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 ^ { -1 } , whereas their chromospheric counterparts have a slightly higher average velocity of 1.4 km s ^ { -1 } .
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 ^ { -1 } was found in the simulated G-band images and an average of 1.8 km s ^ { -1 } 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 \sim 4 s between layers of the simulated data set were established and values of \sim 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 .