We recover two-dimensional (2-D) magnetic field and flow field configurations from three spacecraft encounters with a single large-scale reconnection exhaust structure in the solar wind, using a new reconstruction method (Sonnerup and Teh, 2008) based on the ideal single-fluid MHD equations in a steady-state, 2-D geometry. The reconstruction is performed in the rest frame of the X-line, where the flow into, and the plasma jetting within, the exhaust region are clearly visible. The event was first identified by Phan et al. (2006) in the ACE, Cluster, and Wind data sets; they argued that quasi-steady reconnection persisted for over 2 h at a long (390 RE) X-line. The reconnection exhaust is sandwiched between two discontinuities, both of which contain elements of intermediate- and slow-mode behavior; these elements are co-located rather than being spatially separated. These composite discontinuities do not satisfy the coplanarity condition or the standard MHD jump conditions. For all three spacecraft, the Walén regression line slope was positive (negative) for the leading (trailing) discontinuity. Our MHD reconstruction shows that: (1) the X-line orientation was close to the bisector of the overall magnetic shear angle and exhibited a slow rotating motion toward the Sun-Earth line; (2) the X-line moved earthward, dawnward, and southward; (3) the reconnection electric field was small (~0.02 mV/m on average) and gradually decreased from the first crossing (ACE) to the last (Wind). The magnetic field and flow field configurations recovered from ACE and Cluster are similar while those recovered from Wind also include a magnetic island and an associated vortex. Reconnection persisted for at least 2.4 h involving inflow into the exhaust region from its two sides. Time-dependence in the reconnection electric fields seen by ACE and Wind indicates local temporal variations in the field configuration. In addition to the reconstruction results, we provide a description and analysis of many details from the crossings by the spacecraft.

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