  A key process in planet formation is the exchange of angular momentum between
a growing planet and the protoplanetary disc, which makes the planet migrate
through the disc. Several works show that in general low-mass and
intermediate-mass planets migrate towards the central star, unless corotation
torques become dominant. Recently, a new kind of torque, called the thermal
torque, was proposed as a new source that can generate outward migration of
low-mass planets. While the Lindblad and corotation torques depend mostly on
the properties of the protoplanetary disc and on the planet mass, the thermal
torque depends also on the luminosity of the planet, arising mainly from the
accretion of solids. Thus, the accretion of solids plays an important role not
only in the formation of the planet but also in its migration process. In a
previous work, we evaluated the thermal torque effects on planetary growth and
migration mainly in the planetesimal accretion paradigm. In this new work, we
study the role of the thermal torque within the pebble accretion paradigm.
Computations are carried out consistently in the framework of a global model of
planet formation that includes disc evolution, dust growth and evolution, and
pebble formation. We also incorporate updated prescriptions of the thermal
torque derived from high resolution hydrodynamical simulations. Our simulations
show that the thermal torque generates extended regions of outward migration in
low viscosity discs. This has a significant impact in the formation of the
planets.
