Testing the Jeans, Toomre and Bonnor-Ebert concepts for planetesimal formation: 3D streaming instability simulations of diffusion regulated formation of planetesimals

Abstract

We perform streaming instability simulations at Hill density and beyond, to demonstrate that Planetesimal formation is not completed when pebble accumulations exceed the local Hill density. We find that Hill density is not a sufficient criterion for further gravitational collapse of a pebble cloud into a planetesimal, but that additionally the accumulated mass has to be large enough to overcome turbulent diffusion. A Toomre analysis of the system indicates that linear self-gravity modes play no role on the scale of our numerical simulation. We nevertheless find that self-gravity, by vertically contracting the pebble layer, increases the strength of turbulence, which is either an indication of Kelvin Helmholtz Instability or a boost of the streaming-instability. We furthermore determine the Bonnor-Ebert central density to which a pebble cloud of given mass has to be compressed before it would be able to continue contraction against internal diffusion. As the equivalent "solid body" size of the pebble cloud scales with the central density to the power of -1/6, it is much easier to have a pebble cloud of 100 km equivalent size to collapse than one of 10 km for the same level of turbulent diffusion. This can explain the lack of small bodies in the solar system and predicts to have small objects formed by gravitational collapse at large pebble to gas ratios, in the outskirts of the solar nebula and at late times of generally reduced gas mass.

28 pages, 7 figures, ApJ in press (updated citation list and minus some typos)

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• Turbulent Dust-trapping Rings as Efficient Sites for Planetesimal Formation
• Constraints on planetesimal accretion inferred from particle-size distribution in CO chondrites
• Implications of Jupiter Inward Gas-Driven Migration for the Inner Solar System
• Implications for the collisional strength of Jupiter Trojans from the Eurybates family
• On the non-axisymmetric fragmentation of rings generated by the Secular Gravitational Instability
• Three-Dimensional Dust Stirring by a Giant Planet Embedded in a Protoplanetary Disk
• Filling in the Gaps: Can Gravitationally Unstable Discs Form the Seeds of Gas Giant Planets?
• On the evolution of pebble-accreting planets in evolving protoplanetary discs
• Collisional heating of icy planetesimals. I. Catastrophic collisions