Dark matter halo response to the disk growth

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dc.creatorChoi, Jun-Hwan
dc.creatorLu, Yu
dc.creatorMo, H. J.
dc.creatorWeinberg, Martin D.
dc.date2006-04-27
dc.date2006-10-16
dc.date.accessioned2026-07-07T10:23:03Z
dc.date.available2026-07-07T10:23:03Z
dc.descriptionWe consider the sensitivity of the circular-orbit adiabatic contraction approximation to the baryon condensation rate and the orbital structure of dark matter halos in the $Λ$CDM paradigm. Using one-dimensional hydrodynamic simulations including the dark matter halo mass accretion history and gas cooling, we demonstrate that the adiabatic approximation is approximately valid even though halos and disks may assemble simultaneously. We further demonstrate the validity of the simple approximation for $Λ$CDM halos with isotropic velocity distributions using three-dimensional N-body simulations. This result is easily understood: an isotropic velocity distribution in a cuspy halo requires more circular orbits than radial orbits. Conversely, the approximation is poor in the extreme case of a radial orbit halo. It overestimates the response a core dark matter halo, where radial orbit fraction is larger. Because no astronomically relevant models are dominated by low-angular momentum orbits in the vicinity of the disk and the growth time scale is never shorter than a dynamical time, we conclude that the adiabatic contraction approximation is useful in modeling the response of dark matter halos to the growth of a disk.
dc.description7 pages, 6 figures, accepted for publication in MNRAS
dc.identifierhttps://arxiv.org/abs/astro-ph/0604587
dc.identifierhttp://arxiv.org/abs/astro-ph/0604587
dc.identifierMon.Not.Roy.Astron.Soc.372:1869-1874,2006
dc.identifierdoi:10.1111/j.1365-2966.2006.10990.x
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/175691
dc.subjectAstrophysics
dc.titleDark matter halo response to the disk growth
dc.typetext

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