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

Abstract

Recent three-dimensional magnetohydrodynamical simulations have identified a disk wind by which gas materials are lost from the surface of a protoplanetary disk, which can significantly alter the evolution of the inner disk and the formation of terrestrial planets. A simultaneous description of the realistic evolution of the gaseous and solid components in a disk may provide a clue for solving the problem of the mass concentration of the terrestrial planets in the solar system. We simulate the formation of terrestrial planets from planetary embryos in a disk that evolves via magnetorotational instability and a disk wind. The aim is to examine the effects of a disk wind on the orbital evolution and final configuration of planetary systems. We perform N-body simulations of sixty 0.1 Earth-mass embryos in an evolving disk. The evolution of the gas surface density of the disk is tracked by solving a one-dimensional diffusion equation with a sink term that accounts for the disk wind. We find that even in the case of a weak disk wind, the radial slope of the gas surface density of the inner disk becomes shallower, which slows or halts the type I migration of embryos. If the effect of the disk wind is strong, the disk profile is significantly altered (e.g., positive surface density gradient, inside-out evacuation), leading to outward migration of embryos inside ~ 1 AU. Disk winds play an essential role in terrestrial planet formation inside a few AU by changing the disk profile. In addition, embryos can undergo convergent migration to ~ 1 AU in certainly probable conditions. In such a case, the characteristic features of the solar system's terrestrial planets (e.g., mass concentration around 1 AU, late giant impact) may be reproduced.

8 pages, 4 figures, accepted for publication in A&A

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Cited by in corpus (11)

• Evolution of Protoplanetary Discs with Magnetically Driven Disc Winds
• Can dead zones create structures like a transition disk?
• A reassessment of the in situ formation of close-in super-Earths
• The Galilean Satellites Formed Slowly from Pebbles
• Evolution of the Water Snow Line in Magnetically Accreting Protoplanetary Disks
• Population study on MHD wind-driven disc evolution -- Confronting theory and observation
• The Roles of Dust Growth in the Temperature Evolution and Snow Line Migration in Magnetically Accreting Protoplanetary Disks
• Effects of global gas flows on type I migration
• Structure of Protoplanetary Discs with Magnetically-driven Winds
• The late formation of chondrites as a consequence of Jupiter-induced gaps and rings
• Early Initiation of Inner Solar System Formation at Dead-Zone Inner Edge