  The conversion of magnetic energy into other forms during solar flares is one
of the outstanding open problems in solar physics. It is generally accepted
that magnetic reconnection plays a crucial role in these conversion processes.
To achieve the rapid energy release required in solar flares, an anomalous
resistivity, orders of magnitude higher than the Spitzer resistivity, is often
used in MHD simulations of reconnection. Spitzer resistivity is based on
Coulomb scattering, which becomes negligible at the high energies achieved by
accelerated particles. As a result, simulations of particle acceleration in
reconnection events are often performed in the absence of any interaction
between accelerated particles and any background plasma. This need not be the
case for scattering associated with anomalous resistivity caused by turbulence
within solar flares, as the higher resistivity implies an elevated scattering
rate. We present results of test particle calculations, with and without pitch
angle scattering, subject to fields derived from MHD simulations of
two-dimensional (2D) X-point reconnection. Scattering rates proportional to the
ratio of the anomalous resistivity to the local Spitzer resistivity, as well as
at fixed values, are considered. Pitch angle scattering, which is independent
of the anomalous resistivity, causes higher maximum energies in comparison to
those obtained without scattering. Scattering rates which are dependent on the
local anomalous resistivity tend to produce fewer highly energised particles
due to weaker scattering in the separatrices, even though scattering in the
current sheet may be stronger when compared to resistivity-independent
scattering. Strong scattering also causes an increase in the number of
particles exiting the computational box in the reconnection outflow region, as
opposed to along the separatrices as is the case in the absence of scattering.
