Migration coefficient, ƒ_I,visc, as a function of distance to the star and planet mass for a solar-mass star with a disc size of 71 AU at t = 0. Inside of the transition radius (~5 AU), the disc is viscously heated, and for certain masses, the planet experiences outward migration. The sharp switch to inward migration at ~0.2 AU is caused by the significant decrease in opacity due to the evaporation of silicate and metal grains, which occurs at ~1000 K. We also show ƒ_I,visc at different times and for different stellar masses and disc sizes in Appendix B.