Magnetic flux ropes as models of a solar flare and transition of flare filament into CMI-regim of motion

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Аннотация

A new physical mechanism of flare energy release in force-free magnetic flux ropes is described: as the top of the magnetic rope-loop enters the corona, the external pressure G, which keeps it from expanding, steadily decreases. At its critically low value, the longitudinal field tends to zero on the magnetic surface where the currents change sign, and the force-free parameter and azimuthal current near this surface grow without limit, approaching the rupture. This excites plasma turbulence in the rope and serves as a flare trigger. Rapid dissipation of the field and currents on the anomalous plasma resistance induces an electric field much higher than the Dreiser field. The forces acting on the flare filament in the corona are described, and the conditions for its transition to the dynamic CME regime are discussed.

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Авторлар туралы

A. Solov’ev

Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo

Хат алмасуға жауапты Автор.
Email: solov@gaoran.ru
Ресей, St. Petersburg

О. Korolkova

Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo

Email: korolkova@gaoran.ru
Ресей, St. Petersburg

Е. Kirichek

Central Astronomical Observatory of the Russian Academy of Sciences at Pulkovo

Email: elenakirichek@gmail.com
Ресей, St. Petersburg

Әдебиет тізімі

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2. Fig. 1. A section of a shielded magnetic bundle of radius a is shown, the current (large arrows) changes sign at a distance from the axis, so that . (a) Bundle with a strong current on the axis. (b) Bundle with a peripheral current sheath.

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3. Fig. 3. For function (8) – – the azimuthal field and longitudinal current are shown, which changes sign at kr = 1.

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4. Fig. 4. The flow function (dashed line) and the distribution of longitudinal currents (solid line) in model 2 for different values of the parameter m.

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5. Fig. 2. Function (10). The dotted line is the longitudinal field at G = 2.5, the solid line is G = Gcrit = 2.0. The azimuthal field is shown separately by an arrow.

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6. Fig. 5. Longitudinal magnetic field at m = 2 (second model) and different G. Solid line – G = , dotted line – G = 2. Dash-dotted line – azimuthal field.

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7. Fig. 6. Cross-section of the bundle for the case when the direction of the field on the lower bypass of the bundle coincides with the direction of the external transverse field. The external force is directed upward.

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8. Fig. 7. The direction of the external transverse field coincides with the direction of the azimuthal field on the upper bypass. A magnetic dome is formed, preventing the rise of the bundle.

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