### Abstract

We present a reconstruction technique to solve the steady resistive MHD equations in two dimensions with initial inputs of field and plasma data from a single spacecraft as it passes through a coherent structure in space. At least two components of directly measured electric fields (the spacecraft spin-plane components) are required for the reconstruction, to produce two-dimensional (2-D) field and plasma maps of the cross section of the structure. For convenience, the resistivity tensor η is assumed diagonal in the reconstruction coordinates, which allows its values to be estimated from Ohm's law, E + v × B = η · j. In the present paper, all three components of the electric field are used. We benchmark our numerical code by use of an exact, axi-symmetric solution of the resistive MHD equations and then apply it to synthetic data from a 3-D, resistive, MHD numerical simulation of reconnection in the geomagnetic tail, in a phase of the event where time dependence and deviations from 2-D are both weak. The resistivity used in the simulation is time-independent and localized around the reconnection site in an ellipsoidal region. For the magnetic field, plasma density, and pressure, we find very good agreement between the reconstruction results and the simulation, but the electric field and plasma velocity are not predicted with the same high accuracy.

Original language | English |
---|---|

Pages (from-to) | 2113-2125 |

Number of pages | 13 |

Journal | Annales Geophysicae |

Volume | 28 |

Issue number | 11 |

DOIs | |

Publication status | Published - 2010 |

Externally published | Yes |

### Fingerprint

### Keywords

- Magnetospheric physics (Magnetopause, cusp, and boundary layers)
- Space plasma physics (Magnetic reconnection; Numerical simulation studies)

### ASJC Scopus subject areas

- Earth and Planetary Sciences (miscellaneous)
- Atmospheric Science
- Astronomy and Astrophysics
- Space and Planetary Science
- Geology

### Cite this

*Annales Geophysicae*,

*28*(11), 2113-2125. https://doi.org/10.5194/angeo-28-2113-2010

**Resistive MHD reconstruction of two-dimensional coherent structures in space.** / Wai Leong, Teh; Sonnerup, B. U Ö; Birn, J.; Denton, R. E.

Research output: Contribution to journal › Article

*Annales Geophysicae*, vol. 28, no. 11, pp. 2113-2125. https://doi.org/10.5194/angeo-28-2113-2010

}

TY - JOUR

T1 - Resistive MHD reconstruction of two-dimensional coherent structures in space

AU - Wai Leong, Teh

AU - Sonnerup, B. U Ö

AU - Birn, J.

AU - Denton, R. E.

PY - 2010

Y1 - 2010

N2 - We present a reconstruction technique to solve the steady resistive MHD equations in two dimensions with initial inputs of field and plasma data from a single spacecraft as it passes through a coherent structure in space. At least two components of directly measured electric fields (the spacecraft spin-plane components) are required for the reconstruction, to produce two-dimensional (2-D) field and plasma maps of the cross section of the structure. For convenience, the resistivity tensor η is assumed diagonal in the reconstruction coordinates, which allows its values to be estimated from Ohm's law, E + v × B = η · j. In the present paper, all three components of the electric field are used. We benchmark our numerical code by use of an exact, axi-symmetric solution of the resistive MHD equations and then apply it to synthetic data from a 3-D, resistive, MHD numerical simulation of reconnection in the geomagnetic tail, in a phase of the event where time dependence and deviations from 2-D are both weak. The resistivity used in the simulation is time-independent and localized around the reconnection site in an ellipsoidal region. For the magnetic field, plasma density, and pressure, we find very good agreement between the reconstruction results and the simulation, but the electric field and plasma velocity are not predicted with the same high accuracy.

AB - We present a reconstruction technique to solve the steady resistive MHD equations in two dimensions with initial inputs of field and plasma data from a single spacecraft as it passes through a coherent structure in space. At least two components of directly measured electric fields (the spacecraft spin-plane components) are required for the reconstruction, to produce two-dimensional (2-D) field and plasma maps of the cross section of the structure. For convenience, the resistivity tensor η is assumed diagonal in the reconstruction coordinates, which allows its values to be estimated from Ohm's law, E + v × B = η · j. In the present paper, all three components of the electric field are used. We benchmark our numerical code by use of an exact, axi-symmetric solution of the resistive MHD equations and then apply it to synthetic data from a 3-D, resistive, MHD numerical simulation of reconnection in the geomagnetic tail, in a phase of the event where time dependence and deviations from 2-D are both weak. The resistivity used in the simulation is time-independent and localized around the reconnection site in an ellipsoidal region. For the magnetic field, plasma density, and pressure, we find very good agreement between the reconstruction results and the simulation, but the electric field and plasma velocity are not predicted with the same high accuracy.

KW - Magnetospheric physics (Magnetopause, cusp, and boundary layers)

KW - Space plasma physics (Magnetic reconnection; Numerical simulation studies)

UR - http://www.scopus.com/inward/record.url?scp=78649438788&partnerID=8YFLogxK

UR - http://www.scopus.com/inward/citedby.url?scp=78649438788&partnerID=8YFLogxK

U2 - 10.5194/angeo-28-2113-2010

DO - 10.5194/angeo-28-2113-2010

M3 - Article

AN - SCOPUS:78649438788

VL - 28

SP - 2113

EP - 2125

JO - Annales Geophysicae

JF - Annales Geophysicae

SN - 0992-7689

IS - 11

ER -