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Planetesimal formation in self-gravitating discs - dust trapping by vortices

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http://arxiv.org/abs/1508.02879
http://adsabs.harvard.edu/abs/2015MNRAS.453.4232G
Original languageEnglish
Pages (from-to)4232-4243
JournalMonthly Notices of the Royal Astronomical Society
Volume453
DOIs
StatePublished - 1 Nov 2015

Abstract

The mechanism through which metre-sized boulders grow to km-sized planetesimals in protoplanetary discs is a subject of active research, since it is critical for planet formation. To avoid spiralling into the protostar due to aerodynamic drag, objects must rapidly grow from cm-sized pebbles, which are tightly coupled to the gas, to large boulders of 1-100 m in diameter. It is already well known that overdensities in the gaseous component of the disc provide potential sites for the collection of solids, and that significant density structures in the gaseous component of the disc (e.g. spiral density waves) can trap solids efficiently enough for the solid component of the disc to undergo further gravitational collapse due to their own self-gravity. In this work, we employ the PENCIL CODE to conduct local shearing sheet simulations of massive self-gravitating protoplanetary discs, to study the effect of anticyclonic transient vortices, or eddies, on the evolution of solids in these discs. We find that these types of structures are extremely efficient at concentrating small and intermediate-sized dust particles with friction times comparable to, or less than, the local orbital period of the disc. This can lead to significant over-densities in the solid component of the disc, with density enhancements comparable to, and even higher, than those within spiral density waves; increasing the rate of gravitational collapse of solids into bound structures.

    Research areas

  • accretion, accretion discs, gravitation, hydrodynamics, instabilities, planets and satellites: formation

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