Oral Presentation

Turbulence and Magnetic fields in Galaxy Clusters: a Simulation Study

Author(s): Soonyoung Roh (UNIST) and Dongsu Ryu (UNIST)

Presenter: Soonyoung Roh (UNIST)

Magnetic fields in clusters of galaxies play a critical role in shaping up the intracluster medium. The existence of magnetic fields in clusters is demonstrated by the rotation measure of polarized radio galaxies and the synchrotron emission of cluster-wide diffuse sources (radio halos and relics). In some relics, the magnetic fields are believed to have a few μG strength and a Mpc scale. The observed magnetic fields are conjectured to be produced by the process of small-scale turbulence dynamo. Yet, the dynamo in clusters is not well understood. To investigate the dynamo, we simulate the development of turbulence and the follow-up amplification of magnetic fields in clusters using a newly developed three-dimensional magnetohydrodynamical code. Turbulence is induced in highly stratified backgrounds expected in clusters, and driven sporadically mimicking major mergers. We here present preliminary results, aiming to answer whether the turbulence dynamo scenario can explain observed magnetic fields in clusters of galaxies.