Thermal trigger for solar flares and coronal loops formation

Details Thermal trigger for solar flares and coronal loops formation Thermal trigger for solar flares and coronal loops formation

Jan 1982

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1982soph...75..237s&link_type=abstract

Solar Physics, vol. 75, Jan. 1982, p. 237-244.

Physics

10

Coronal Loops, Magnetohydrodynamic Stability, Plasma Temperature, Solar Corona, Solar Flares, Thermal Instability, Approximation, Chromosphere, Current Sheets, Density Distribution, High Temperature Plasmas, Neutral Sheets, Plasma Density, Radiative Heat Transfer, Solar Magnetic Field, Temperature Distribution

Scientific paper

Solar flares result from the fast release of magnetic energy of electric currents in the upper chromosphere and low corona. The accumulation of magnetic energy may be achieved in the form of a plane or curve pinched current sheet. In order to explain cold loops in the solar corona, longitudinal stability for a current sheet, uniform along the current, is considered. In the MHD approximation, the stability problem is solved for the plane neutral sheet and small disturbances propagating along the current. The current sheet is shown to break up into a system of cooler and denser filaments, parallel to the magnetic field lines, due to radiative cooling. This process corresponds to the condensation mode of a thermal instability and can trigger a solar flare, as well as cause the formation of very dense cold filaments surrounded by a high-temperature, low-density plasma inside the current sheet. The hot plasma is cooled by radiation and compressed within the filaments; the cold dense plasma then flows out from the current sheet along the filaments.

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