Fermi acceleration at fast shock in a solar flare and impulsive loop-top hard X-ray source

Details Fermi acceleration at fast shock in a solar flare and impulsive loop-top hard X-ray source Fermi acceleration at fast shock in a solar flare and impulsive loop-top hard X-ray source

1998-01-13

arxiv.org/abs/astro-ph/9801109v1

Astronomy and Astrophysics

Astrophysics

13 pages, 3 postscript figures, used AASTeX macros; accepted in Astrophysical Journal Letters

Scientific paper

10.1086/311207

We propose that non-thermal electrons are efficiently accelerated by first-order Fermi process at the fast shock, as a natural consequence of the new magnetohydrodynamic picture of the flaring region revealed with Yohkoh. An oblique fast shock is naturally formed below the reconnection site, and boosts the acceleration to significantly decrease the injection energy. The slow shocks attached to the reconnection X-point heat the plasma up to 10--20 MK, exceeding the injection energy. The combination of the oblique shock configuration and the pre-heating by the slow shock allows bulk electron acceleration from the thermal pool. The accelerated electrons are trapped between the two slow shocks due to the magnetic mirror downstream of the fast shock, thus explaining the impulsive loop-top hard X-ray source discovered with Yohkoh. Acceleration time scale is ~ 0.3--0.6 s, which is consistent with the time scale of impulsive bursts. When these electrons stream away from the region enclosed by the fast shock and the slow shocks, they are released toward the footpoints and may form the simultaneous double-source hard X-ray structure at the footpoints of the reconnected field lines.

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