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Disk solids are critical in many planet formation processes, however, theireffect on planet migration remains largely unexplored. Here we assess for thefirst time this important issue by building on the systematic measurements ofdust torques on an embedded planet by Benitez-Llambay & Pessah (2018). Adoptingstandard models for the gaseous disk and its solid content, we quantify theimpact of the dust torque for a wide range of conditions describing thedisk/planet system. We show that the total torque can be positive and revertinward planet migration for planetary cores with $M_{\rm p} \lesssim 10M_\oplus$. We compute formation tracks for low-mass embryos for conditionsusually invoked when modeling planet formation processes. Our most importantconclusion is that dust torques can have a significant impact on the migrationand formation history of planetary embryos. The most important implications ofour findings are: $\it{i})$ For nominal dust-to-gas mass ratios $\epsilon\simeq 0.01$, low-mass planets migrate outwards beyond the water ice-line ifmost of the mass in solids is in particles with Stokes numbers St $\simeq 0.1$.$\it{ii})$. For $\epsilon \gtrsim 0.02-0.05$, solids with small Stokes numbers,St $\simeq 0.01$, can play a dominant role if most of the mass is in thoseparticles. $\it{iii})$ Dust torques have the potential to enable low-massplanetary cores formed in the inner disk to migrate outwards and act as theseed for massive planets at distances of tens of au.

Quantifying the Impact of the Dust Torque on the Migration of Low-mass Planets