  In weakly ionized discs turbulence can be generated through the vertical
shear instability (VSI). Embedded planets feel a stochastic component in the
torques acting on them which can impact their migration. In this work we study
the interplay between a growing planet embedded in a protoplanetary disc and
the VSI-turbulence. We performed a series of three-dimensional hydrodynamical
simulations for locally isothermal discs with embedded planets in the mass
range from 5 to 100 Earth masses. We study planets embedded in an inviscid disc
that is VSI unstable, becomes turbulent and generates angular momentum
transport with an effective $\alpha = 5 \cdot 10^{-4}$. This is compared to the
corresponding viscous disc using exactly this $\alpha$-value.
  In general we find that the planets have only a weak impact on the disc
turbulence. Only for the largest planet ($100 M_\oplus$) the turbulent activity
becomes enhanced inside of the planet. The depth and width of a gap created by
the more massive planets ($30, 100 M_\oplus$) in the turbulent disc equal
exactly that of the corresponding viscous case, leading to very similar torque
strengths acting on the planet, with small stochastic fluctuations for the VSI
disc. At the gap edges vortices are generated that are stronger and longer
lived in the VSI disc. Low mass planets (with $M_p \leq 10 M_\oplus$) do not
open gaps in the disc in both cases but generate for the turbulent disc an
over-density behind the planet that exerts a significant negative torque. This
can boost the inward migration in VSI turbulent discs well above the Type I
rate.
  Due to the finite turbulence level in realistic three-dimensional discs the
gap depth will always be limited and migration will not stall in inviscid
discs.
