<i>MHD Instabilities</i>

Bateman, G.; Grimm, R.C.

doi:10.1063/1.2995243

Cited by 161 publications

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“…(6), (7)) becomes impossible. The plasma filament can now deviate from the magnetic field lines, the effect that can be called "resistive ballooning" (e.g., [13]). In the frame co-moving with the plasma filament, there will appear a time-varying magnetic field threading the flux tube in the direction perpendicular to the flux tube.…”

Section: Resistive Ballooningmentioning

confidence: 99%

The dynamics of an isolated plasma filament at the edge of a toroidal device

Ryutov

2006

Physics of Plasmas

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The dynamics of an isolated plasma filament (an isolated blob) in the far scrape-off layer (SOL) of a toroidal device is described, with a proper averaging of the geometrical parameters as well as plasma parameters along the filament. The analysis is limited to the magnetohydrodynamic description. The effects of the electrical contact of the filament end with the limiter and of the finite plasma resistivity are also discussed.

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Section: Resistive Ballooningmentioning

confidence: 99%

The dynamics of an isolated plasma filament at the edge of a toroidal device

Ryutov

2006

Physics of Plasmas

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“…The threshold is reached when the magnitude of magnetic fields of the overlying arcades decrease faster with height than the magnetic pressure which pushes the flux rope upwards, which also decreases with time during the rise of the flux rope. The process was first proposed by van Tend & Kuperus (1978), and it was shown by to correspond to the "torus instability" first proposed by Bateman (1978) in tokamaks, and first revisited for solar eruptions by Kliem & Török (2006).…”

Section: Discussionmentioning

confidence: 99%

“…The stability properties of the modeled systems were analyzed, in pretty much the same way as in the electric-wire models. Equilibrium curves were identified, and the lack of existing solutions were found for specific parameters, in particular for strong axial fields and when thermal pressure was taken into account (Low 1977;Birn et al 1978;Heyvaerts et al 1982;Zwingmann 1987).…”

Section: Axial Flux Increasementioning

confidence: 99%

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The physical mechanisms that initiate and drive solar eruptions

Aulanier

2013

Proc. IAU

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Abstract. Solar eruptions are due to a sudden destabilization of force-free coronal magnetic fields. But the detailed mechanisms which can bring the corona towards an eruptive stage, then trigger and drive the eruption, and finally make it explosive, are not fully understood. A large variety of storage-and-release models have been developed and opposed to each other since 40 years. For example, photospheric flux emergence vs. flux cancellation, localized coronal reconnection vs. large-scale ideal instabilities and loss of equilibria, tether-cutting vs. breakout reconnection, and so on. The competition between all these approaches has led to a tremendous drive in developing and testing all these concepts, by coupling state-of-the-art models and observations. Thanks to these developments, it now becomes possible to compare all these models with one another, and to revisit their interpretation in light of their common and their different behaviors. This approach leads me to argue that no more than two distinct physical mechanisms can actually initiate and drive prominence eruptions: the magnetic breakout and the torus instability. In this view, all other processes (including flux emergence, flux cancellation, flare reconnection and long-range couplings) should be considered as various ways that lead to, or that strengthen, one of the aforementioned driving mechanisms.

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“…4. Growth of MHD perturbations is described by the tearing mode equation [16]: dW m =dt 1:2= 0 0 m , where, 0 m is the stability parameter, is the plasma resistivity, dW m is the width of the magnetic island, dW m 4B r r s R 0 =nsB t 1=2 , r s is the radius of the magnetic surface, B r is the radial magnetic field perturbations, and s is the magnetic shear. (For simplicity, effects of the ''neoclassical'' bootstrap currents and ion polarization flows are not considered in the present analysis of T-10 experiments with low magnetohydrodynamic pressure.)…”

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confidence: 99%

Quasicoherent Oscillations Induced by Nonthermal Electrons during Magnetic Reconnection in the T-10 Tokamak

Savrukhin

Волков

2004

Phys. Rev. Lett.

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Small-scale quasicoherent oscillations of the x-ray emissivity and magnetic field perturbations are observed in the T-10 tokamak during abrupt growth of the m=2, n=1 magnetohydrodynamic modes at the density limit disruption. Analysis indicates a possible link between the small-scale oscillations and nonthermal electron beams induced around the X points of the m=2, n=1 magnetic island during reconnection of magnetic field lines at the disruption instability.

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MHD Instabilities

Cited by 161 publications

References 0 publications

The dynamics of an isolated plasma filament at the edge of a toroidal device

The dynamics of an isolated plasma filament at the edge of a toroidal device

The physical mechanisms that initiate and drive solar eruptions

Quasicoherent Oscillations Induced by Nonthermal Electrons during Magnetic Reconnection in the T-10 Tokamak

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