解开晕下自旋之谜
Solving the puzzle of subhalo spins
摘要：
Onions等人在两个高分辨率孤立晕模拟中研究了次晕的自旋参数分布，最近的工作表明，典型的次晕自旋始终低于场晕的自旋分布。为了进一步研究这个难题，我们分析了一个宇宙体积的模拟，具有足够的分辨率来解决一个显着的subhalo人口。我们证实了Onions等人的结果，并表明亚晕的典型自旋随着质量的减小和与主晕中心的接近程度的增加而减小。我们解释这是越来越大的影响，潮汐剥离在删除外层，因此较高的角动量粒子，subhaloes，因为它们在主机潜在的移动。研究这种效应对红移的依赖性，我们发现典型的次晕自旋随红移的减小而减小。这表明在潮汐剥离情景中预期的时间演变。
英文摘要：
Investigating the spin parameter distribution of subhaloes in two high resolution isolated halo simulations, re- cent work by Onions et al. suggested that typical subhalo spins are consistently lower than the spin distribution found for field haloes. To further examine this puzzle, we have analyzed simulations of a cosmological volume with sufficient resolution to resolve a significant subhalo population. We confirm the result of Onions et al. and show that the typical spin of a subhalo decreases with decreasing mass and increasing proximity to the host halo center. We interpret this as the growing influence of tidal stripping in removing the outer layers, and hence the higher angular momentum particles, of the subhaloes as they move within the host potential. Investigating the redshift dependence of this effect, we find that the typical subhalo spin is smaller with decreasing redshift. This indicates a temporal evolution as expected in the tidal stripping scenario.
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