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We describe the characteristics and evolution of the magnetic field andchromospheric emission in an active region core observed by the Solar OpticalTelescope on Hinode. Consistent with previous studies, we find that the moss isunipolar, the spatial distribution of magnetic flux evolves slowly, and themagnetic field is only moderately inclined. We show that the field lineinclination and horizontal component are coherent, and that the magnetic fieldis mostly sheared in the inter-moss regions where the highest magnetic fluxvariability is seen. Using extrapolations from SP magnetograms we show that themagnetic connectivity in the moss is different than in the quiet Sun becausemost of the magnetic field extends to significant coronal heights. The magneticflux, field vector, and chromospheric emission in the moss also appear highlydynamic, but actually show only small scale variations in magnitude ontime-scales longer than the cooling times for hydrodynamic loops computed fromour extrapolations, suggesting high-frequency (continuous) heating events. Someevidence is found for flux (Ca 2 intensity) changes on the order of 100--200 G(DN) on time-scales of 20--30 mins that could be taken as indicative oflow-frequency heating. We find, however, that only a small fraction (10%) ofour simulated loops would be expected to cool on these time-scales, and we findno clear evidence that the flux changes consistently produce intensity changesin the chromosphere. The magnetic flux and chromospheric intensity in mostindividual SOT pixels in the moss vary by less than ~ 20% and ~ 10%,respectively, on loop cooling time-scales. In view of the high energyrequirements of the chromosphere, we suggest that these variations could besufficient for the heating of `warm' EUV loops, but that the high basal levelsmay be more important for powering the hot core loops rooted in the moss.

Characteristics and Evolution of the Magnetic field and Chromospheric Emission in an Active Region Core Observed by Hinode