Proton acceleration during coalescence of two parallel current loops in solar flares

Details Proton acceleration during coalescence of two parallel current loops in solar flares Proton acceleration during coalescence of two parallel current loops in solar flares

Oct 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004a%26a...426..333s&link_type=abstract

Astronomy and Astrophysics, v.426, p.333-341 (2004)

Astronomy and Astrophysics

Astrophysics

2

Acceleration Of Particles, Magnetohydrodynamics (Mhd), Sun: Flares

Scientific paper

We investigate the plasma dynamics during coalescence of two parallel current loops in solar flares by using a resistive three-dimensional MHD simulation code, paying particular attention finding the most effective electromagnetic fields for the production of high-energy protons. Next we investigate the orbit of many protons in the electromagnetic fields obtained from the MHD simulations. We investigate two cases of the coalescence process: (1) co-helicity reconnection where only the poloidal magnetic field produced from the axial currents dissipates and (2) counter-helicity reconnection where both poloidal and axial magnetic fields dissipate. We found a bump-on-tail distribution in the same direction as the original loop current for both the cases of co-helicity and counter-helicity. It is shown that the maximum proton energy exceeds the energy (2.223 MeV) of the observed prompt nuclear de-excitation lines of gamma-ray, and that proton energy spectrum is neither a pure power-law type nor a pure exponential type. We may conclude that anisotropic proton acceleration along the loop can be realized both for co-helicity and counter-helicity reconnection during the coalescence of two parallel loops.

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