MHD Simulations of the Internal Shocks in Magnetic Reconnection Jet in the Solar Flare: Possibility of the Particle Acceleration

Details MHD Simulations of the Internal Shocks in Magnetic Reconnection Jet in the Solar Flare: Possibility of the Particle Acceleration MHD Simulations of the Internal Shocks in Magnetic Reconnection Jet in the Solar Flare: Possibility of the Particle Acceleration

Jul 2003

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003icrc....6.3351t&link_type=abstract

Proceedings of the 28th International Cosmic Ray Conference. July 31-August 7, 2003. Trukuba, Japan. Under the auspices of the I

Physics

1

Scientific paper

The solar atmosphere is filled with the high-energy particles. The satellites such as Yohkoh and RHESSI observe the Xand gamma-ray emissions from them. They are accelerated in solar flares. The their origin is, however, not fully known yet. In this paper, we examine how the magnetic reconnection creates the fast shocks, by performing two-dimensional numerical resistive magnetohydro dynamic simulations. As the results, we find that the current sheet becomes thin by tearing instability, and it collapses to Sweet-Parker current sheet. The thin current sheet becomes unstable to the tearing instability again. The fast reconnection starts immediately after the plasmoid ejection, which are created by the secondary tearing instability. The internal shocks are created inside the reconnection jet due to the non-steady plasmoid-ejection. In the next phase, the magnetic reconnection jet oscillates in the current sheet, which is due to Kelvin-Helmholtzlike instability, or turbulent reconnection. The reconnection jet collides with two standing slow shocks, so that the fast shocks are created by oblique shocks. The fast shocks created by the magnetic reconnection are possible sites for the particle acceleration in the solar flare.

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