Oral Presentation

Growth of solid particles in protoplanetary disks with magnetically driven disk winds

Author(s): Koh Kuwabara(The University of Tokyo);Hiroshi Kobayashi(Nagoya University);Tetsuro Taki(The University of Tokyo);Takeru Suzuki(The University of Tokyo)

Presenter: Koh Kuwabara (The University of Tokyo)

One of the severe problems in the planet formation is "the radial drift barrier", namely solid particles accrete to the central star before growing to km-size planetesimals.
In order to investigate how the magnetically driven disk wind affects this radial drift barrier, we calculated the collisional growth of dust particles in evolving gaseous protoplanetary disks under the 1+1 D (time + radial distance) approximation.
We solved a coagulation equation of solid particles under a single-size approximation with neglecting the effect of collisional fragmentation in various conditions of turbulent viscosity and the mass loss and magnetic braking by the disk wind.
We found that a dust ring is formed in the case with weak turbulence and efficient mass loss by the disk wind.
This is because the direction of the gas-pressure gradient is reversed in the inner region and the solid component migrates radially outward to merge to another ring formed in the outer region.
On the other hand, in cases with strong turbulence the effect of the disk wind is not prominent, and the radial drift barrier cannot be overcome in these cases.