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Low-mass planets that are in the process of growing larger withinprotoplanetary disks exchange torques with the disk and change their semi-majoraxis accordingly. This process is called type I migration and is stronglydependent on the underlying disk structure. As a result, there are manyuncertainties about planetary migration in general. In a number of simulations,the current type I migration rates lead to planets reaching the inner edge ofthe disk within the disk lifetime. A new kind of torque exchange between planetand disk, the thermal torque, aims to slow down inward migration via theheating torque. The heating torque may even cause planets to migrate outwards,if the planetary luminosity is large enough. Here, we study the influence onplanetary migration of the thermal torque on top of previous type I models. Wefind that the formula of Paardekooper et al. (2011) allows for more outwardmigration than that of Jim\'enez & Masset (2017) in most configurations, but wealso find that planets evolve to very similar mass and final orbital radiususing both formulae in a single planet-formation scenario, including pebble andgas accretion. Adding the thermal torque can introduce new, but small, regionsof outwards migration if the accretion rates onto the planet correspond totypical solid accretion rates following the pebble accretion scenario. If theaccretion rates onto the planets become very large, as could be the case inenvironments with large pebble fluxes (e.g., high-metallicity environments),the thermal torque can allow more efficient outward migration. However, eventhen, the changes for the final mass and orbital positions in our planetformation scenario are quite small. This implies that for single planetevolution scenarios, the influence of the heating torque is probablynegligible.

Influence of migration models and thermal torque on planetary growth in the pebble accretion scenario