Overview of a slice of the gas velocity field in the same plane as in Figs. 8 and 9. Arrows correspond to the radial and vertical components of the velocity on the slice and the colour shows the norm of the full 3D velocity. Most of the gas accreted by the planet enters the Hill sphere through the midplane and the tilted spiral arm shocks.The spiral arms give vertical kicks to the passing flows, forcing them to flow along the shock downwards into the midplane, where a region of increased compression is generated, marked with (b) in Figs. 8 and 9. This gas then decompresses and free-falls onto the CPD. However, the majority of the incoming gas is eventuallyaccreted by the planet. This happens either after some residing time in the CPD or by directly flowing over the CPD and colliding with flow from the opposite side of the Hill radius. We note that the global meridional circulation noted in the isothermal runs of Morbidelli et al. (2014) is an azimuthally averaged feature and is therefore not visible in this slice.