Coronal Implosion and Particle Acceleration in the Wake of a Filament Eruption

Details Coronal Implosion and Particle Acceleration in the Wake of a Filament Eruption Coronal Implosion and Particle Acceleration in the Wake of a Filament Eruption

2009-08-08

arxiv.org/abs/0908.1137v1

Astrophysical Journal Letters 703 (2009) L23-L28

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

accepted to ApJL

Scientific paper

10.1088/0004-637X/703/1/L23

We study the evolution of a group of TRACE 195 A coronal loops overlying a reverse S-shaped filament on 2001 June 15. These loops were initially pushed upward with the filament ascending and kinking slowly, but as soon as the filament rose explosively, they began to contract at a speed of ~100 km/s, and sustained for at least 12 min, presumably due to the reduced magnetic pressure underneath with the filament escaping. Despite the contraction following the expansion, the loops of interest remained largely intact during the filament eruption, rather than formed via reconnection. These contracting loops naturally formed a shrinking trap, in which hot electrons of several keV, in an order of magnitude estimation, can be accelerated to nonthermal energies. A single hard X-ray burst, with no corresponding rise in GOES soft X-ray flux, was recorded by the Hard X-ray Telescope (HXT) on board Yohkoh, when the contracting loops expectedly approached the post-flare arcade originating from the filament eruption. HXT images reveal a coronal source distinctly above the top of the soft X-ray arcade by ~15". The injecting electron population for the coronal source (thin target) is hardening by ~1.5 powers relative to the footpoint emission (thick target), which is consistent with electron trapping in the weak diffusion limit. Although we can not rule out additional reconnection, observational evidences suggest that the shrinking coronal trap may play a significant role in the observed nonthermal hard X-ray emission during the flare decay phase.

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