{"paper":{"title":"The Efficiency of Magnetic Field Amplification at Shocks by Turbulence","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO"],"primary_cat":"astro-ph.HE","authors_text":"Mateusz Ruszkowski, Maxim Markevitch, S. Peng Oh, Suoqing Ji","submitted_at":"2016-03-28T20:00:00Z","abstract_excerpt":"Turbulent dynamo field amplification has often been invoked to explain the strong field strengths in thin rims in supernova shocks ($\\sim 100 \\, \\mu$G) and in radio relics in galaxy clusters ($\\sim \\mu$G). We present high resolution MHD simulations of the interaction between pre-shock turbulence, clumping and shocks, to quantify the conditions under which turbulent dynamo amplification can be significant. We demonstrate numerically converged field amplification which scales with Alfv\\'en Mach number, $B/B_0 \\propto {\\mathcal M}_{\\rm A}$, up to ${\\mathcal M}_{\\rm A} \\sim 150$. This implies that"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1603.08518","kind":"arxiv","version":2},"verdict":{"id":null,"model_set":{},"created_at":null,"strongest_claim":"","one_line_summary":"","pipeline_version":null,"weakest_assumption":"","pith_extraction_headline":""},"references":{"count":0,"sample":[],"resolved_work":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57","internal_anchors":0},"formal_canon":{"evidence_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"author_claims":{"count":0,"strong_count":0,"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"builder_version":"pith-number-builder-2026-05-17-v1"}