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Multiwavelength observations of the propagating disturbances (PDs),discovered by Atmospheric Imaging Assembly (AIA) onboard Solar DynamicsObservatory (SDO), are analyzed to determine its driving mechanism and physicalnature. Two magnetic strands in the localised corona are observed to approachand merge with each other followed by the generation of brightening, whichfurther propagates in a cusp-shaped magnetic channel. Differential emissionmeasure analysis shows an occurrence of heating in this region-of-interest(ROI). We extrapolate potential magnetic field lines at coronal heights fromobserved Helioseismic and Magnetic Imager (HMI) vector magnetogram via Green'sfunction method using MPI-AMRVAC. We analyze the field to locate magnetic nullsand quasi-separatrix layers (QSLs) which are preferential locations formagnetic reconnection. Dominant QSLs including a magnetic null are found toexist and match the geometry followed by PDs, therefore, it provides conclusiveevidence of magnetic reconnection. In addition, spectroscopic analysis ofInterface Region Imaging Spectrograph (IRIS) Si IV 1393.77 {\AA} line profilesshow a rise of line-width in the same time range depicting presence of massmotion in the observed cusp-shaped region. PDs are observed to exhibitperiodicities of around four minutes. The speeds of PDs measured by SurfingTransform Technique are almost close to each other in four different SDO/AIAbandpasses, i.e., 304, 171, 193 and 131 {\AA} excluding the interpretation ofPDs in terms of slow magnetoacoustic waves. We describe comprehensively theobserved PDs as quasi-periodic plasma flows generated due to periodicreconnection in vicinity of a coronal magnetic null.

Reconnection generated plasma flows in the quasi-separatrix layer in localised solar corona