  Magnetic reconnection is believed to be the primary mechanism by which
non-potential energy stored in coronal magnetic fields is rapidly released
during solar eruptive events. Unfortunately, owing to the small spatial scales
on which reconnection is thought to occur, it is not directly observable in the
solar corona. However, larger scale processes, such as associated inflow and
outflow, and signatures of accelerated particles have been put forward as
evidence of reconnection. We explore the origin of a persistent Type I radio
source that accompanies a coronal X--shaped structure during its passage across
the disk. Of particular interest is the time range around a partial collapse of
the structure that is associated with inflow, outflow, and signatures of
particle acceleration. Imaging radio observations from the NRH were used to
localise the radio source. SDO AIA EUV observations from the same time period
were analysed, looking for evidence of inflows and outflows. Further
\texttt{mpole} magnetic reconstructions using SDO HMI observations allowed the
magnetic connectivity associated with the radio source to be determined. The
Type I radio source was well aligned with a magnetic separator identified in
the extrapolations. During the partial collapse, gradual (1 km/s) and fast (5
km/s) inflow phases and fast (30 km/s) and rapid (80-100 km/s) outflow phases
were observed, resulting in an estimated reconnection rate of ~ 0.06. The radio
source brightening and dimming was found to be co-temporal with increased soft
x-ray emission in both RHESSI and GOES. We interpret the brightening and
dimming of the radio emission as evidence for accelerated electrons in the
reconnection region responding to a gradual fall and rapid rise in electric
drift velocity, in response to the inflowing and outflowing field lines. These
results present a comprehensive example of 3D null-point reconnection.

Solar and Stellar Astrophysics