  Dust rings in protoplanetary discs are often observed in thermal dust
emission and could be favourable environments for planet formation. While dust
rings readily form in gas pressure maxima, their long-term stability is key to
both their observability and potential to assist in planet formation. We
investigate the stability of the dust ring generated by interactions of a
protoplanetary disc with a Neptune sized planet and consider its possible long
term evolution using the FARGO3D Multifluid code. We look at the onset of the
Rossby Wave Instability (RWI) and compare how the addition of dust in a disc
can alter the stability of the gas phase. We find that with the addition of
dust, the rings generated by planet disc interactions are more prone to RWI and
can cause the gas phase to become unstable. The instability is shown to occur
more easily for higher Stokes number dust, as it accumulates into a more narrow
ring which triggers the RWI, while the initial dust fraction plays a more minor
role in the stability properties. We show that the dusty RWI generates vortices
that collect dust in their cores, which could be sites for further planetesimal
formation. We conclude that the addition of dust can cause a ring in a
protoplanetary disc to become more prone to instability leading to a different
long term evolution compared to gas only simulations of the RWI.
