  We present observational evidence of compressible magnetohydrodynamic wave
modes propagating from the solar photosphere through to the base of the
transition region in a solar magnetic pore. High cadence images were obtained
simultaneously across four wavelength bands using the Dunn Solar Telescope.
Employing Fourier and wavelet techniques, sausage-mode oscillations displaying
significant power were detected in both intensity and area fluctuations. The
intensity and area fluctuations exhibit a range of periods from 181-412s, with
an average period ~290s, consistent with the global p-mode spectrum. Intensity
and area oscillations present in adjacent bandpasses were found to be
out-of-phase with one another, displaying phase angles of 6.12 degrees, 5.82
degrees and 15.97 degrees between 4170 Angstrom continuum - G-band, G-band - Na
I D1 and Na I D1 - Ca II K heights, respectively, reiterating the presence of
upwardly-propagating sausage-mode waves. A phase relationship of ~0 degrees
between same-bandpass emission and area perturbations of the pore best
categorises the waves as belonging to the `slow' regime of a dispersion
diagram. Theoretical calculations reveal that the waves are surface modes, with
initial photospheric energies in excess of 35000 W/m^2. The wave energetics
indicate a substantial decrease in energy with atmospheric height, confirming
that magnetic pores are able to transport waves that exhibit appreciable energy
damping, which may release considerable energy into the local chromospheric
plasma.

Solar and Stellar Astrophysics