  Oscillatory reconnection is a relaxation process in magnetised plasma, with
an inherent periodicity that is exclusively dependent on the properties of the
background plasma. This study focuses on the seismological prospects of
oscillatory reconnection in the solar corona. We perform three sets of
parameter studies (for characteristic coronal values of the background magnetic
field, density and temperature) using the PLUTO code to solve the fully
compressive, resistive MHD equations for a 2D magnetic X-point. From each
parameter study, we derive the period of the oscillatory reconnection. We find
that this period is inversely proportional to the characteristic strength of
the background magnetic field and the square root of the initial plasma
temperature, while following a square root dependency upon the equilibrium
plasma density. These results reveal an inverse proportionality between the
magnitude of the Alfv\'en speed and the period, as well as the background sound
speed and the period. Furthermore, we note that the addition of anisotropic
thermal conduction only leads to a small increase in the mean value for the
period. Finally, we establish an empirical formula that gives the value for the
period in relation to the background magnetic field, density and temperature.
This gives us a quantified relation for oscillatory reconnection, to be used as
a plasma diagnostic in the solar corona, opening up the possibility of using
oscillatory reconnection for coronal seismology.
