The turbulent pressure support in galaxy clusters revisited

Conduction and Turbulent Mixing in Galaxy Clusters

We discuss hydrostatic models of galaxy clusters in which heat diffusion balances radiative cooling. We consider two different sources of diffusion, thermal conduction and turbulent mixing, parameterized by dimensionless coefficients, f and αmix, respectively. Models with thermal conduction give reasonably good fits to the density and temperature profiles of several cooling flow clusters, but s...

Turbulent Velocity Fields in SPH–simulated Galaxy Clusters: Scaling Laws for the Turbulent Energy

We present a study of the turbulent velocity fields in the Intra Cluster Medium of a sample of 21 galaxy clusters simulated by the SPH–code Gadget2, using a new numerical scheme where the artificial viscosity is suppressed outside shocks. The turbulent motions in the ICM of our simulated clusters are detected with a novel method devised to better disentangle laminar bulk motions from chaotic on...

Ram pressure stripping of disk galaxies in galaxy clusters

While galaxies move through the intracluster medium of their host cluster, they experience a ram pressure which removes at least a significant part of their interstellar medium. This ram pressure stripping appears to be especially important for spiral galaxies: this scenario is a good candidate to explain the differences observed between cluster spirals in the nearby universe and their field co...

Galaxy Clusters

Galaxy Activity in Merging Binary Galaxy Clusters

We present the results of a study of galaxy activity in two merging binary clusters (A168 and A1750) using the Sloan Digital Sky Survey (SDSS) data supplemented with the data in the literature. We have investigated the merger histories of A168 and A1750 by combining the results from a two-body dynamical model and X-ray data. In A168 two subclusters appear to have passed each other and to be com...