Evolution of the global disk dust-to-gas ratio of all matching simulations with the Ricci et al. (2010) R10-0 opacity model, for three different cases and three different snapshots, from 300 kyr-3 Myr. From left to right, the smooth case, a planet with planet/star mass ratio at 1/3r_c, and a planet with the same ratio at 2/3r_c. Different limits are used on the x-axis to highlight the evolution of the dust-to-gas ratio. The initial dust-to-gas ratio is 0.01. For the smooth case the dust-to-gas ratio decreases by three orders of magnitude up to 3 Myr. When a planet is included the disk dust mass is retained and leads to a much higher dust-to-gas ratio. In the case where the planet is the inner part of the disk (middle column), there are cases at 3 Myr where the ratio is higher than 0.01. The gas mass moves faster than the dust mass in this case.