Magnetic field reconnection theory and the solar wind ? Magnetosphere interaction: A review

Pudovkin, M. I.; Semenov, V. S.

doi:10.1007/bf00241346

Cited by 91 publications

(44 citation statements)

References 72 publications

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“…It has to be remembered here that the model presented is based on the supposition on the subsolar point reconnection, and as this takes place most probably for jHj b 50 (Pudovkin and Semenov, 1989), the model may be inadequate for cases with extremely northward IMF.…”

Section: Discussionmentioning

confidence: 99%

Magnetopause stand-off distance in dependence on the magnetosheath and solar wind parameters

1998

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Abstract. A model of the magnetosheath structure proposed in a recent paper from the authors is extended to estimate the magnetopause stand-o distance from solar wind data. For this purpose, the relationship of the magnetopause location to the magnetosheath and solar wind parameters is studied. It is shown that magnetopause erosion may be explained in terms of the magnetosheath magnetic ®eld penetration into the magnetosphere. The coecient of penetration (the ratio of the magnetospheric magnetic ®eld depression to the intensity of the magnetosheath magnetic ®eld f mcz Àf m sin 2 Ha2, is estimated and found approximately to equal 1. It is shown that having combined a magnetosheath model presented in an earlier paper and the magnetosheath ®eld penetration model presented in this paper, it is possible to predict the magnetopause stand-o distance from solar wind parameters.

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Section: Discussionmentioning

confidence: 99%

Magnetopause stand-off distance in dependence on the magnetosheath and solar wind parameters

1998

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“…Since the leading part of the string develops a loop, which gives rise to an antiparallel magnetic field configuration (see Figure 2), it would seem natural to suggest that reconnection could fulfill the role of this additional process. Reconnection is able to cut the fragment of the tube with negative energy, which corresponds to this loop, and thus release stresses which are building up, similar to what happens in current sheet configurations in the magnetospheric and solar context [5,18,19]. In the case of the solar-terrestrial interaction, …”

Section: Test Particle -Flux Tube Comparisonmentioning

confidence: 88%

“…Our conclusion is based on the investigation of the Earth's magnetosphere, where we have the benefit of direct spacecraft measurements. It turns out that the energy of the magnetospheric substorm comes from the magnetic energy stored in the magnetotail which is released in an explosive way by virtue of reconnection producing narrow flows of accelerating plasma [18]. The reconnection events at the magnetopause [18,20] (boundary of the magnetosphere) and solar flares [19] present other examples of this exlosive energy release, when magnetic energy is first accumulated and then reconnection converts it into kinetic and internal energy to produce jets of accelerated plasma.…”

Section: Discussionmentioning

confidence: 99%

Energy Confinement for a Relativistic Magnetic Flux Tube in the Ergosphere of a Kerr Black Hole

et al. 2002

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In the MHD description of plasma phenomena the concept of magnetic field lines frozen into the plasma turns out to be very useful. We present here a method of introducing Lagrangian coordinates into relativistic MHD equations in general relativity, which enables a convenient mathematical formulation for the behaviour of flux tubes. With the introduction of these Lagrangian, so-called "frozen-in" coordinates, the relativistic MHD equations reduce to a set of nonlinear 1D string equations, and the plasma may therefore be regarded as a gas of nonlinear strings corresponding to flux tubes. Numerical simulation shows that if such a tube/string falls into a Kerr black hole, then the leading portion loses angular momentum and energy as the string brakes, and to compensate for this loss, momentum and energy is radiated to infinity to conserve energy and momentum for the tube. Inside the ergosphere the energy of the leading part turns out to be negative after some time, and the rest of the tube then gets energy from the hole. In our simulations most of the compensated positive energy is also localized inside the ergosphere because 1 the inward speed of the plasma is approximately equal to the velocity of the MHD wave which transports energy outside. Therefore, an additional physical process has to be included which can remove energy from the ergophere.Magnetic reconnection seems fills this role releasing Maxwellian stresses and producing a relativistic jet.

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“…Therefore, most of the coordinate systems (Pudovkin and Semenov, 1985;Pustovitov, 1999) based on Euler potentials (4), such as the helicity system (34), can also still be applied to magnetic structures with non-zero helicity K = 0. On the other hand, one has to be particularly careful with the vector potential.…”

Section: Discussion and Summarymentioning

confidence: 99%

Euler potentials for the MHD Kamchatnov-Hopf soliton solution

Семенов

Korovinski

Biernat

2002

Nonlin. Processes Geophys.

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Abstract. In the MHD description of plasma phenomena the concept of magnetic helicity turns out to be very useful. We present here an example of introducing Euler potentials into a topological MHD soliton which has non-trivial helicity. The MHD soliton solution (Kamchatnov, 1982) is based on the Hopf invariant of the mapping of a 3-D sphere into a 2-D sphere; it can have arbitrary helicity depending on control parameters. It is shown how to define Euler potentials globally. The singular curve of the Euler potential plays the key role in computing helicity. With the introduction of Euler potentials, the helicity can be calculated as an integral over the surface bounded by this singular curve. A special programme for visualization is worked out. Helicity coordinates are introduced which can be useful for numerical simulations where helicity control is needed.

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Magnetic field reconnection theory and the solar wind ? Magnetosphere interaction: A review

Cited by 91 publications

References 72 publications

Magnetopause stand-off distance in dependence on the magnetosheath and solar wind parameters

Magnetopause stand-off distance in dependence on the magnetosheath and solar wind parameters

Energy Confinement for a Relativistic Magnetic Flux Tube in the Ergosphere of a Kerr Black Hole

Euler potentials for the MHD Kamchatnov-Hopf soliton solution

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