| Abstract * |
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Both coronal plumes and network jets are rooted in network lanes. The relationship between the two, however, has yet to be addressed. For this purpose, we perform an observational analysis using images acquired on 2015 December 4 with the Atmospheric Imaging Assembly (AIA) 171Å passband to follow the evolution of coronal plumes, the observations taken by the Interface Region Imaging Spectrograph (IRIS) at slit-jaw 1330Å to study the network jets, and the line-of-sight magnetograms taken by the Helioseismic and Magnetic Imager (HMI) to overview the photospheric magnetic features in the regions. Four regions in the network lanes are identified and labeled R1–R4, which are abundant with network jets. R1 and R2 are associated with coronal plumes that could be clearly seen for at least five days, while coronal plumes are hardly seen in R3 and R4 for at least three days. Furthermore, while magnetic features in all these regions are dominated by positive polarity, they are more compact (suggesting stronger convergence) in R1 and R2 than that in R3 and R4.We develop an automated method to identify and track the network jets in the regions.We find that the network jets rooted in R1 and R2 are higher and faster than those in R3 and R4, indicating that network regions producing stronger coronal plumes also tend to produce more dynamic network jets.We suggest that the stronger convergence in R1 and R2 might provide a condition for faster shocks and/or more small-scale magnetic reconnection events that power more dynamic network jets and coronal plumes. |
