  Over the past number of years, great strides have been made in identifying
the various low-order magnetohydrodynamic wave modes observable in a number of
magnetic structures found within the solar atmosphere. However, one aspect of
these modes that has remained elusive, until now, is their designation as
either surface or body modes. This property has significant implications on how
these modes transfer energy from the waveguide to the surrounding plasma. Here,
for the first time to our knowledge, we present conclusive, direct evidence of
these wave characteristics in numerous pores which were observed to support
sausage modes. As well as outlining methods to detect these modes in
observations, we make estimates of the energies associated with each mode. We
find surface modes more frequently in the data, and also that surface modes
appear to carry more energy than those displaying signatures of body modes. We
find frequencies in the range of ~2 to 12 mHz with body modes as high as 11
mHz, but we do not find surface modes above 10 mHz. It is expected that the
techniques we have applied will help researchers search for surface and body
signatures in other modes and in differing structures to those presented here.
