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We explore dust flow in the hottest parts of protoplanetary discs using theforces of gravity, gas drag and radiation pressure. Our main focus is on theoptically thin regions of dusty disc, where the dust is exposed to the mostextreme heating conditions and dynamical perturbations: the surface ofoptically thick disc and the inner dust sublimation zone. We utilise resultsfrom two numerically strenuous fields of research. The first is thequasi-stationary solutions on gas velocity and density distributions frommangetohydrodynamical (MHD) simulations of accretion discs. This is criticalfor implementing a more realistic gas drag impact on dust movements. The secondis the optical depth structure from a high-resolution dust radiation transfer.This step is critical for a better understanding of dust distribution withinthe disc. We describe a numerical method that incorporates these solutions intothe dust dynamics equations. We use this to integrate dust trajectories underdifferent disc wind models and show how grains end up trapped in flows thatrange from simple accretion onto the star to outflows into outer disc regions.We demonstrate how the radiation pressure force plays one of the key roles inthis process and cannot be ignored. It erodes the dusty disc surface, reducesits height, resists dust accretion onto the star, and helps the disc wind inpushing grains outwards. The changes in grain size and porosity significantlyaffect the results, with smaller and porous grains being influenced morestrongly by the disc wind and radiation pressure.

Inner dusty regions of protoplanetary discs -- II. Dust dynamics driven by radiation pressure and disc winds