  The solid material of protoplanetary discs forms an asymmetric pattern around
a low-mass planet (M_p<=10M_Earth) due to the combined effect of dust-gas
interaction and the gravitational attraction of the planet. Recently, it has
been shown that although the total solid mass is negligible compared to that of
gas in protoplanetary discs, a positive torque can be emerged by a certain size
solid species. The torque magnitude can overcome that of gas which may result
in outward planetary migration. In this study, we show that the accretion of
solid species by the planet strengthens the magnitude of solid torque being
either positive or negative. We run two-dimensional, high-resolution (1.5Kx3K)
global hydrodynamic simulations of an embedded low-mass planet in a
protoplanetary disc. The solid material is handled as a pressureless fluid.
Strong accretion of well-coupled solid species by a M_p<0.3M_Earth protoplanet
results in the formation of such a strongly asymmetric solid pattern close to
the planet that the positive solid torque can overcome that of gas by two
times. However, the accretion of solids in the pebble regime results in
increased magnitude negative torque felt by protoplanets and strengthened
positive torque for Earth-mass planets. For M_p>=3M_Earth planets the magnitude
of the solid torque is positive, however, independent of the accretion strength
investigated. We conclude that the migration of solid accreting planets can be
substantially departed from the canonical type-I prediction.
