  We report observations of an eruptive X2.8 flare on 2013 May 13, which shows
two distinct episodes of energy release in the impulsive phase. The first
episode is characterized by the eruption of a magnetic flux rope, similar to
the energy-release process in most standard eruptive flares. While the second
episode, which is stronger than the first normal one and shows enhanced
high-energy X-ray and even $\gamma$-ray emissions, is closely associated with
magnetic reconnection of a large-scale loop in the aftermath of the eruption.
The reconnection inflow of the loop leg is observed in the Solar Dynamics
Observatory (SDO)/Atmospheric Imaging Assembly (AIA) 304 \r{A} passband and
accelerates towards the reconnection region to a speed as high as $\sim$130
km/s. Simultaneously the corresponding outflow jets are observed in the AIA hot
passbands with a speed of $\sim$740 km/s and mean temperature of $\sim$14 MK.
RHESSI observations show a strong burst of hard X-ray (HXR) and $\gamma$-ray
emissions with hard electron spectra of $\delta\approx3$, exhibiting a
soft-hard-harder behavior. A distinct altitude decrease of the HXR loop-top
source coincides with the inward swing of the loop leg observed in the AIA 304
\r{A} passband, which is suggested to be related to the coronal implosion. This
fast inflow of magnetic flux contained in the loop leg greatly enhances the
reconnection rate and results in very efficient particle acceleration in the
second-step reconnection, which also helps to achieve a second higher
temperature peak up to T $\approx$ 30 MK.
