Fig. 5.
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Velocity vectors of the gas flow onto a disc-instability protoplanet (see Fig. 2, top) on the x − y plane (top), x − z plane (middle), and y − z plane (bottom), overplotted on the corresponding densities (in units of g cm−3). Gas infall velocities onto the protoplanet are asymmetric; higher velocities are seen towards the poles of the protoplanet.
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