Individual torque components of the Paardekooper et al. (2011) and Jiménez & Masset (2017) formulae for planets at 3 AU and 1 Myr, depending on planetary mass. The Jiménez & Masset (2017) formula adds new contributions, but the total torque looks similar. This is just one arbitrarily chosen set of disk evolution time and position in the disk, which manifests many general trends. Outwards migration occurs when the total torque is positive. This plot shows outwards migration caused by the heating torque (see Sect. 4) for small planets as well as outwards migration caused by the corotation torques for slightly heavier planets. The pebble flux through the disk is , which is relevant for the thermal torque as discussed in Sect. 4. The viscosity is set to α = 5.4 × 10⁻³ during these simulations.