Issue |
A&A
Volume 579, July 2015
|
|
---|---|---|
Article Number | A65 | |
Number of page(s) | 8 | |
Section | Planets and planetary systems | |
DOI | https://doi.org/10.1051/0004-6361/201525636 | |
Published online | 29 June 2015 |
Formation of terrestrial planets in disks evolving via disk winds and implications for the origin of the solar system’s terrestrial planets
1
Observatoire de la Côte d’Azur, Boulevard de l’Observatoire,
06304
Nice Cedex 4,
France
e-mail: omasahiro@oca.eu
2
Nagoya University, Furo-cho, Chikusa-ku, Nagoya, Aichi
464-8602,
Japan
Received:
9
January
2015
Accepted:
20
April
2015
Context. 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.
Aims. 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.
Methods. 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.
Results. 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.
Conclusions. 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.
Key words: planets and satellites: formation / protoplanetary disks / planet-disk interactions
© ESO, 2015
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