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Modelling ripples in Orion with coupled dust dynamics and radiative transfer

T Hendrix, R Keppens and Peter Camps UGent (2015) ASTRONOMY & ASTROPHYSICS. 575.
abstract
Aims. In light of the recent detection of direct evidence for the formation of Kelvin-Helmholtz instabilities in the Orion nebula, we expand upon previous modelling efforts by numerically simulating the shear-flow driven gas and dust dynamics in locations where the HII region and the molecular cloud interact. We aim to directly confront the simulation results with the infrared observations. Methods. To numerically model the onset and full nonlinear development of the Kelvin-Helmholtz instability we take the setup proposed to interpret the observations, and adjust it to a full 3D hydrodynamical simulation that includes the dynamics of gas as well as dust. A dust grain distribution with sizes between 5-250 nm is used, exploiting the gas + dust module of the MPI-AMRVAC code, in which the dust species are represented by several pressureless dust fluids. The evolution of the model is followed well into the nonlinear phase. The output of these simulations is then used as input for the SKIRT dust radiative transfer code to obtain infrared images at several stages of the evolution, which can be compared to the observations. Results. We confirm that a 3D Kelvin-Helmholtz instability is able to develop in the proposed setup, and that the formation of the instability is not inhibited by the addition of dust. Kelvin-Helmholtz billows form at the end of the linear phase, and synthetic observations of the billows show striking similarities to the infrared observations. It is pointed out that the high density dust regions preferentially collect on the flanks of the billows. To get agreement with the observed Kelvin-Helmholtz ripples, the assumed geometry between the background radiation, the billows and the observer is seen to be of critical importance.
Please use this url to cite or link to this publication:
author
organization
year
type
journalArticle (original)
publication status
published
subject
keyword
radiative transfer, hydrodynamics, ISM: kinematics and dynamics, ISM: structure, KELVIN-HELMHOLTZ INSTABILITY, MOLECULAR CLOUD, MAGNETIC-FIELD, WIND, TURBULENCE, SOLAR, PARAMETERS, EVOLUTION, GRAINS, SKIRT, extinction, ISM: clouds, dust
journal title
ASTRONOMY & ASTROPHYSICS
Astron. Astrophys.
volume
575
article number
A110
pages
7 pages
Web of Science type
Article
Web of Science id
000360710400011
JCR category
ASTRONOMY & ASTROPHYSICS
JCR impact factor
5.185 (2015)
JCR rank
12/61 (2015)
JCR quartile
1 (2015)
ISSN
1432-0746
DOI
10.1051/0004-6361/201425498
language
English
UGent publication?
yes
classification
A1
copyright statement
I have transferred the copyright for this publication to the publisher
id
7060014
handle
http://hdl.handle.net/1854/LU-7060014
date created
2016-01-28 11:21:43
date last changed
2017-03-01 10:11:31
@article{7060014,
  abstract     = {Aims. In light of the recent detection of direct evidence for the formation of Kelvin-Helmholtz instabilities in the Orion nebula, we expand upon previous modelling efforts by numerically simulating the shear-flow driven gas and dust dynamics in locations where the HII region and the molecular cloud interact. We aim to directly confront the simulation results with the infrared observations. 
Methods. To numerically model the onset and full nonlinear development of the Kelvin-Helmholtz instability we take the setup proposed to interpret the observations, and adjust it to a full 3D hydrodynamical simulation that includes the dynamics of gas as well as dust. A dust grain distribution with sizes between 5-250 nm is used, exploiting the gas + dust module of the MPI-AMRVAC code, in which the dust species are represented by several pressureless dust fluids. The evolution of the model is followed well into the nonlinear phase. The output of these simulations is then used as input for the SKIRT dust radiative transfer code to obtain infrared images at several stages of the evolution, which can be compared to the observations. 
Results. We confirm that a 3D Kelvin-Helmholtz instability is able to develop in the proposed setup, and that the formation of the instability is not inhibited by the addition of dust. Kelvin-Helmholtz billows form at the end of the linear phase, and synthetic observations of the billows show striking similarities to the infrared observations. It is pointed out that the high density dust regions preferentially collect on the flanks of the billows. To get agreement with the observed Kelvin-Helmholtz ripples, the assumed geometry between the background radiation, the billows and the observer is seen to be of critical importance.},
  articleno    = {A110},
  author       = {Hendrix, T and Keppens, R and Camps, Peter},
  issn         = {1432-0746},
  journal      = {ASTRONOMY \& ASTROPHYSICS},
  keyword      = {radiative transfer,hydrodynamics,ISM: kinematics and dynamics,ISM: structure,KELVIN-HELMHOLTZ INSTABILITY,MOLECULAR CLOUD,MAGNETIC-FIELD,WIND,TURBULENCE,SOLAR,PARAMETERS,EVOLUTION,GRAINS,SKIRT,extinction,ISM: clouds,dust},
  language     = {eng},
  pages        = {7},
  title        = {Modelling ripples in Orion with coupled dust dynamics and radiative transfer},
  url          = {http://dx.doi.org/10.1051/0004-6361/201425498},
  volume       = {575},
  year         = {2015},
}

Chicago
Hendrix, T, R Keppens, and Peter Camps. 2015. “Modelling Ripples in Orion with Coupled Dust Dynamics and Radiative Transfer.” Astronomy & Astrophysics 575.
APA
Hendrix, T, Keppens, R., & Camps, P. (2015). Modelling ripples in Orion with coupled dust dynamics and radiative transfer. ASTRONOMY & ASTROPHYSICS, 575.
Vancouver
1.
Hendrix T, Keppens R, Camps P. Modelling ripples in Orion with coupled dust dynamics and radiative transfer. ASTRONOMY & ASTROPHYSICS. 2015;575.
MLA
Hendrix, T, R Keppens, and Peter Camps. “Modelling Ripples in Orion with Coupled Dust Dynamics and Radiative Transfer.” ASTRONOMY & ASTROPHYSICS 575 (2015): n. pag. Print.