  The multi-scaled solar magnetic field consists of two major components:
active regions (ARs) and magnetic network. Unraveling the cycle-dependent
properties and interrelations of these components is crucial for understanding
the evolution of the solar magnetic field. In this study, we investigate these
components using magnetic power spectra derived from high-resolution and
continuous synoptic magnetograms since cycle 23 onwards. Our results show that
the size of the magnetic network ranges from 26 Mm to 41 Mm without dependence
on the solar cycle. The power of the network field ($P_{NW}$) accounts for
approximately 20\% of the total power during any phase of solar cycles. In
contrast to the AR power ($P_{AR}$), $P_{NW}$ displays a weaker cycle
dependence, as described by the relationship $P_{NW}$ $\approx$ 0.6* $P_{AR}$ +
40. The power-law index between AR sizes and magnetic network sizes presents a
strong anti-correlation with the activity level. Additionally, our study
indicates that in the absence of sunspots on the solar disc, the magnetic power
spectra remain time-independent, consistently exhibiting similarity in both
shape and power. This study introduces a new method to investigate the
properties of the magnetic network and provides magnetic power spectra for
high-resolution simulations of the solar magnetic field at the surface at
various phases of solar cycles.
