Signatures of the coalescence instability in solar flares

Details Signatures of the coalescence instability in solar flares Signatures of the coalescence instability in solar flares

Nov 1984

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1984esasp.207..193n&link_type=abstract

In ESA Plasma Astrophys. p 193-196 (SEE N85-22270 12-90)

Astronomy and Astrophysics

Astrophysics

3

Coalescing, Magnetohydrodynamic Stability, Particle Acceleration, Solar Flares, Current Density, Electron Energy, High Energy Interactions, Particle Production, Proton Energy

Scientific paper

Double sub-peak structures in the quasi periodic oscillations in the time profiles of solar flares in 1980 and 1982 are discussed. Computer simulations of the coalescence instability of two current loops agree with observations of the (widely differing) flares. The simultaneous accelerations of electrons and ions, and the double sub-peak structure in quasi periodic pulses are well explained. The double sub-peak structure is more pronounced when the currents in the two loops are sufficient for fast coalescence to occur. This corresponds to the 1980 flare. When the currents are insufficient for fast coalescence, the double sub-peak structure is less pronounced, as in the 1982 flare. Observations suggest the collision of the two microwave sources for the 1982 event. It is argued that this mechanism is a plausible particle acceleration mechanism in solar flares.

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