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 × 10−1 M ⊙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.
Magnetized Outflows from Short-lived Neutron Star Merger Remnants Can Produce a Blue Kilonova / Curtis, Sanjana; Bosch, Pablo; Mösta, Philipp; Radice, David; Bernuzzi, Sebastiano; Perego, Albino; Haas, Roland; Schnetter, Erik. - In: THE ASTROPHYSICAL JOURNAL LETTERS. - ISSN 2041-8205. - 961:1(2024). [10.3847/2041-8213/ad0fe1]
Magnetized Outflows from Short-lived Neutron Star Merger Remnants Can Produce a Blue Kilonova
Bernuzzi, Sebastiano;Perego, Albino;
2024-01-01
Abstract
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 × 10−1 M ⊙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.File | Dimensione | Formato | |
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