Orbital migration of low-mass planets in evolutionary radiative models: Avoiding catastrophic infall

Understand

Outward migration of low-mass planets has recently been shown to be a possibility in non-barotropic disks.

• We examine the consequences of this result in evolutionary models of protoplanetary disks.
• Planet migration occurs towards equilibrium radii with zero torque.
• These radii themselves migrate inwards because of viscous accretion and photoevaporation.