The
2005 May 13 two ribbon flare evolution is examined in UV and HXR using
data from RHESSI and TRACE to better understand the 3D evolution of
magnetic reconnection and energy release. After the peak of the solar
flare, the RHESSI HXR images illustrate a ribbon structure. At this
time, the two UV ribbons are spatially and temporally resolved and it
is observed that ‘negative’ HXRs expand along with the negative UV
ribbon. This is further evidenced by a rough linear correlation between
the HXR and UV light curves as well as a correlation between the HXR
light curve and reconnection rate given by the UV ribbons. We conclude
that by comparing UV and HXR sources with the reconnection rate, the
spatially resolved energy release rate can then be derived.
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