A model for the solar flare

Details A model for the solar flare A model for the solar flare

Jul 1975

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1975stin...7615007c&link_type=abstract

Presented at conf. at Natl. Center for Atmospheric Res., Boulder, Colo., 23-25 Sep. 1974 p 361-371

Physics

Chromosphere, Solar Corona, Solar Flares, Emission Spectra, H Alpha Line, Solar Magnetic Field, Solar Spectra

Scientific paper

It is suggested that many solar flares occur due to an interaction between newly emerging magnetic flux and an active region filament. A current sheet forms between the new and old flux and, when its electric current density exceeds a critical value, rapid magnetic fields reconnection takes place. Electrons are then accelerated to high energies and follow the magnetic field lines down to the chromosphere where they produce several (typically three) bright H alpha knots. Magnetic energy is continuously released as reconnected prominence fields are allowed to untwist. Two ribbons of H alpha emission are produced by one or more of three mechanisms: energetic particles, thermal conduction or shocks due to infalling material.

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