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High angular resolution observations of discs at mm wavelengths (on scales ofa few au) are now commonplace, but there is a current lack of a comparableangular resolution for observations at cm wavelengths. This presents asignificant barrier to improving our understanding of planet formation, inparticular how dust grains grow from mm to cm sizes. In this paper, we examinethe ability of the Square Kilometre Array (SKA) to observe dust substructure ina young, planet-forming disc at cm wavelengths. We use dusty hydrodynamics andcontinuum radiative transfer to predict the distribution and emission of 1 cmdust grains (or pebbles) within the disc, and simulate continuum observationswith the current SKA1-MID design baseline at frequencies of 12.5 GHz (Band 5b,~2.4 cm) on 5-10 au scales. The SKA will provide high-fidelity observations ofthe cm dust emission substructure in discs for integration times totalling100's of hours. Radial structure can be obtained at a sufficient resolution andS/N from shorter (10's of hours) integration times by azimuthal averaging inthe image plane. By modelling the intensity distribution directly in thevisibility plane, it is possible to recover a similar level of (axisymmetric)structural detail from observations with integration times 1-2 orders ofmagnitude lower than required for high-fidelity imaging. Our resultsdemonstrate that SKA1-MID will provide crucial constraints on the distributionand morphology of the raw material for building planets, the pebbles inprotoplanetary discs.

Observing protoplanetary discs with the Square Kilometre Array -- I. Characterising pebble substructure caused by forming planets