  Magnetic bright points in the solar photosphere, visible in both continuum
and G-band images, indicate footpoints of kilogauss magnetic flux tubes
extending to the corona. The power spectrum of bright-point motion is thus also
the power spectrum of Alfven wave excitation, transporting energy up flux tubes
into the corona. This spectrum is a key input in coronal and heliospheric
models. We produce a power spectrum of bright-point motion using radiative
magnetohydrodynamic simulations, exploiting spatial resolution higher than can
be obtained in present-day observations, while using automated tracking to
produce large data quantities. We find slightly higher amounts of power at all
frequencies compared to observation-based spectra, while confirming the
spectrum shape of recent observations. This also provides a prediction for
observations of bright points with DKIST, which will achieve similar resolution
and high sensitivity. We also find a granule size distribution in support of an
observed two-population distribution, and we present results from tracking
passive tracers which show a similar power spectrum to that of bright points.
Finally, we introduce a simplified, laminar model of granulation, with which we
explore the roles of turbulence and of the properties of the granulation
pattern in determining bright-point motion.
