Hall Magnetic Reconnection Rate

Huba, J. D.; Rudakov, L. I.

doi:10.1103/physrevlett.93.175003

Cited by 93 publications

(90 citation statements)

References 16 publications

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“…The fraction that reconnect, and end up in the earth's magnetotail, is controlled by the reconnection rate. Assuming this is the Sweet-Parker rate, approximately one in a hundred thousand lines reconnect as opposed to the measured value of one in ten (Hughes, 1995). The predictions of Sweet-Parker strikingly disagree with the observations.…”

Section: A Early History Of Magnetic Reconnection Theorycontrasting

confidence: 44%

“…The magnetopause is the boundary that separates the geomagnetic field and plasma of terrestrial origin from the solar wind plasma (Hughes, 1995). Figure 8 is a schematic of the magnetosphere showing it on both the dayside and night side.…”

Section: B Magnetic Reconnection In the Magnetospherementioning

confidence: 99%

“…The energy and plasma in these magnetotails are intermittently released into the inner magnetosphere during the magnetic substorms. It is generally believed that, during a substorm, solar wind plasma and energy are injected into the magnetosphere and then released from it through magnetic reconnection processes (Hughes, 1995).…”

Section: B Magnetic Reconnection In the Magnetospherementioning

confidence: 99%

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Magnetic Reconnection

Yamada¹

2009

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We review the fundamental physics of magnetic reconnection in laboratory and space plasmas, by discussing results from theory, numerical simulations, observations from space satellites, and the recent results from laboratory plasma experiments. After a brief review of the well-known early work, we discuss representative recent experimental and theoretical work and attempt to interpret the essence of significant modern findings. In the area of local reconnection physics, many significant findings have been made with regard to two-fluid physics and are related to the cause of fast reconnection. Profiles of the neutral sheet, Hall currents, and the effects of guide field, collisions, and micro-turbulence are discussed to understand the fundamental processes in a local reconnection layer both in space and laboratory plasmas. While the understanding of the global reconnection dynamics is less developed, notable findings have been made on this issue through detailed documentation of magnetic self-organization phenomena in fusion plasmas. Application of magnetic reconnection physics to astrophysical plasmas is also briefly discussed.

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Section: A Early History Of Magnetic Reconnection Theorycontrasting

confidence: 44%

Section: B Magnetic Reconnection In the Magnetospherementioning

confidence: 99%

Section: B Magnetic Reconnection In the Magnetospherementioning

confidence: 99%

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Magnetic Reconnection

Yamada¹

2009

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“…For the three initial magnetic field configurations adopted here, both the magnetic structure and the magnetic energy spectrum have not revealed any significant difference between the low and high ␤ regime. It has been shown that Hall physics is an important ingredient in the development of fast reconnection [42][43][44][45][46][47][48][49][50][51][52] and can have an influence on the linear and nonlinear evolution of the tearing instability. 42,53,54 Future work will include the Hall effect in studying the dynamical evolution of the current sheet.…”

Section: -12mentioning

confidence: 99%

Three-dimensional simulations of compressible tearing instability

et al. 2008

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Three-dimensional numerical simulations of the tearing instability in the framework of compressible and resistive magnetohydrodynamics are presented. Simulations have been performed with a novel Eulerian conservative high order code, including an explicit resistivity, which uses implicit high order numerical schemes having higher spectral resolution than classical schemes. The linear and non linear evolution of the tearing instability has been followed for force-free and pressure-balanced initial equilibrium configurations. Pressure equilibrium configurations are subject to a secondary instability which drives the system toward a quasi two dimensional structure oriented perpendicularly to the initial configuration. The development of secondary instabilities is suppressed by a guide field allowing the coalescence instability to fully develop in the system. Force-free initial configurations follow an intermediate path with respect the previous cases: Strong coalescence of magnetic islands, due to the non linear evolution of the tearing instability, is observed before the system enters in a phase dominated by 3D modes. The histories of the differing initial current-sheet equilibria have counterparts in the energy spectra that, for all three cases, are observed to be strongly anisotropic.

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“…The influence of the Hall physics on the reconnection dynamics has been shown in several studies to be dependent on the relation between the Hall parameter c H and the inverse of the Lundqvist number L u . 5,8,22,6 Especially when c H 2 Ͼ L u −1 , the Hall effect has been shown to dominate significantly. It is also shown that the inclusion of the Hall term brings the dynamics of Whistler waves into the system.…”

Section: Discussionmentioning

confidence: 99%

Hall effects on the steady structure of the rotational layer at the dayside magnetopause

Westerberg

Åkerstedt

2007

Physics of Plasmas

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The influence of the Hall term in the generalized Ohm's law on the large-scale plasma flow during conditions of ongoing magnetic reconnection at the dayside magnetopause ͑MP͒ is investigated. Of special interest is the plasma flow behavior during the transition of the MP transition layer as the Hall effect grows in proportion to the viscous-resistive effects. The governing equations are solved approximately by an ordinary perturbation expansion in orders of large Reynolds and Lundqvist numbers. It is shown that the flow pattern is strongly dependent on the magnitude of the Hall parameter; as it approaches zero, the viscous-resistive solution is obtained, while for an ordering of the same magnitude as the resistivity/viscosity, the Hall effect begins to affect the flow structure severely. For an increasing value on the Hall parameter, oscillations are brought into the system, an effect that is enhanced with the magnitude of the Hall parameter. Furthermore, it is shown that as the Hall effect begins to dominate, the transition layer thickens.

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Hall Magnetic Reconnection Rate

Cited by 93 publications

References 16 publications

Magnetic Reconnection

Magnetic Reconnection

Three-dimensional simulations of compressible tearing instability

Hall effects on the steady structure of the rotational layer at the dayside magnetopause

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