disk with the ‘good’ local aspect ratio that allows them not to migrate any more.

The reason of this parametric dependence of the evolution on $H/r$ is quite clear if one looks at the gas density profile at the moment when the planets are released (Fig. \[profiles\]). As explained in Crida et al. (2006), the disk aspect ratio governs the width and the depth of the gaps opened by the planets. Therefore, if $H/r$ is large, there is more gas at the location of Saturn (i.e. just outside Jupiter’s orbit) than in the case where $H/r$ is small. Consistently, there is slightly less gas inside of Jupiter’s orbit (for $r<0.7$), because less material has been removed from the common gap formed by the two planets. As MS01 correctly pointed out, the direction of migration of Jupiter depends on the balance of the torques that the planet receives respectively from the disk inside its orbit (which pushes the planet outward) and and from the disk outside its orbit (which pushes the planet inward). In the case of an isolated planet, the torque from the outer disk is typically stronger, so that the planet migrates toward the Sun. But in this case, 