  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 with the
Atmospheric Imaging Assembly (AIA) 171{\AA} passband to follow the evolution of
coronal plumes, the observations taken by the Interface Region Imaging
Spectrograph (IRIS) slit-jaw 1330{\AA} to study the network jets, and the
line-of-sight magnetograms taken by the Helioseismic and Magnetic Imager (HMI)
to overview the the photospheric magnetic features in the regions. Four regions
in the network lanes are identified, and labeled ``R1--R4''. We find that
coronal plumes are clearly seen only in ``R1''&''R2'' but not in ``R3''&``R4'',
even though network jets abound in all these regions. Furthermore, while
magnetic features in all these regions are dominated by positive polarity, they
are more compact (suggesting stronger convergence) in ``R1''&``R2'' than that
in ``R3''&``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''&``R2'' are higher and faster than that in ``R3''&``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''&``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.
