We present a 3D general-relativistic magnetohydrodynamic simulation of a short-lived neutron star remnant formed in the aftermath of a binary neutron star merger. The simulation uses an M1 neutrino transport scheme to track neutrino–matter interactions and is well suited to studying the resulting nucleosynthesis and kilonova emission. A magnetized wind is driven from the remnant and ejects neutron-rich material at a quasi-steady-state rate of 0.8 × 10−1M⊙s−1. We find that the ejecta in our simulations underproduce r-process abundances beyond the second r-process peak. For sufficiently long-lived remnants, these outflows alone can produce blue kilonovae, including the blue kilonova component observed for AT2017gfo.
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Title
Magnetized Outflows from Short-lived Neutron Star Merger Remnants Can Produce a Blue Kilonova
Funding Information
NWO, OCENW.XL21.XL21.038 U.S. Department of Energy, Office of Science, Division of Nuclear Physics, DE-SC0021177 National Science Foundation, PHY-2011725 National Science Foundation, PHY-2020275 National Science Foundation, PHY-2116686 National Science Foundation, AST-2108467 EU Horizon, ERC Consolidator Grant, InspiReM-101043372 Deutsche Forschungsgemeinschaft (DFG), Project MEMI, BE 6301/2-1 Government of Canada, Department of Innovation, Science and Economic Development Province of Ontario, Ministry of Colleges and Universities National Science Foundation, OAC-2004879 National Science Foundation, OAC-2103680 National Science Foundation, OAC-1238993
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