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We investigate under what circumstances an embedded planet in aprotoplanetary disc may sculpt the dust distribution such that itobservationally presents as a `transition' disc. We concern ourselves with`transition' discs that have large holes ($\gtrsim 10$ AU) and high accretionrates ($\sim 10^{-9}-10^{-8}$ M$_\odot$ yr$^{-1}$). Particularly, those discswhich photoevaporative models struggle to explain. Assuming the standardpicture for how massive planets sculpt their parent discs, along with theobserved accretion rates in `transition' discs, we find that the accretionluminosity from the forming planet is significant, and can dominate over thestellar luminosity at the gap edge. This planetary accretion luminosity canapply a significant radiation pressure to small ($s\lesssim 1\mu$m) dustparticles provided they are suitably decoupled from the gas. Secular evolutioncalculations that account for the evolution of the gas and dust components in adisc with an embedded, accreting planet, show that only with the addition ofthe radiation pressure can we explain the full observed characteristics of a`transition' disc (NIR dip in the SED, mm cavity and high accretion rate). Atsuitably high planet masses ($\gtrsim 3-4$ M$_J$), radiation pressure from theaccreting planet is able to hold back the small dust particles, producing aheavily dust-depleted inner disc that is optically thin (vertically andradially) to Infra-Red radiation. We use our models to calculate syntheticobservations and present a observational evolutionary scenario for a formingplanet, sculpting its parent disc. The planet-disc system will present as a`transition' disc with a dip in the SED, only when the planet mass andplanetary accretion rate is high enough. At other times it will present as adisc with a primordial SED, but with a cavity in the mm, as observed in ahandful of protoplanetary discs.

Accreting planets as dust dams in `transition' discs