title: Dynamical finite-amplitude magnetic reconnection at an X-type neutral point

authors: McClymont, A.N.

abstract: The linear theory of magnetic reconnection demonstrates that the rate of energy release at an X-type neutral point is "fast" - only logarithmically dependent on the plasma resistivity - if the field is strictly two-dimensional, gas pressure is absent, and perturbations are small. The present paper explores the response of the X-point to finite amplitude disturbances under the more realistic conditions of limited compressibility and a finite nonplanar magnetic field component. We show that fast reconnection is not inhibited by large amplitudes of the perturbation - in fact, both the reconnection rate and the ohmic dissipation rate increase with decreasing plasma resistivity. This "super fast" scaling can be understood by a simple, one-dimensional dynamic collapse model. However, the presence of finite gas pressure or an axial magnetic field component stalls the collapse by providing backpressure which retards the imploding magnetic wave: the current sheet is prevented from thinning and reconnection drops toward the static diffusion rate. Thus we overrule the initial implosion as a means of rapidly liberating magnetic energy when gas pressure or an axial magnetic field are present, as they are in the solar corona. But in this case the initial collapse does not provide the complete picture. Gas is subsequently squeezed out of the current sheet, allowing a higher current density to be attained. Thus the possibility of fast reconnection remains open. The dynamics of the evolution are complicated; it is not yet clear under exactly what conditions fast reconnection may be attainable. © 1996. The American Astronomical Society. All rights reserved.

text: Dynamical finite-amplitude magnetic reconnection at an X-type neutral point The linear theory of magnetic reconnection demonstrates that the rate of energy release at an X-type neutral point is "fast" - only logarithmically dependent on the plasma resistivity - if the field is strictly two-dimensional, gas pressure is absent, and perturbations are small. The present paper explores the response of the X-point to finite amplitude disturbances under the more realistic conditions of limited compressibility and a finite nonplanar magnetic field component. We show that fast reconnection is not inhibited by large amplitudes of the perturbation - in fact, both the reconnection rate and the ohmic dissipation rate increase with decreasing plasma resistivity. This "super fast" scaling can be understood by a simple, one-dimensional dynamic collapse model. However, the presence of finite gas pressure or an axial magnetic field component stalls the collapse by providing backpressure which retards the imploding magnetic wave: the current sheet is prevented from thinning and reconnection drops toward the static diffusion rate. Thus we overrule the initial implosion as a means of rapidly liberating magnetic energy when gas pressure or an axial magnetic field are present, as they are in the solar corona. But in this case the initial collapse does not provide the complete picture. Gas is subsequently squeezed out of the current sheet, allowing a higher current density to be attained. Thus the possibility of fast reconnection remains open. The dynamics of the evolution are complicated; it is not yet clear under exactly what conditions fast reconnection may be attainable. © 1996. The American Astronomical Society. All rights reserved.

year: 1996

title: Magnetic energy release in dynamic fan reconnection models

authors: Craig, Ian J.D.

subjects: MHD—plasmas—sun

abstract: The problem of dynamic, three-dimensional magnetic reconnection is considered. Analytic “fan current” solutions are derived by superposing plane-wave disturbances on magnetic X-point equilibria. The localization of the wave produces a strong current sheet containing the neutral point. It is shown that the classical rate of resistive dissipation in the sheet, namely Wn~n1/2, represents the slowest possible energy-loss rate for the disturbance. The conditions required for fast coronal reconnection are then discussed. It is pointed out that significant “flare-like” energy release may be possible under physically realizable conditions. Moreover, the small length scales associated with the current sheet widths of order ∆x~n1/2 suggest that conditions are probably collisionless close to the neutral point. It is argued that our results are consistent with magnetic reconnection simulations that display “stalling” of the merging rate at small plasma resistivities.

text: Magnetic energy release in dynamic fan reconnection models The problem of dynamic, three-dimensional magnetic reconnection is considered. Analytic “fan current” solutions are derived by superposing plane-wave disturbances on magnetic X-point equilibria. The localization of the wave produces a strong current sheet containing the neutral point. It is shown that the classical rate of resistive dissipation in the sheet, namely Wn~n1/2, represents the slowest possible energy-loss rate for the disturbance. The conditions required for fast coronal reconnection are then discussed. It is pointed out that significant “flare-like” energy release may be possible under physically realizable conditions. Moreover, the small length scales associated with the current sheet widths of order ∆x~n1/2 suggest that conditions are probably collisionless close to the neutral point. It is argued that our results are consistent with magnetic reconnection simulations that display “stalling” of the merging rate at small plasma resistivities.

year: 1999-01

title: Between the borders

authors: Apiata, Hāwea

abstract: Ekphrasis in response to the artwork 'Taniko Border 6' by Ngāti Raukawa artist, John Bevan Ford.

text: Between the borders Ekphrasis in response to the artwork 'Taniko Border 6' by Ngāti Raukawa artist, John Bevan Ford.

year: 2023-11-30