  Fast inward migration of planetary cores is a common problem in the current
planet formation paradigm. Even though dust is ubiquitous in protoplanetary
disks, its dynamical role in the migration history of planetary embryos has not
been assessed. In this Letter, we show that the scattered pebble-flow induced
by a low-mass planetary embryo leads to an asymmetric dust-density distribution
that is able to exert a net torque. By analyzing a large suite of multifluid
hydrodynamical simulations addressing the interaction between the disk and a
low-mass planet on a fixed circular orbit, and neglecting dust feedback onto
the gas, we identify two different regimes, gas- and gravity-dominated, where
the scattered pebble-flow results in almost all cases in positive torques. We
collect our measurements in a first torque map for dusty disks, which will
enable the incorporation of the effect of dust dynamics on migration into
population synthesis models. Depending on the dust drift speed, the dust-to-gas
mass ratio/distribution and the embryo mass, the dust-induced torque has the
potential to halt inward migration or even induce fast outward migration of
planetary cores. We thus anticipate that dust-driven migration could play a
dominant role during the formation history of planets. Because dust torques
scale with disk metallicity, we propose that dust-driven outward migration may
enhance the occurrence of distant giant planets in higher-metallicity systems.
