Growth tracks of planets that have been inserted at different radii after 1 Myr with the Jiménez & Masset (2017) formula (no thermal torque) in black and the Jiménez & Masset (2017) + Masset (2017) formula (includes thermal torque) in red. The lines become dashed when the planets reach pebble isolation mass and are accreting gas. An increased pebble flux of was used to achieve a larger contribution from the thermal torque. After performing significant outwards migration, planets thatgrow with the thermal torque migrate to the star quickly and grow less massive than the planets that were evolved without thermal torque, which reach runaway gas accretion. This might be due to the fact that heavier planets migrate faster, which gives them less time to contract an envelope before reaching the inner edge of the disk.