  Oscillatory reconnection can manifest through the interaction between the
ubiquitous MHD waves and omnipresent null points in the solar atmosphere and is
characterized by an inherent periodicity. In the current study, we focus on the
relationship between the period of oscillatory reconnection and the strength of
the wave pulse initially perturbing the null point, in a hot coronal plasma. We
use the PLUTO code to solve the fully compressive, resistive MHD equations for
a 2D magnetic X-point. Using wave pulses with a wide range of amplitudes, we
perform a parameter study to obtain values for the period, considering the
presence and absence of anisotropic thermal conduction separately. In both
cases, we find that the resulting period is independent of the strength of the
initial perturbation. The addition of anisotropic thermal conduction only leads
to an increase in the mean value for the period, in agreement with our previous
study. We also consider a different type of initial driver and we obtain an
oscillation period matching the independent trend previously mentioned. Thus,
we report for the first time on the independence between the type and strength
of the initializing wave pulse and the resulting period of oscillatory
reconnection in a hot coronal plasma. This makes oscillatory reconnection a
promising mechanism to be used within the context of coronal seismology.
