EDP Sciences
Free access
Volume 417, Number 1, April I 2004
Page(s) 361 - 374
Section Planets and planetary systems
DOI http://dx.doi.org/10.1051/0004-6361:20034417

A&A 417, 361-374 (2004)
DOI: 10.1051/0004-6361:20034417

Simulations of dust-trapping vortices in protoplanetary discs

A. Johansen1, 2, A. C. Andersen1 and A. Brandenburg1

1  NORDITA, Blegdamsvej 17, 2100 Copenhagen, Denmark
    e-mail: [anja; brandenb]@nordita.dk
2  Astronomical Obs., NBIfAFG, Copenhagen University, Juliane Maries Vej 30, 2100 Copenhagen, Denmark

(Received 30 September 2003 / Accepted 18 December 2003 )

Local three-dimensional shearing box simulations of the compressible coupled dust-gas equations are used in the fluid approximation to study the evolution of different initial vortex configurations in a protoplanetary disc and their dust-trapping capabilities. The initial conditions for the gas are derived from an analytic solution to the compressible Euler equation and the continuity equation. The solution is valid if there is a vacuum outside the vortex. In the simulations the vortex is either embedded in a hot corona, or it is extended in a cylindrical fashion in the vertical direction. Both configurations are found to survive for at least one orbit and lead to accumulation of dust inside the vortex. This confirms earlier findings that dust accumulates in anticyclonic vortices, indicating that this is a viable mechanism for planetesimal formation.

Key words: solar system: formation -- accretion, accretion discs -- hydrodynamics -- instabilities -- methods: numerical -- turbulence

Offprint request: A. Johansen, ajohan@astro.ku.dk

© ESO 2004

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