Angular momentum evolution in dark-matter haloes

被引：7

作者：

Book, Laura G. ^{[1
]}

Brooks, Alyson ^{[1
]}

Peter, Annika H. G. ^{[1
]}

Benson, Andrew J. ^{[1
]}

Governato, Fabio ^{[2
]}

机构：

[1] CALTECH, Pasadena, CA 91125 USA

[2] Univ Washington, Dept Astron, Seattle, WA 98195 USA

来源：

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY | 2011年 / 411卷 / 03期

关键词：

galaxies: haloes; galaxies: kinematics and dynamics; HIERARCHICAL GALAXY FORMATION; UNIVERSAL DENSITY PROFILE; ACTIVE GALACTIC NUCLEI; COSMOLOGICAL SIMULATIONS; ADIABATIC CONTRACTION; DWARF GALAXIES; DISK GALAXIES; MERGER TREES; BLACK-HOLES; MASS MODELS;

D O I：

10.1111/j.1365-2966.2010.17824.x

中图分类号：

P1 [天文学];

学科分类号：

0704 ;

摘要：

We have analysed high-resolution N-body simulations of dark-matter (DM) haloes, focusing specifically on the evolution of angular momentum. We find that not only is individual particle angular momentum not conserved, but the angular momentum of radial shells also varies over the age of the Universe by up to factors of a few. We find that torques from external structure are the most likely cause for this distribution shift. Since the model of adiabatic contraction that is often applied to model the effects of galaxy evolution on the DM density profile in a halo assumes angular momentum conservation, this variation implies that there is a fundamental limit on the possible accuracy of the adiabatic contraction model in modelling the response of DM haloes to the growth of galaxies.

引用

页码：1963 / 1976

页数：14

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