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THE EFFECT OF GAS COOLING ON THE SHAPES OF DARK MATTER HALOS

机译:气体冷却对暗物质晕圈形状的影响

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We analyze the effect of dissipation on the shapes of dark matter (DM) halos using high-resolution cosmological gasdynamics simulations of clusters and galaxies in the ACDM cosmology. We find that halos formed in simulations with gas cooling are significantly more spherical than corresponding halos formed in adiabatic simulations. Gas cooling results in an average increase of the principle axis ratios of halos by ~0.2-0.4 in the inner regions. The systematic difference decreases slowly with radius but persists almost to the virial radius. We argue that the differences in simulations with and without cooling arise both during periods of quiescent evolution, when gas cools and condenses toward the center, and during major mergers. We perform a series of high-resolution N-body simulations to study the shapes of remnants in major mergers of DM halos and halos with embedded stellar disks. In the DM halo-only mergers, the shape of the remnants depends only on the orbital angular momentum of the encounter and not on the internal structure of the halos. However, significant shape changes in the DM distribution may result if stellar disks are included. In this case the shape of the DM halos is correlated with the morphology of the stellar remnants.
机译:我们使用ACDM宇宙学中的星团和星系的高分辨率宇宙学气体动力学模拟,分析了消散对暗物质(DM)光环形状的影响。我们发现,在气体冷却模拟中形成的光晕比绝热模拟中形成的相应光晕明显更大。气体冷却使内部光晕的主轴比平均增加了〜0.2-0.4。系统差异随半径缓慢减小,但几乎一直保持到病毒半径。我们认为,在有和没有冷却的情况下,模拟的差异都是在静态演化期间,气体向中心冷却和凝结期间以及大型合并期间出现的。我们执行了一系列高分辨率的N体模拟,以研究DM光晕和带有嵌入式星盘的光晕的主要合并中的残留物形状。在仅DM光晕合并中,残余物的形状仅取决于相遇的轨道角动量,而不取决于光晕的内部结构。但是,如果包括星盘,则可能会导致DM分布中形状发生重大变化。在这种情况下,DM光晕的形状与恒星残留物的形态有关。

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