Resurgence of CO in a warm bubble around accreting protoplanets and its observability

Open Access

Fig. A.1

Top: Midplane radial mass flux of large dust grains in a planetocentric coordinate frame. The composite color gradient shows log ${\dot{M}}_{p c}$ $\dot{\mathcal{M}}_{pc}$ wherever ${\dot{M}}_{p c} > 0$ $\dot{\mathcal{M}}_{pc}>0$ (red; flux towards the planet) and $log | {\dot{M}}_{p c} |$ $\log |\dot{\mathcal{M}}_{pc}|$ wherever ${\dot{M}}_{p c} < 0$ $\dot{\mathcal{M}}_{pc}<0$ (blue; flux away from the planet). The underlying planetocentric mesh was only used for the purpose of calculating ${\dot{M}}_{p c}$ $\dot{\mathcal{M}}_{pc}$ ; it does not correspond to the mesh used in our hydrodynamic simulations. The black circle marks the Hill radius. The green isocontour is where ${\dot{M}}_{p c} = 0$ $\dot{\mathcal{M}}_{pc}=0$ . Bottom: Flow topology of large dust grains obtained with the line integral convolution (LIC) method. Individual columns (left to right, respectively) correspond to simulation times t =375, 400, and 425 orbits.

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