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We present high-cadence observations and simulations of the solarphotosphere, obtained using the Rapid Oscillations in the Solar Atmosphereimaging system and the MuRAM magneto-hydrodynamic code, respectively. Eachdataset demonstrates a wealth of magneto-acoustic oscillatory behaviour,visible as periodic intensity fluctuations with periods in the range 110-600 s.Almost no propagating waves with periods less than 140s and 110s are detectedin the observational and simulated datasets, respectively. High concentrationsof power are found in highly magnetised regions, such as magnetic bright pointsand intergranular lanes. Radiative diagnostics of the photospheric simulationsreplicate our observational results, confirming that the current breed ofmagneto-hydrodynamic simulations are able to accurately represent the lowersolar atmosphere. All observed oscillations are generated as a result ofnaturally occurring magnetoconvective processes, with no specific input driverpresent. Using contribution functions extracted from our numerical simulations,we estimate minimum G-band and 4170 Angstrom continuum formation heights of 100km and 25 km, respectively. Detected magneto-acoustic oscillations exhibit adominant phase delay of -8 degrees between the G-band and 4170 Angstromcontinuum observations, suggesting the presence of upwardly propagating waves.More than 73% of MBPs (73% from observations, 96% from simulations) displayupwardly propagating wave phenomena, suggesting the abundant nature ofoscillatory behaviour detected higher in the solar atmosphere may be tracedback to magnetoconvective processes occurring in the upper layers of the Sun'sconvection zone.

Propagating Wave Phenomena Detected in Observations and Simulations of the Lower Solar Atmosphere