The shape of dark matter haloes in the Aquarius simulations: Evolution and memory
We use the high resolution cosmological N-body simulations from the Aquarius project to investigate in detail the mechanisms that determine the shape of Milky Way-type dark matter haloes. We find that, when measured at the instantaneous virial radius, the shape of individual haloes changes with time...
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2012-02-01
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Series: | EPJ Web of Conferences |
Online Access: | http://dx.doi.org/10.1051/epjconf/20121901009 |
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doaj-037fd3106f9245efb4135f0d621c76bd2021-08-02T18:20:15ZengEDP SciencesEPJ Web of Conferences2100-014X2012-02-01190100910.1051/epjconf/20121901009The shape of dark matter haloes in the Aquarius simulations: Evolution and memorySales L.V.Helmi A.Vera-Ciro C.A.We use the high resolution cosmological N-body simulations from the Aquarius project to investigate in detail the mechanisms that determine the shape of Milky Way-type dark matter haloes. We find that, when measured at the instantaneous virial radius, the shape of individual haloes changes with time, evolving from a typically prolate configuration at early stages to a more triaxial/oblate geometry at the present day. This evolution in halo shape correlates well with the distribution of the infalling material: prolate configurations arise when haloes are fed through narrow filaments, which characterizes the early epochs of halo assembly, whereas triaxial/oblate configurations result as the accretion turns more isotropic at later times. Interestingly, at redshift z = 0, clear imprints of the past history of each halo are recorded in their shapes at different radii, which also exhibit a variation from prolate in the inner regions to triaxial/oblate in the outskirts. Provided that the Aquarius haloes are fair representatives of Milky Way-like 1012M☉ objects, we conclude that the shape of such dark matter haloes is a complex, time-dependent property, with each radial shell retaining memory of the conditions at the time of collapse. http://dx.doi.org/10.1051/epjconf/20121901009 |
collection |
DOAJ |
language |
English |
format |
Article |
sources |
DOAJ |
author |
Sales L.V. Helmi A. Vera-Ciro C.A. |
spellingShingle |
Sales L.V. Helmi A. Vera-Ciro C.A. The shape of dark matter haloes in the Aquarius simulations: Evolution and memory EPJ Web of Conferences |
author_facet |
Sales L.V. Helmi A. Vera-Ciro C.A. |
author_sort |
Sales L.V. |
title |
The shape of dark matter haloes in the Aquarius simulations: Evolution and memory |
title_short |
The shape of dark matter haloes in the Aquarius simulations: Evolution and memory |
title_full |
The shape of dark matter haloes in the Aquarius simulations: Evolution and memory |
title_fullStr |
The shape of dark matter haloes in the Aquarius simulations: Evolution and memory |
title_full_unstemmed |
The shape of dark matter haloes in the Aquarius simulations: Evolution and memory |
title_sort |
shape of dark matter haloes in the aquarius simulations: evolution and memory |
publisher |
EDP Sciences |
series |
EPJ Web of Conferences |
issn |
2100-014X |
publishDate |
2012-02-01 |
description |
We use the high resolution cosmological N-body simulations from the Aquarius project to investigate in detail the mechanisms that determine the shape of Milky Way-type dark matter haloes. We find that, when measured at the instantaneous virial radius, the shape of individual haloes changes with time, evolving from a typically prolate configuration at early stages to a more triaxial/oblate geometry at the present day. This evolution in halo shape correlates well with the distribution of the infalling material: prolate configurations arise when haloes are fed through narrow filaments, which characterizes the early epochs of halo assembly, whereas triaxial/oblate configurations result as the accretion turns more isotropic at later times. Interestingly, at redshift z = 0, clear imprints of the past history of each halo are recorded in their shapes at different radii, which also exhibit a variation from prolate in the inner regions to triaxial/oblate in the outskirts. Provided that the Aquarius haloes are fair representatives of Milky Way-like 1012M☉ objects, we conclude that the shape of such dark matter haloes is a complex, time-dependent property, with each radial shell retaining memory of the conditions at the time of collapse. |
url |
http://dx.doi.org/10.1051/epjconf/20121901009 |
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