Formation and Evolution of X-Ray Clusters: A Hydrodynamic Simulation of the Intracluster Medium
Formation and Evolution of X-Ray Clusters: A Hydrodynamic Simulation of the Intracluster Medium
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X 射线团簇的形成和演化：团内介质的流体动力学模拟
DOI：
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发表时间：
1990
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通讯作者：
A. Evrard
中科院分区：
文献类型：
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作者：
A. Evrard
利用数值模拟方法研究了后发座星系团中热团内介质的热力学历史，该方法结合了自洽演化暗物质质量分布中碰撞重子分量的三维流体动力学。该模型演化到低红移的状态，其X射线和光学性质与Coma和A2256惊人地相似。在z = 0处看到的椭圆形X射线等照度线是在z = 0.2处发生的合并事件的残留物;因此，Coma和A2256可能在不久的过去遭受了中度合并事件。该模型还表明，Coma丰富度集群应显示约0.5 mK的Suniaev-Zel'dovich中心递减。参考文献70篇。
The thermodynamic history of the hot intracluster medium in a cluster of Coma richness was examined using a numerical simulation incorporating three-dimensional hydrodynamics of a collisional baryonic component within a self-consistently evolving dark matter mass distribution. The model evolves to states at low redshifts whose X-ray and optical properties are strikingly similar to Coma and A2256. The elliptical X-ray isophotes seen at z = 0 are remnants of a merger event which occurred at z = 0.2; thus, Coma and A2256 probably suffered moderate merger events in the recent past. The model also indicates that clusters of Coma richness should display a Suniaev-Zel'dovich central decrement of about 0.5 mK. 70 refs.