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Oscillatory reconnection can manifest through the interaction between theubiquitous MHD waves and omnipresent null points in the solar atmosphere and ischaracterized by an inherent periodicity. In the current study, we focus on therelationship between the period of oscillatory reconnection and the strength ofthe wave pulse initially perturbing the null point, in a hot coronal plasma. Weuse the PLUTO code to solve the fully compressive, resistive MHD equations fora 2D magnetic X-point. Using wave pulses with a wide range of amplitudes, weperform a parameter study to obtain values for the period, considering thepresence and absence of anisotropic thermal conduction separately. In bothcases, we find that the resulting period is independent of the strength of theinitial perturbation. The addition of anisotropic thermal conduction only leadsto an increase in the mean value for the period, in agreement with our previousstudy. We also consider a different type of initial driver and we obtain anoscillation period matching the independent trend previously mentioned. Thus,we report for the first time on the independence between the type and strengthof the initializing wave pulse and the resulting period of oscillatoryreconnection in a hot coronal plasma. This makes oscillatory reconnection apromising mechanism to be used within the context of coronal seismology.

The independence of oscillatory reconnection periodicity from the initial pulse