Migration of Earth-sized planets in 3D radiative discs

摘要: In this paper, we address the migration of small mass planets in 3D radiative disks. Indeed, is known to be too fast inwards locally isothermal conditions. However, thermal effects could reverse its direction, potentially saving inner, optically thick parts protoplanetary disc. This effect has been seen for masses larger than 5 Earth masses, but minimum happen never probed numerically, although it crucial importance planet formation scenarios. We have extended hydro-dynamical code FARGO 3D, with diffusion. With code, perform simulations embedded down 2 masses. For a set discs parameters which outward shown range $[5, 35]$ find that transition inward occurs $[3, 5]$ The appears due an unexpected phenomenon: asymmetric cold and dense finger gas driven by circulation libration streamlines. recover phenomenon 2D where control cooling through simple modeling energy equation.