  Millimeter sized dust grains experience radial velocities exceeding the gas
velocities 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 over
time, amplifying the rate of abundance change. Therefore, the elemental
abundances of the star are sensitive to disk processes that alter the
composition and timing of disk accretion. We perform numerical 1D log-radial
simulations integrating the disk advection-diffusion equation, accounting for
phase transitions of chemical species at the evaporation fronts. They reveal a
peak of refractory abundance within the first 2 Myr of
$\Delta\mathrm{[X/H]}\sim 5\times 10^{-2}$ if grain growth is significant, but
subsequent accretion diminishes previous refractory abundance increases for
long-lived disks. Planet formation can reduce the abundance of dust species
whose evaporation fronts lie within the planet's orbit by opening a gap and
consequently blocking inward drifting pebbles. We expect the accretion of the
Solar protoplanetary disk with Jupiter present to have changed the Sun's
elemental abundances by ${\sim}10^{-2}$ throughout its lifetime. These
considerations are also applied to the HD106515 wide binary system. We find
that measurements of $\Delta\mathrm{[X/H]}$ are in reasonable agreement with
results from simulations where the observed giant planet around HD106515 A is
included and if HD106515B's disk formed planetesimals more efficiently.
Simulations where the planet formed inside the water ice line are more
favorable to agree with observations. Even though the general changes in the
stellar abundances due to disk accretion are small, they are detectable at
current sensitivities, indicating that the here presented methods can be used
to constrain the planet formation pathway.
