2003/10/01 by Torsten Ensslin, T. A. Enßlin, C. Vogt +5
Physics and Astronomy · #Astrophysics (astro-ph) #Astrophysics and Cosmic Phenomena #Astrophysics and Star Formation Studies #FOS: Physical sciences #Solar and Space Plasma Dynamics #astro-ph
paper · pdf · doi:10.48550/arxiv.astro-ph/0310028
Oral presentation for ``The Riddle of Cooling Flows in Galaxies and Clusters of Galaxies'' held at Charlottesville, VA USA May 31 - June 4 2003. Proceedings at http://www.astro.virginia.edu/coolflow/, eds T. H. Reiprich, J. C. Kempner and N. Soker. 7 pages, 11 figures
arxiv created 2003/10/01 · openalex publication_date 2003/10/01 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
Cooling flows are regions where the importance of non-thermal intra-cluster medium components such as magnetic fields and cosmic rays may be strongest within a galaxy cluster. They are also regions where such components are best detectable due to the high gas density which influences Faraday rotation measurements of magnetic fields and secondary particle production in hadronic interactions of cosmic ray nuclei with the ambient thermal gas. New estimates of magnetic fields in cooling flow and non-cooling flow clusters are presented, which are based on a newly developed Fourier analysis of extended Faraday rotation maps. We further present new constraints on the cluster cosmic ray proton population using radio and gamma-ray observations measurements of cluster cooling flows, which are especially suited for this purpose due to their high gas and magnetic energy densities. We argue that radio synchrotron emission of cosmic ray electrons generated hadronically by cosmic ray protons is a very plausible explanation for the radio mini-halos observed in some cooling flows.