Mechanism for Major Disruptions in Tokamaks

Waddell, B. V.; Carreras, B. A.; Hicks, H.R.; Holmes, J. A.; Lee, D. K.

doi:10.1103/physrevlett.41.1386

Cited by 118 publications

(69 citation statements)

References 10 publications

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“…These modes, although more sensitive to profile and slower growing, can terminate the discharge by means of a "major disruption" before the current can be increased above the Kruskal-Shafranov limit. [For a theoretical discussion of major disruptions, see Waddell et al (1978Waddell et al ( , 1979, Bateman (1978), and Hicks et al (1980) Shafranov (1970) first pointed out that this pessimistic result is strongly dependent upon the shape of the current profile. He showed both analytically and numerically that for more realistic profiles, where the current goes smoothly to zero at the plasma surface, the stability prop-In general the m )2 external kinks impose more stringent conditions on q(a) and the current profile than those corresponding to the m = 1 mode.…”

Section: Consider First Suydam's Criterionmentioning

confidence: 99%

Ideal magnetohydrodynamic theory of magnetic fusion systems

1982

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Ideal magnetohydrodynamic theory and its apphcation to magnetic fusion systems are reviewed. The review begins with a description and derivation of the model as well as a discussion of the region of validity. Next, the general properties are derived which are valid for arbitrary geometry and demonstrate the inherently sound physical foundation of the model. The equilibrium behavior of the currently most promising toroidal magnetic fusion concepts are then discussed in detail. Finally, the stability of such equilibria is investigated. Included are discussions of the general stability properties of arbitrary magnetic geometries and of detailed applications to those concepts of current fusion interest. CONTENTS

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Section: Consider First Suydam's Criterionmentioning

confidence: 99%

Ideal magnetohydrodynamic theory of magnetic fusion systems

1982

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“…The eruption is sometimes preceded by preheating (Webb et al, 1976;Schmahl et aI., 1986), mass outflow through the legs (Rust, Nakagawa and Neupert, 1975;Vrgnak et al, 1987), or by the photospheric magnetic field reorganization such as emerging flux, moving pores, flux cancellation, etc. (Schmieder, 1990).…”

Section: Introductionmentioning

confidence: 99%

Eruptive instability of cylindrical prominences

Vršnak¹

1990

Sol Phys

109

101

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The stability of prominences and the dynamics of an eruption are studied. The prominence is represented by an uniformly twisted, curved, magnetic tube, anchored at both ends in the photosphere. Several stages of the eruption are analyzed, from the pre-eruptive phase and the onset of the instability, up to the late phases of the process. Before the eruption, the prominence evolves through a series of equilibrium states, slowly ascending either due to an increase of the electric current or to mass loss. The eruption starts when the ratio of the current to the total mass attains a critical value after which no neighbouring equilibrium exists. The linearized equation of motion was used to obtain the instability threshold, which is presented in a form enabling comparison with the observations. The height at which the prominence erupts depends on the twist, and is typically comparable with the footpoint half-separation. Low-lying prominences are stable even for large twists. The importance of the external field reconnection below the filament, and the mass loss through the legs in the early phases of the eruption is stressed. The oscillations of stable prominences with periods on the Alfv6n time-scale are discussed. The results are compared with the observations.

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“…99 Both codes have been under development by large groups for over a decade are descendants of disruption simulations carried out over thirty years ago 100,101 and are sufficiently computationally demanding that only a few disruption examples have been run. These codes have the advantage that they are presently usable, but they intertwine the force balance and evolution calculations in order to be able to simulate evolution on the Alfvénic time scale.…”

Section: Integrated Simulationsmentioning

confidence: 99%