Metal mixing by buoyant bubbles in galaxy clusters
Metal mixing by buoyant bubbles in galaxy clusters
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DOI：
10.1111/j.1365-2966.2006.11300.x
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发表时间：
2006-11
影响因子：
4.8
通讯作者：
E. Roediger;M. Brueggen;P. Rebusco;H. Boehringer;E. Churazov;International University Bremen;Mpa Garching;M. Garching;Space Research Institute Moscow
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文献类型：
--
作者：
E. Roediger;M. Brueggen;P. Rebusco;H. Boehringer;E. Churazov;International University Bremen;Mpa Garching;M. Garching;Space Research Institute Moscow
利用自适应网格上的一系列三维流体动力学模拟，我们对星系团中气泡运动对金属丰度分布的影响进行了系统的研究。特别是，我们已经研究了依赖于泡沫的大小和位置，泡沫的复发时间，这些泡沫膨胀的方式和潜在的集群配置文件。我们发现，在流体静力学集团模型，所产生的金属分布是非常拉长沿着方向的气泡。如果金属分布是球形的，则需要团簇中的各向异性或环境运动。为了参数化气泡的金属输运，我们计算有效的扩散系数。从我们简单的实验中推断出的扩散系数在半径为10 kpc时的值约为1029 cm 2 s-1。运行模拟英仙座集群产量扩散系数，同意非常好，从观测推断。
Using a series of three-dimensional, hydrodynamic simulations on an adaptive grid, we have performed a systematic study on the effect of bubble-induced motions on metallicity profiles in clusters of galaxies. In particular, we have studied the dependence on the bubble size and position, the recurrence times of the bubbles, the way these bubbles are inflated and the underlying cluster profile. We find that in hydrostatic cluster models, the resulting metal distribution is very elongated along the direction of the bubbles. Anisotropies in the cluster or ambient motions are needed if the metal distribution is to be spherical. In order to parametrize the metal transport by bubbles, we compute effective diffusion coefficients. The diffusion coefficients inferred from our simple experiments lie at values of around ∼10 29 cm 2 s -1 at a radius of 10 kpc. The runs modelled on the Perseus cluster yield diffusion coefficients that agree very well with those inferred from observations.