{"paper":{"title":"Global simulations of strongly magnetized remnant massive neutron stars formed in binary neutron star mergers","license":"http://arxiv.org/licenses/nonexclusive-distrib/1.0/","headline":"","cross_cats":["astro-ph.CO","astro-ph.SR","gr-qc"],"primary_cat":"astro-ph.HE","authors_text":"Kenta Kiuchi, Koutarou Kyutoku, Masaru Shibata, Yuichiro Sekiguchi","submitted_at":"2017-10-03T18:00:05Z","abstract_excerpt":"We perform a general-relativistic magnetohydrodynamics simulation for $\\approx 30$ ms after merger of a binary neutron star to a remnant massive neutron star (RMNS) with a high spatial resolution of the finest grid resolution $12.5$ m. First, we estimate that the Kelvin-Helmholtz instability at merger could amplify the magnetic-field energy up to $\\sim 1\\%$ of the thermal energy. Second, we find that the magnetorotational instability in the RMNS envelope and torus with $\\rho < 10^{13}~{\\rm g~cm^{-3}}$ sustains magneto-turbulent state and the effective viscous parameter in these regions is like"},"claims":{"count":0,"items":[],"snapshot_sha256":"258153158e38e3291e3d48162225fcdb2d5a3ed65a07baac614ab91432fd4f57"},"source":{"id":"1710.01311","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"}