Solar flares can release coronal magnetic energy explosively and may impact
the safety of near-earth space environments. Their structures and properties on
macroscale have been interpreted successfully by the generally-accepted
two-dimension standard model invoking magnetic reconnection theory as the key
energy conversion mechanism. Nevertheless, some momentous dynamical features as
discovered by recent high-resolution observations remain elusive. Here, we
report a self-consistent high-resolution three-dimension magnetohydrodynamical
simulation of turbulent magnetic reconnection within a flare current sheet. It
is found that fragmented current patches of different scales are spontaneously
generated with a well-developed turbulence spectrum at the current sheet, as
well as at the flare loop-top region. The close coupling of tearing-mode and
Kelvin-Helmholtz instabilities plays a critical role in developing turbulent
reconnection and in forming dynamical structures with synthetic observables in
good agreement with realistic observations. The sophisticated modeling makes a
paradigm shift from the traditional to three-dimension turbulent reconnection
model unifying flare dynamical structures of different scales.Comment: 15 pages, 8 figure, accepted for publication in ApJ
