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Recent three-dimensional magnetohydrodynamical simulations have identified adisk wind by which gas materials are lost from the surface of a protoplanetarydisk, which can significantly alter the evolution of the inner disk and theformation of terrestrial planets. A simultaneous description of the realisticevolution of the gaseous and solid components in a disk may provide a clue forsolving the problem of the mass concentration of the terrestrial planets in thesolar system. We simulate the formation of terrestrial planets from planetaryembryos in a disk that evolves via magnetorotational instability and a diskwind. The aim is to examine the effects of a disk wind on the orbital evolutionand final configuration of planetary systems. We perform N-body simulations ofsixty 0.1 Earth-mass embryos in an evolving disk. The evolution of the gassurface density of the disk is tracked by solving a one-dimensional diffusionequation with a sink term that accounts for the disk wind. We find that even inthe case of a weak disk wind, the radial slope of the gas surface density ofthe inner disk becomes shallower, which slows or halts the type I migration ofembryos. If the effect of the disk wind is strong, the disk profile issignificantly altered (e.g., positive surface density gradient, inside-outevacuation), leading to outward migration of embryos inside ~ 1 AU. Disk windsplay an essential role in terrestrial planet formation inside a few AU bychanging the disk profile. In addition, embryos can undergo convergentmigration to ~ 1 AU in certainly probable conditions. In such a case, thecharacteristic features of the solar system's terrestrial planets (e.g., massconcentration around 1 AU, late giant impact) may be reproduced.

Formation of terrestrial planets in disks evolving via disk winds and implications for the origin of the solar system's terrestrial planets