Volume 608, December 2017
|Number of page(s)||9|
|Section||Planets and planetary systems|
|Published online||08 December 2017|
Effects of global gas flows on type I migration
1 Division of Theoretical AstronomyNational Astronomical Observatory of Japan, 2-21-1, Osawa, Mitaka, 181-8588 Tokyo, Japan
2 School of Arts & Sciences, University of Tokyo, 3-8-1, Komaba, Meguro, 153-8902 Tokyo, Japan
3 Laboratoire Lagrange, Université Côte d’Azur, Observatoire de la Côte d’Azur, CNRS, Bd de l’Observatoire, CS 34229, 06304 Nice Cedex 4, France
4 Institut Universitaire de France, 103 boulevard Saint-Michel, 75005 Paris, France
Received: 14 March 2017
Accepted: 20 September 2017
Context. Magnetically-driven disk winds would alter the surface density slope of gas in the inner region of a protoplanetary disk (r ≲ 1 au). This in turn affects planet formation. Recently, the effect of disk wind torque has been considered with the suggestion that it would carve out the surface density of the disk from inside and would induce global gas flows (wind-driven accretion).
Aims. We aim to investigate effects of global gas flows on type I migration and also examine planet formation.
Methods. A simplified approach was taken to address this issue, and N-body simulations with isolation-mass planets were also performed.
Results. In previous studies, the effect of gas flow induced by turbulence-driven accretion has been taken into account for its desaturation effect of the corotation torque. If more rapid gas flows (e.g., wind-driven accretion) are considered, the desaturation effect can be modified. In MRI-inactive disks, in which the wind-driven accretion dominates the disk evolution, the gas flow at the midplane plays an important role. If this flow is fast, the corotation torque is efficiently desaturated. Then, the fact that the surface density slope can be positive in the inner region due to the wind torque can generate an outward migration region extended to super-Earth mass planets. In this case, we observe that no planets fall onto the central star in N-body simulations with migration forces imposed to reproduce such migration pattern. We also see that super-Earth mass planets can undergo outward migration.
Conclusions. Relatively rapid gas flows affects type I migration and thus the formation of close-in planets.
Key words: planets and satellites: formation / planet-disk interactions / methods: numerical
© ESO, 2017
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