Magnetic field amplification by cosmic ray-driven turbulence – I. Isotropic CR diffusion
Magnetic field amplification by cosmic ray-driven turbulence – I. Isotropic CR diffusion
复制标题
宇宙射线驱动湍流的磁场放大 – I. 各向同性 CR 扩散
DOI：
10.1093/mnras/stt1566
复制
发表时间：
2013
影响因子：
4.8
通讯作者：
M. Brüggen
中科院分区：
文献类型：
--
作者：
M. Brüggen
我们已经进行了磁流体动力学模拟研究的冲击波的前兆磁场的放大。在超新星遗迹中发生的强烈冲击的前兆中需要强磁场。观测还表明，磁场放大发生在星系团中的弱冲击中，并产生所谓的无线电遗迹。在这里，我们将宇宙射线驱动的湍流对磁场放大的研究扩展到弱激波。放大是由湍流驱动的，湍流是由宇宙射线压力作用于上游流体中的密度不均匀性产生的。从星系团外围的X射线数据推断出的聚集可能提供了一些种子的不均匀性。磁场功率谱和法拉第地图。此外，我们研究如何同步辐射的冲击前兆可以用来验证这种不稳定性的存在和约束必要的等离子体参数。
We have performed magnetohydrodynamical simulations to study the amplification of magnetic fields in the precursors of shock waves. Strong magnetic fields are required in the precursors of the strong shocks that occur in supernova remnants. Observations also suggest that magnetic field amplification takes place in the weak shocks that occur in galaxy clusters and that produce so-called radio relics. Here, we extend the study of magnetic field amplification by cosmic-ray driven turbulence to weak shocks. The amplification is driven by turbulence that is produced by the cosmic-ray pressure acting on the density inhomogeneities in the upstream fluid. The clumping that has been inferred from X-ray data for the outskirts of galaxy clusters could provide some of the seed inhomogeneities. Magnetic field power spectra and Faraday maps are produced. Furthermore, we investigate how the synchrotron emission in the shock precursor can be used to verify the existence of this instability and constrain essential plasma parameters.
DOI：
10.1111/j.1365-2966.2011.19523.x
发表时间：
2011-07
影响因子：
4.8
作者：
A. Bonafede;K. Dolag;F. Stasyszyn;G. Murante;S. Borgani
通讯作者：
A. Bonafede;K. Dolag;F. Stasyszyn;G. Murante;S. Borgani
簇内介质中气体团簇的性质和气体团簇因子
影响因子：
4.8
作者：
Eckert;Simionescu;Brüggen;Ettori
通讯作者：
Ettori