A Unified Picture of Solar Flares as Avalanches of Magnetic Reconnection

Details A Unified Picture of Solar Flares as Avalanches of Magnetic Reconnection A Unified Picture of Solar Flares as Avalanches of Magnetic Reconnection

May 1992

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1992aas...180.3014l&link_type=abstract

American Astronomical Society, 180th AAS Meeting, #30.14; Bulletin of the American Astronomical Society, Vol. 24, p.777

Astronomy and Astrophysics

Astronomy

Scientific paper

The coronal magnetic field is expected to be in a twisted tangled state due to photospheric convective motions. These motions can drive the magnetic field to a statistically steady state where energy is released impulsively. We show that a simple model of magnetic energy release in a 3-dimensional complex magnetized plasma can quantitatively explain the observed distributions of solar flare energies, peak fluxes, and durations. This model implies that the energy release process is fundamentally the same for flares of all sizes. Observational predictions of this model are discussed.

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