The temperature-mass relation in magnetized galaxy clusters
The temperature-mass relation in magnetized galaxy clusters
复制标题
磁化星系团中的温度-质量关系
DOI：
10.1051/0004-6361:20010094
复制
发表时间：
2001
影响因子：
6.5
通讯作者：
M. Bartelmann
中科院分区：
文献类型：
--
作者：
K. Dolag;A. Evrard;M. Bartelmann
我们使用宇宙学、磁流体力学对星系团的模拟来量化磁场在这些星系团中的动力学重要性。选择了高红移时初始磁场强度的设置，以便在模拟中很好地重现在低红移星团中观测到的法拉第旋转测量结果。在低密度、空间平坦的CDM宇宙学模型的框架下，计算了一组星系团的星系团内气体温度、热压和磁压的径向无因子数。我们发现，在初始磁场强度的实际范围内，星系团内气体的温度变化不到5%。
We use cosmological, magneto-hydrodynamic simulations of galaxy clusters to quantify the dynamical importance of magnetic elds in these clusters. The set-up of initial magnetic eld strengths at high redshifts is chosen such that observed Faraday-rotation measurements in low-redshift clusters are well reproduced in the simulations. We compute the radial proles of the intracluster gas temperature and of the thermal and magnetic pressure in a set of clusters simulated in the framework of an Einstein-de Sitter and a low-density, spatially-flat CDM cosmological model. We nd that, for a realistic range of initial magnetic eld strengths, the temperature of the intracluster gas changes by less than5%