A magnetodynamic mechanism for the heating of emerging magnetic flux tubes and loop flares

Details A magnetodynamic mechanism for the heating of emerging magnetic flux tubes and loop flares A magnetodynamic mechanism for the heating of emerging magnetic flux tubes and loop flares

Sep 1988

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1988soph..116..291u&link_type=abstract

Solar Physics (ISSN 0038-0938), vol. 116, no. 2, 1988, p. 291-307.

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47

Coronal Loops, Magnetic Field Configurations, Magnetic Flux, Magnetohydrodynamics, Solar Flares, Solar Magnetic Field, Computational Astrophysics, Computerized Simulation, Doppler Effect, H Alpha Line, Solar Activity, Solar Spectra, Temporal Distribution

Scientific paper

A new magnetodynamic model for loop flares is proposed to explain the observational facts obtained from space during the last solar activity maximum. In the model, the supply of energy to the loop top comes from below the chromosphere immediately before the flare (30 s - 1 min before the hard X-ray impulsive bursts) in the form of the relaxing fronts of magnetic twist of opposite sign. These packets are thought to be built up in the process of loop emergence, stored at the footpoints of the loop below the photosphere, and released when the part of the feet floats up further. These released packets of magnetic twist drive the mass in the high chromosphere and transition zone into helical flows with pinch heating, and when these collide at the top of the loop, a very hot region appears there with a violent unwinding of the twists, resulting in the rapid dynamical annihilation of the magnetic energy, Bφ2/8π. Electrons and ions, raised to medium energies in the pinch at the incidence of the packets to the loop, are accelerated further by the Fermi-I mechanism between the approaching fronts of magnetic twist, and when Bφ is weakened by unwinding they are released towards the chromosphere, and cause simultaneous γ-ray and hard X-ray bursts.

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