MHD wave phenomena have been readily observed in recent years in various magnetic elements found within the solar atmosphere. They are often touted as a possible mechanism in channeling energy to the outer layers of the solar atmosphere. Recent advances in both observational techniques and instrumentation has gradually bridged the gap between observations and theory of these phenomena, as various wave modes have been identified and their properties studied across a wide range of structures. For example, numerous contemporary studies have identified and studied the properties associated with compressible sausage modes in different bandpasses, often employing magnetic pores as a test bed. However, the spatial structuring of the mode within the flux tube, that is, the surface and body characteristics, has thus far been ignored in observational studies. We employed high spatial and temporal resolution observations from a combination of both ground- (ROSA) and space-based (SDO) instrumentation to study several pore datasets, which were observed to support sausage modes. Using a range of techniques, we observed and were able to classify, for the first time, the surface and body characteristics for the wave modes observed within the pores. The most frequently occurring oscillation period in our observations was found to be ~300s, which is consistent with the p-mode spectrum. We find surface modes more frequently in the data. We find frequencies in the range of ~2–12 mHz, with body modes as high as 11 mHz, but we do not find surface modes above 10 mHz. Estimates made for the energetics of these wave modes will also be discussed within the context of our results.
