High-resolution simulations of planetesimal formation in turbulent protoplanetary discs
(2011) In Astronomy & Astrophysics 529.- Abstract
- We present high-resolution computer simulations of dust dynamics and planetesimal formation in turbulence generated by the magnetorotational instability. We show that the turbulent viscosity associated with magnetorotational turbulence in a non-stratified shearing box increases when going from 256(3) to 512(3) grid points in the presence of a weak imposed magnetic field, yielding a turbulent viscosity of alpha approximate to 0.003 at high resolution. Particles representing approximately meter-sized boulders concentrate in large-scale high-pressure regions in the simulation box. The appearance of zonal flows and particle concentration in pressure bumps is relatively similar at moderate (256(3)) and high (512(3)) resolution. In the... (More)
- We present high-resolution computer simulations of dust dynamics and planetesimal formation in turbulence generated by the magnetorotational instability. We show that the turbulent viscosity associated with magnetorotational turbulence in a non-stratified shearing box increases when going from 256(3) to 512(3) grid points in the presence of a weak imposed magnetic field, yielding a turbulent viscosity of alpha approximate to 0.003 at high resolution. Particles representing approximately meter-sized boulders concentrate in large-scale high-pressure regions in the simulation box. The appearance of zonal flows and particle concentration in pressure bumps is relatively similar at moderate (256(3)) and high (512(3)) resolution. In the moderate-resolution simulation we activate particle self-gravity at a time when there is little particle concentration, in contrast with previous simulations where particle self-gravity was activated during a concentration event. We observe that bound clumps form over the next ten orbits, with initial birth masses of a few times the dwarf planet Ceres. At high resolution we activate self-gravity during a particle concentration event, leading to a burst of planetesimal formation, with clump masses ranging from a significant fraction of to several times the mass of Ceres. We present a new domain decomposition algorithm for particle-mesh schemes. Particles are spread evenly among the processors and the local gas velocity field and assigned drag forces are exchanged between a domain-decomposed mesh and discrete blocks of particles. We obtain good load balancing on up to 4096 cores even in simulations where particles sediment to the mid-plane and concentrate in pressure bumps. (Less)
Please use this url to cite or link to this publication:
https://lup.lub.lu.se/record/1966026
- author
- Johansen, Anders LU ; Klahr, H. and Henning, Th.
- organization
- publishing date
- 2011
- type
- Contribution to journal
- publication status
- published
- subject
- keywords
- (MHD), magnetohydrodynamics, accretion disks, accretion, methods: numerical, planets and satellites: formation, planetary systems, turbulence
- in
- Astronomy & Astrophysics
- volume
- 529
- publisher
- EDP Sciences
- external identifiers
-
- wos:000289557200070
- scopus:79953299905
- ISSN
- 0004-6361
- DOI
- 10.1051/0004-6361/201015979
- language
- English
- LU publication?
- yes
- id
- 152069d4-9cc6-460d-b912-8fb685ae3dcf (old id 1966026)
- date added to LUP
- 2016-04-01 13:21:04
- date last changed
- 2022-12-11 17:38:45
@article{152069d4-9cc6-460d-b912-8fb685ae3dcf,
abstract = {{We present high-resolution computer simulations of dust dynamics and planetesimal formation in turbulence generated by the magnetorotational instability. We show that the turbulent viscosity associated with magnetorotational turbulence in a non-stratified shearing box increases when going from 256(3) to 512(3) grid points in the presence of a weak imposed magnetic field, yielding a turbulent viscosity of alpha approximate to 0.003 at high resolution. Particles representing approximately meter-sized boulders concentrate in large-scale high-pressure regions in the simulation box. The appearance of zonal flows and particle concentration in pressure bumps is relatively similar at moderate (256(3)) and high (512(3)) resolution. In the moderate-resolution simulation we activate particle self-gravity at a time when there is little particle concentration, in contrast with previous simulations where particle self-gravity was activated during a concentration event. We observe that bound clumps form over the next ten orbits, with initial birth masses of a few times the dwarf planet Ceres. At high resolution we activate self-gravity during a particle concentration event, leading to a burst of planetesimal formation, with clump masses ranging from a significant fraction of to several times the mass of Ceres. We present a new domain decomposition algorithm for particle-mesh schemes. Particles are spread evenly among the processors and the local gas velocity field and assigned drag forces are exchanged between a domain-decomposed mesh and discrete blocks of particles. We obtain good load balancing on up to 4096 cores even in simulations where particles sediment to the mid-plane and concentrate in pressure bumps.}},
author = {{Johansen, Anders and Klahr, H. and Henning, Th.}},
issn = {{0004-6361}},
keywords = {{(MHD); magnetohydrodynamics; accretion disks; accretion; methods: numerical; planets and satellites: formation; planetary systems; turbulence}},
language = {{eng}},
publisher = {{EDP Sciences}},
series = {{Astronomy & Astrophysics}},
title = {{High-resolution simulations of planetesimal formation in turbulent protoplanetary discs}},
url = {{http://dx.doi.org/10.1051/0004-6361/201015979}},
doi = {{10.1051/0004-6361/201015979}},
volume = {{529}},
year = {{2011}},
}