  We have performed power spectral analysis of surface temperatures,
velocities, and magnetic fields, using spectro-polarimetric data taken with the
Hinode Solar Optical Telescope. When we make power spectra in a field-of-view
covering the super-granular scale, kinetic and thermal power spectra have a
prominent peak at the granular scale while the magnetic power spectra have a
broadly distributed power over various spatial scales with weak peaks at both
the granular and supergranular scales. To study the power spectra separately in
internetwork and network regions, power spectra are derived in small
sub-regions extracted from the field-of-view. We examine slopes of the power
spectra using power-law indices, and compare them with the unsigned magnetic
flux density averaged in the sub-regions. The thermal and kinetic spectra are
steeper than the magnetic ones at the sub-granular scale in the internetwork
regions, and the power-law indices differ by about 2. The power-law indices of
the magnetic power spectra are close to or smaller than -1 at that scale, which
suggests the total magnetic energy mainly comes from either the granular scale
magnetic structures or both the granular scale and smaller ones contributing
evenly. The slopes of the thermal and kinetic power spectra become less steep
with increasing unsigned flux density in the network regions. The power-law
indices of all the thermal, kinetic, and magnetic power spectra become similar
when the unsigned flux density is larger than 200 Mx cm^-2.
