Fig. 6
A closeup of the gas surface density Σ (top) and pebble surface density Σp (bottom) after ≃ 5 kyr of evolution in the simulation with pebble accretion but without accretion heating, i.e. Case II. The gaps in the pebble disk are opened by accreting planetary embryos. A fourth embryo is also present in the system but it is located outside the range.
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