Pablo Benı´tez-Llambay1, Fre´de´ric Masset2, Gloria Koenigsberger2 & Judit Szula´gyi3
Planetary systems are born in the disks of gas, dust and rocky fragments that surround newly formed stars. Solid content assembles into ever-larger rocky fragments that eventually become planetary embryos. These then continue their growth by accreting leftover material in the disk. Concurrently, tidal effects in the disk cause a radial drift in the embryo orbits, a process known as migration1–4. Fast inward migration is predicted by theory for embryos smaller than three to fiveEarthmasses5–7. With only inwardmigration, these embryos can only rarely become giant planets located at Earth’s distance fromthe Sunand beyond8,9, incontrastwith observations10. Here we report that asymmetries in the temperature rise associated with accreting infalling material11,12 produce a force (which gives rise to an effect thatwe call ‘heating torque’) that counteracts inward migration.This provides a channel for the formation of giant planets 8 and also explains the strong planet–metallicity correlation found between the incidence of giant planets and the heavy-element abundance of the host stars13,14.