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We examine the role of small-scale transients in the formation and evolutionof solar coronal plumes. We study the dynamics of plume footpoints seen in thevicinity of a coronal hole using the Atmospheric Imaging Assembly (AIA) images,the Helioseismic and Magnetic Imager (HMI) magnetogram on board the SolarDynamics Observatory (SDO) and spectroscopic data from the Interface RegionImaging Spectrograph (IRIS). Quasi-periodic brightenings are observed in thebase of the plumes and are associated with magnetic flux changes. With the highspectral and spatial resolution of IRIS, we identify the sources of theseoscillations and try to understand what role the transients at the foot pointscan play in sustaining the coronal plumes. IRIS sit and stare observationprovide a unique opportunity to study the evolution of foot points of theplumes. We notice enhanced line width, intensity and large deviation from theaverage Doppler shift in the line profiles at specific instances which indicatethe presence of flows at the foot points of plumes. We propose that outflows(jet-like features) as a result of small scale reconnections affect the lineprofiles. These jet-like features may be also responsible for the generation ofpropagating disturbances within the plumes which are observed to be propagatingto larger distances as recorded from multiple AIA channels. These propagatingdisturbances can be explained in terms of slow magnetoacoustic waves.

Dynamics of on-disk plumes as observed with Interface Region Imaging Spectrograph, Atmospheric Imaging Assembly and Helioseismic and Magnetic Imager