  Due to their aerodynamical coupling with gas, pebbles in protoplanetary discs
can drift over large distances to support planet growth in the inner disc. In
the past decade, this pebble accretion has been studied extensively for
aerodynamically small pebbles (Stokes number St < 1). However, accretion can
also operate in the St > 1 mode, e.g., when planetesimals collisionally
fragment to smaller bodies or when the primordial gas disc disperses. This work
aims to extend the study of pebble accretion to these aerodynamically loosely
coupled particles. We integrate the pebble's equation of motion, accounting for
gas drag, stellar and planetary gravity, in the midplane of a laminar disc. The
accretion probability ($\epsilon$) is calculated as function of Stokes number,
disc pressure gradient index, planet mass and eccentricity. We find that for
Stokes number above unity $\epsilon$(St) first rises, due to lower drift and
aided by a large atmospheric capture radius, until it reaches a plateau where
the efficiency approaches 100 per cent. At high St the plateau region
terminates as particles become trapped in resonance. These results are well
described by a semi-analytical "kick-and-drift" model and we also provide fully
analytical prescriptions for $\epsilon$. We apply our model to the accretion of
$\sim 30 \mu$m dust particles in a dispersing protoplanetary and secondary
(CO-rich) debris disc. It shows that physically small particles are mainly
accreted as aerodynamically large Stokes number pebbles during the debris disc
phase. Earth-mass planets may obtain $\sim 25$ per cent of their heavy elements
through this late accretion phase.
