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The motion of faint propagating disturbances (PD) in the solar corona revealsan intricate structure which must be defined by the magnetic field. Applied toquiet Sun observations by the Atmospheric Imaging Assembly (AIA)/Solar DynamicsObservatory (SDO), a novel method reveals a cellular network, with cells oftypical diameters 50\arcsec\ in the cool 304\AA\ channel, and 100\arcsec\ inthe coronal 193\AA\ channel. The 193\AA\ cells can overlie several 304\AA\cells, although both channels share common source and sink regions. The sourcesare points, or narrow corridors, of divergence that occupy the centres ofcells. They are significantly aligned with photospheric network features andenhanced magnetic elements. This shows that the bright network is important tothe production of PDs, and confirms that the network is host to the sourcefootpoint of quiet coronal loops. The other footpoint, or the sinks of the PDs,form the boundaries of the coronal cells. These are not significantly alignedwith the photospheric network - they are generally situated above the darkinternetwork photosphere. They form compact points or corridors, often withoutan obvious signature in the underlying photosphere. We argue that these sinkpoints can either be concentrations of closed field footpoints associated withminor magnetic elements in the internetwork, or concentrations ofupward-aligned open field. The link between the coronal velocity and magneticfields is strengthened by a comparison with a magnetic extrapolation, whichshows several general and specific similarities, thus the velocity maps offer avaluable additional constraint on models.

Tracing the magnetic field topology of the quiet corona using propagating disturbances