2008/02/29 by Y. Dubois, Yohan Dubois, Romain Teyssier +1 · 7 citations
Physics and Astronomy · #Astrophysics #Astrophysics and Star Formation Studies #Computational physics #Cooling flow #Galaxies: Formation, Evolution, Phenomena #Galaxy #Galaxy cluster #Magnetic field #Magnetohydrodynamics #Physics #Radiative cooling #Solar and Space Plasma Dynamics #astro-ph
paper · pdf · doi:10.1051/0004-6361:200809513
4 pages, 6 figures, to be published in A&A, correction in one reference
openalex publication_date 2008/03/19 · arxiv created 2008/03/31 · arxiv updated 2009/12/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Context. Various observations of magnetic fields in the intra-cluster medium (ICM), most of the time restricted to cluster cores, point towards a field strength of a few (synchrotron radiation from radio relics and radio halos, inverse Compton radiation in X-rays and Faraday rotation measure of polarised background sources). Both the origin and the spatial structure of galaxy cluster magnetic fields are still under debate. In particular, the radial profile of the magnetic field, from the core of clusters to their outskirts, is important for cosmic ray propagation within the cosmic web.