Millimeter sized dust grains experience radial velocities exceeding gas values by orders of magnitude. The viscous evolution of the accretion disk adds disk material onto the central star's convective envelope, influencing its elemental abundances [X/H]. At the same time, the envelope mass shrinks as the stellar age increases, amplifying the rate of abundance change. Therefore, the elemental abundances of the star are sensitive to disk processes and model parameters that alter the composition and timing of disk accretion. Numerical 1D log-radial simulations integrating the disk advection-diffusion equation reveal a peak of refractory abundance within the first 2 Myr of Δ[X/H] ~ 5×10<sup>-2</sup> if grain growth is significant, but subsequent volatile-dominated accretion diminishes previous refractory abundance increases for long-lived disks. Planet formation can reduce the abundance of dust species whose ice lines lie within the planet's orbit by preventing solids from reaching the inner edge once the pebble isolation mass limit is reached. We expect the accretion of the Solar protoplanetary disk with Jupiter present to have changed the Sun's elemental abundances by ~ 1×10<sup>-2</sup> throughout its lifetime. These considerations are also applied to the HD106515 wide binary system, where measurements of Δ[X/H] are in reasonable agreement with simulation results if a giant planet formed around A, while B's disk formed planetesimals more efficiently. Simulations where the planet formed inside the water ice line are more favorable to agreement with observations.
[Poster PDF File]