  Oscillatory reconnection (a relaxation mechanism with periodic changes in
connectivity) has been proposed as a potential physical mechanism underpinning
several periodic phenomena in the solar atmosphere including, but not limited
to, quasi-periodic pulsations (QPPs). Despite its importance, however, the
mechanism has never been studied within a hot, coronal plasma. We investigate
oscillatory reconnection in a one million Kelvin plasma by solving the
fully-compressive, resistive MHD equations for a 2D magnetic X-point under
coronal conditions using the PLUTO code. We report on the resulting oscillatory
reconnection including its periodicity and decay rate. We observe a more
complicated oscillating profile for the current density compared to that found
for a cold plasma, due to mode-conversion at the equipartition layer. We also
consider, for the first time, the effect of adding anisotropic thermal
conduction to the oscillatory reconnection mechanism, and we find this
simplifies the spectrum of the oscillation profile and increases the decay
rate. Crucially, the addition of thermal conduction does not prevent the
oscillatory reconnection mechanism from manifesting. Finally, we reveal a
relationship between the equilibrium magnetic field strength, decay rate, and
period of oscillatory reconnection, which opens the tantalising possibility of
utilizing oscillatory reconnection as a seismological tool.
