Loss of equilibrium in coronal loops

Details Loss of equilibrium in coronal loops Loss of equilibrium in coronal loops

Jan 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992soph..137..105l&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 137, Jan. 1992, p. 105-120.

Physics

3

Coronal Loops, Magnetic Field Configurations, Plasma Pressure, Solar Flares, Solar Magnetic Field, Solar Prominences, Stellar Models

Scientific paper

The loss of equilibrium in coronal magnetic field structures is a possible source of energy for coronal heating and solar flares. It is investigated whether such a loss of equilibrium occurs when a coronal loop is progressively twisted by photospheric motions. In studies of 2D cylindrical equilibria, long loops have been found to be of constant cross-sectional area along most of their length, with axial variations being confined to narrow boundary layers. This information is used to develop a 1D line-tied model, for a 2D coronal loop. A twisted loop with a non-zero plasma pressure is also examined. The loss of equilibrium is only found at high-plasma beta. It is conjectured that such high-beta can occur in flare loops and prior to a prominence eruption. However, when the plasma evolves adiabatically, there is no loss of equilibrium.

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