  We compare the properties of kG magnetic structures in the solar network and
in active region plage at high spatial resolution. Our analysis used six SP
scans of the solar disc centre aboard Hinode SOT and inverted the obtained
spectra of the photospheric 6302 \AA line pair using the 2D SPINOR code.
Photospheric magnetic field concentrations in network and plage areas are on
average 1.5 kG strong with inclinations of 10-20 degrees, and have <400 m/s
internal and 2-3 km/s external downflows. At the disc centre, the continuum
intensity of magnetic field concentrations in the network are on average 10%
brighter than the mean quiet Sun, whilst their plage counterparts are 3%
darker. A more detailed analysis revealed that all sizes of individual kG
patches in the network have 150 G higher field strengths on average, 5% higher
continuum contrasts, and 800 m/s faster surrounding downflows than similarly
sized patches in the plage. The speed of the surrounding downflows also
correlates with the patch area, and patches containing pores can produce
supersonic flows exceeding 11 km/s in individual pixels. Furthermore, the
magnetic canopies of kG patches are on average 9 degrees more horizontal in the
plage compared to the network. Most of the differences between the network and
plage are due to their different patch size distributions, but the intrinsic
differences between similarly sized patches is likely results from the
modification of the convection photospheric convection with increasing amounts
of magnetic flux.
