Halo expansion in cosmological hydro simulations: toward a baryonic solution of the cusp/core problem in massive spirals

Show simple item record

dc.creator Gibson, Brad K.
dc.creator Maccio, A. V.
dc.creator Stinson, G.
dc.creator Brook, C. B.
dc.creator Wadsley, J.
dc.creator Couchman, H. M. P.
dc.creator Shen, S.
dc.creator Quinn, T.
dc.date.accessioned 2015-04-08T12:51:39Z
dc.date.available 2015-04-08T12:51:39Z
dc.date.issued 2012-01-01
dc.identifier.issn 2041-8205
dc.identifier.uri http://library2.smu.ca/xmlui/handle/01/26029
dc.description Publisher's version/PDF en_CA
dc.description.abstract A clear prediction of the cold dark matter (CDM) model is the existence of cuspy dark matter halo density profiles on all mass scales. This is not in agreement with the observed rotation curves of spiral galaxies, challenging on small scales the otherwise successful CDM paradigm. In this work we employ high-resolution cosmological hydrodynamical simulations to study the effects of dissipative processes on the inner distribution of dark matter in Milky Way like objects (M [almost equal to] 10[superscript 12] M[circled dot]). Our simulations include supernova feedback, and the effects of the radiation pressure of massive stars before they explode as supernovae. The increased stellar feedback results in the expansion of the dark matter halo instead of contraction with respect to N-body simulations. Baryons are able to erase the dark matter cuspy distribution, creating a flat, cored, dark matter density profile in the central several kiloparsecs of a massive Milky-Way-like halo. The profile is well fit by a Burkert profile, with fitting parameters consistent with the observations. In addition, we obtain flat rotation curves as well as extended, exponential stellar disk profiles. While the stellar disk we obtain is still partially too thick to resemble the Milky Way thin disk, this pilot study shows that there is enough energy available in the baryonic component to alter the dark matter distribution even in massive disk galaxies, providing a possible solution to the long-standing problem of cusps versus cores. en_CA
dc.language.iso en en_CA
dc.publisher American Astronomical Society en_CA
dc.publisher IOP Publishing
dc.relation.uri http://dx.doi.org/10.1088/2041-8205/744/1/L9
dc.rights Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
dc.subject.lcsh Cosmology -- Mathematical models
dc.subject.lcsh Galaxies -- Formation
dc.subject.lcsh Hydrodynamics
dc.title Halo expansion in cosmological hydro simulations: toward a baryonic solution of the cusp/core problem in massive spirals en_CA
dc.type Text en_CA
dcterms.bibliographicCitation Astrophysical Journal Letters 744(1), L9. (2012) en_CA


Files in this item


 

Copyright statement:

 
Article is made available in accordance with the publisher’s policy and is subject to copyright law. Please refer to the publisher’s site. Any re-use of this article is to be in accordance with the publisher’s copyright policy. This posting is in no way granting any permission for re-use to the reader/user.
 
Published Version: http://dx.doi.org/10.1088/2041-8205/744/1/L9
 
 

This item appears in the following Collection(s)

Show simple item record