Same as Fig. 2, but now for a 12 M_Jup planet. Note that the accretion disk is substantially larger than in the 1 M_Jup case. a) The H₂O ice line appears much later than in the Jovian scenario, here at 1.334 Myr. The planetary accretion rate is about 10³M_Gan Myr^-1 and viscous heating is dominant in this phase. b) Once the planetary accretion rate has dropped to 10 M_Gan Myr^-1 at 1.43 Myr, the H₂O ice line is at a similar location as in the Jupiter-like scenario, that is, between the orbits of Europa and Ganymede.