Angular momentum evolution in dark-matter haloes

Angular momentum evolution in dark-matter haloes
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暗物质晕中的角动量演化

DOI：
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发表时间：
2010
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通讯作者：
U. Washington
U. Washington
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文献类型：
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作者：
L. Book;A. Brooks;A. Peter;A. Benson;Fabio Governato California Institute of Technology;A. Department;U. Washington

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我们已经分析了高分辨率的N体模拟暗物质（DM）晕，特别侧重于角动量的演变。我们发现，不仅单个粒子的角动量不守恒，而且径向壳层的角动量也会随着宇宙年龄的变化而变化。我们发现，从外部结构的扭矩是最有可能的原因，这种分布的转变。由于绝热收缩模型 该模型常用于模拟星系演化对晕中DM密度分布的影响 假设角动量守恒，这种变化意味着有一个基本的限制，在模拟DM晕星系的增长的反应的绝热收缩模型的可能精度。
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.