  High cadence, multi-wavelength observations and simulations are employed for
the analysis of solar photospheric magnetic bright points (MBPs) in the quiet
Sun. The observations were obtained with the Rapid Oscillations in the Solar
Atmosphere (ROSA) imager and the Interferometric BIdimensional Spectrometer
(IBIS) at the Dunn Solar Telescope. Our analysis reveals that photospheric MBPs
have an average transverse velocity of approximately 1 km/s, whereas their
chromospheric counterparts have a slightly higher average velocity of 1.4 km/s.
Additionally, chromospheric MBPs were found to be around 63% larger than the
equivalent photospheric MBPs. These velocity values were compared with the
output of numerical simulations generated using the MURaM code. The simulated
results were similar, but slightly elevated, when compared to the observed
data. An average velocity of 1.3 km/s was found in the simulated G-band images
and an average of 1.8 km/s seen in the velocity domain at a height of 500 km
above the continuum formation layer. Delays in the change of velocities were
also analysed. Average delays of ~4 s between layers of the simulated data set
were established and values of ~29 s observed between G-band and Ca II K ROSA
observations. The delays in the simulations are likely to be the result of
oblique granular shock waves, whereas those found in the observations are
possibly the result of a semi-rigid flux tube.
