  One of the most important features in the solar atmosphere is magnetic
network and its rela- tionship with the transition region (TR), and coronal
brightness. It is important to understand how energy is transported into the
corona and how it travels along the magnetic-field lines be- tween deep
photosphere and chromosphere through the TR and corona. An excellent proxy for
transportation is the Interface Region Imaging Spectrograph (IRIS) raster scans
and imaging observations in near-ultraviolet (NUV) and far-ultraviolet (FUV)
emission channels with high time-spatial resolutions. In this study, we focus
on the quiet Sun as observed with IRIS. The data with high signal to noise
ratio in Si IV, C II and Mg II k lines and with strong emission intensities
show a high correlation in TR bright network points. The results of the IRIS
intensity maps and dopplergrams are compared with those of Atmo- spheric
Imaging Assembly (AIA) and Helioseismic and Magnetic Imager (HMI) instruments
onboard the Solar Dynamical Observatory (SDO). The average network intensity
profiles show a strong correlation with AIA coronal channels. Furthermore, we
applied simultaneous observations of magnetic network from HMI and found a
strong relationship between the network bright points in all levels of the
solar atmosphere. These features in network elements exhibited high doppler
velocity regions and large mag- netic signatures. A dominative fraction of
corona bright points emission, accompanied by the magnetic origins in
photosphere, suggest that magnetic-field concentrations in the network rosettes
could help couple between inner and outer solar atmosphere.
