  Recent IRIS observations have revealed a prevalence of intermittent
small-scale jets with apparent speeds of 80 - 250 km s$^{-1}$, emanating from
small-scale bright regions inside network boundaries of coronal holes. We find
that these network jets appear not only in coronal holes but also in quiet-sun
regions. Using IRIS 1330A (C II) slit-jaw images, we extract several parameters
of these network jets, e.g. apparent speed, length, lifetime and increase in
foot-point brightness. Using several observations, we find that some properties
of the jets are very similar but others are obviously different between the
quiet sun and coronal holes. For example, our study shows that the coronal-hole
jets appear to be faster and longer than those in the quiet sun. This can be
directly attributed to a difference in the magnetic configuration of the two
regions with open magnetic field lines rooted in coronal holes and magnetic
loops often present in quiet sun. We have also detected compact bright loops,
likely transition region loops, mostly in quiet sun. These small loop-like
regions are generally devoid of network jets. In spite of different magnetic
structures in the coronal hole and quiet sun in the transition region, there
appears to be no substantial difference for the increase in foot-point
brightness of the jets, which suggests that the generation mechanism of these
network jets is likely the same in both regions.
