Dusty photoevaporation in protoplanetary discs

Planets form from tiny dust grains that grow within thick gas discs around young stars. We can observe these discs due to size-dependent thermal emission from dust so knowing the locations and behaviour of each grain size is important. We develop new hydrodynamic and semi-analytic models that shed new light on dust dynamics at the surface of discs undergoing photoevaporation from the central star. From these models, we can infer a maximum entrainable grain size as a function of disc/stellar properties and predict whether settling of dust within the disc affects which grains are carried into the wind.