  In a previous work, we investigated the evolution of the flow field around
sunspots during sunspot decay and compared it with the flow field of
supergranular cells. The decay of a sunspot proceeds as it interacts with its
surroundings. This is manifested by the changes observed in the flow field
surrounding the decaying spot. We now investigate in detail the evolution of
the flow field in the direct periphery of the sunspots of the same sample and
aim to provide a complete picture of the role of large-scale flows present in
sunspot cells. We analyse the horizontal velocity profiles of sunspots obtained
from observations by the Helioseismic and Magnetic Imager (HMI) on board the
Solar Dynamics Observatory (SDO). We follow their evolution across the solar
disc from their stable phase to their decay and their final disappearance. We
find two different scenarios for the evolution of the flow region surrounding a
spot in the final stage of its decay: (i) either the flow cell implodes and
disappears under the action of the surrounding supergranules or (ii) it
outlives the spot. In the later case, an inwards flow towards the remaining
naked spot develops in the vicinity closest to the spot followed by an outflow
further out. These findings provide observational evidence to theoretical
predictions by realistic magnetohydrodynamic (MHD) sunspot and moat region
simulations. The Evershed flow and the moat flow, both connected to the
presence of fully fledged sunspots in a spot cell, vanish when penumbrae decay.
Moat flows decline into supergranular flows. The final fate of a spot cell
depends on its interaction with the surrounding supergranular cells. In the
case of non-imploding spot cells, the remaining naked spot develops a
converging inflow driven by radiative cooling and a geometrical alignment of
granules in its periphery which is similar to that observed in pores.
