On the energetics of slow magnetic tearing

Arion, Douglas N.

doi:10.1086/161754

Cited by 4 publications

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“…In the last few years, several authors (Adler, Kulsrud & White 1980;Arion 1984;Bondeson & Sobel 1984) have performed detailed analyses on how the equilibrium energy balance evolves when a resistive instability takes place. However, all these analyses deal with the parameter range typical of laboratory plasmas, i.e.…”

Section: Introductionmentioning

confidence: 99%

Energy variations at the onset of the tearing instability

Torricelli‐Ciamponi

1986

J. Plasma Phys.

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The resistive instability of a simple one-dimensional current sheet model has been investigated both in the long and in the short wavelength approximation. For the linear phase of the instability it is possible to derive, by means of an expansion technique, an analytical expression for the growth rate and for the perturbation itself. The variations of each kind of energy (magnetic, kinetic and dissipated energies, Poynting vector, work against pressure gradients and magnetic forces) are then exactly computed. Different behaviour of the System is obtained for different wavelengths. In particular, the driving energy for the instability is found to come from different regions: for high wavenumber α there is a decrease of the magnetic energy in the inner resistive region where the reconnection occurs, whereas for low-α modes the magnetic energy decreases in the outer ideal region. Moreover, the amount of Joule dissipation is found to increase with decreasing α so that the low-α regime is the most efficient.

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Section: Introductionmentioning

confidence: 99%

Energy variations at the onset of the tearing instability

Torricelli‐Ciamponi

1986

J. Plasma Phys.

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Particle Acceleration

Vlahos

Machado²,

Ramaty

et al. 1989

Energetic Phenomena on the Sun

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Stimulated dissipation of magnetic discontinuities and the origin of solar flares

Parker

1987

Sol Phys

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It is proposed that the principal cause of the confined solar flare is the dissipation of magnetic energy at the many small-scale pre-existing tangential dscontinuities in the local bipolar magnetic field. The discontinuities are a consequence of the continuous shuffling and intermixing of the footpoints of the bipolar field by the turbulent photospheric granules. The X-ray corona within the bipolar field is presumed to be a consequence of the continuing dissipation by reconnection at these discontinuities. A flare results when static deformation and/or internal agitation of the field stimulates the onset of rapid reconnection at the many small internal discontinuities. The discontinuities are partially exhausted by the flare, so that the post-flare X-ray emission of that particular loop is substantially below the pre-flare level for a period of some hours while the discontinuities are being rejuvenated.

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On the energetics of slow magnetic tearing

Cited by 4 publications

References 0 publications

Energy variations at the onset of the tearing instability

Energy variations at the onset of the tearing instability

Particle Acceleration

Stimulated dissipation of magnetic discontinuities and the origin of solar flares

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