  We investigate planetary migration in the dead zone of a protoplanetary disk
where there are a set of spiral waves propagating inward due to the turbulence
in the active zone and the Rossby wave instability (RWI), which occurs at the
transition between the dead and active zones. We perform global 3D unstratified
magnetohydrodynamical (MHD) simulations of a gaseous disk with the FARGO3D
code, using weak gradients in the static resistivity profiles that trigger the
formation of a vortex at the outer edge of the dead zone. We find that once the
Rossby vortex develops, spiral waves in the dead zone emerge and interact with
embedded migrating planets by wave interference, which notably changes their
migration. The inward migration becomes faster depending on the mass of the
planet, due mostly to the constructive (destructive) interference between the
outer (inner) spiral arm of the planet and, the destruction of the dynamics of
the horseshoe region by means of the set of background spiral waves propagating
inward. The constructive wave interference produces a more negative Lindblad
differential torque which inevitably leads to an inward migration. Lastly, for
massive planets embedded in the dead zone, we find that the spiral waves can
create an asymmetric wider and depeer gap than in the case of $\alpha$-disks,
and can prevent the formation of vortices at the outer edge of the gap. The
latter could generate a faster or slower migration compared to the standard
type-II migration.
