Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks

Details Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks Planet formation bursts at the borders of the dead zone in 2D numerical simulations of circumstellar disks

2009-01-12

arxiv.org/abs/0901.1638v4

Astronomy and Astrophysics

Astrophysics

Earth and Planetary Astrophysics

19 pages, 15 figures + Appendices. Accepted by A&A. Nature of replacement: included a missing reference

Scientific paper

10.1051/0004-6361/200811265

As accretion in protoplanetary disks is enabled by turbulent viscosity, the border between active and inactive (dead) zones constitutes a location where there is an abrupt change in the accretion flow. The gas accumulation that ensues triggers the Rossby wave instability, that in turn saturates into anticyclonic vortices. It was suggested that the trapping of solids within them leads to a burst of planet formation on very short timescales. We perform two-dimensional global simulations of the dynamics of gas and solids in a non-magnetized thin protoplanetary disk with the Pencil Code. We use multiple particle species of radius 1, 10, 30, and 100 cm, solving for the particles' gravitational interaction by a particle-mesh method. The dead zone is modeled as a region of low viscosity. Adiabatic and locally isothermal equations of state are used. We find that the Rossby wave instability is triggered under a variety of conditions, thus making vortex formation a robust process. Inside the vortices, fast accumulation of solids occurs and the particles collapse into objects of planetary mass in timescales as short as five orbits. Because the drag force is size-dependent, aerodynamical sorting ensues within the vortical motion, and the first bound structures formed are composed primarily of similarly-sized particles. In addition to erosion due to ram pressure, we identify gas tides from the massive vortices as a disrupting agent of formed protoplanetary embryos. We also estimate the collisional velocity history of the particles that compose the most massive embryo by the end of the simulation, finding that the vast majority of them never experienced a collision with another particle at speeds faster than 1 m/s.

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