Simulations of dust-trapping vortices in protoplanetary discs

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Simulations of dust-trapping vortices in protoplanetary discs. / Johansen, A.; Andersen, A. C.; Brandenburg, A.

In: Astronomy and Astrophysics, Vol. 417, No. 1, 01.04.2004, p. 361-374.

Research output: Contribution to journal › Journal article › Research › peer-review

Harvard

Johansen, A, Andersen, AC & Brandenburg, A 2004, 'Simulations of dust-trapping vortices in protoplanetary discs', Astronomy and Astrophysics, vol. 417, no. 1, pp. 361-374. https://doi.org/10.1051/0004-6361:20034417

APA

Johansen, A., Andersen, A. C., & Brandenburg, A. (2004). Simulations of dust-trapping vortices in protoplanetary discs. Astronomy and Astrophysics, 417(1), 361-374. https://doi.org/10.1051/0004-6361:20034417

Vancouver

Johansen A, Andersen AC, Brandenburg A. Simulations of dust-trapping vortices in protoplanetary discs. Astronomy and Astrophysics. 2004 Apr 1;417(1):361-374. https://doi.org/10.1051/0004-6361:20034417

Author

Johansen, A. ; Andersen, A. C. ; Brandenburg, A. / Simulations of dust-trapping vortices in protoplanetary discs. In: Astronomy and Astrophysics. 2004 ; Vol. 417, No. 1. pp. 361-374.

Bibtex

@article{63db0a9191044f92ac7261f5983d5c67,
title = "Simulations of dust-trapping vortices in protoplanetary discs",
abstract = "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.",
keywords = "Accretion, accretion discs, Hydrodynamics, Instabilities, Methods: numerical, Solar system: formation, Turbulence",
author = "A. Johansen and Andersen, {A. C.} and A. Brandenburg",
year = "2004",
month = apr,
day = "1",
doi = "10.1051/0004-6361:20034417",
language = "English",
volume = "417",
pages = "361--374",
journal = "Astronomy & Astrophysics",
issn = "0004-6361",
publisher = "E D P Sciences",
number = "1",

}

RIS

TY - JOUR

T1 - Simulations of dust-trapping vortices in protoplanetary discs

AU - Johansen, A.

AU - Andersen, A. C.

AU - Brandenburg, A.

PY - 2004/4/1

Y1 - 2004/4/1

N2 - 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.

AB - 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.

KW - Accretion, accretion discs

KW - Hydrodynamics

KW - Instabilities

KW - Methods: numerical

KW - Solar system: formation

KW - Turbulence

UR - http://www.scopus.com/inward/record.url?scp=1842582819&partnerID=8YFLogxK

U2 - 10.1051/0004-6361:20034417

DO - 10.1051/0004-6361:20034417

M3 - Journal article

AN - SCOPUS:1842582819

VL - 417

SP - 361

EP - 374

JO - Astronomy & Astrophysics

JF - Astronomy & Astrophysics

SN - 0004-6361

IS - 1

ER -

ID: 232623193