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 .