Simulations show double neutron star mergers peak 80-250 million years after star formation across metallicities, with 15% quick mergers and over 20% delayed over a billion years.
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4 Pith papers cite this work. Polarity classification is still indexing.
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2026 4representative citing papers
A one-zone model shows that observed [Y/Eu] and [Sr/Eu] trends require a prompt first-peak channel, delayed BNS mergers dominating Eu, and delayed AGB s-process with t_min > 0.3 Gyr.
Latest GW neutron star merger rates are consistent with short GRBs being produced by BNS mergers if jets are wide or rates low, with NSBH mergers subdominant.
Magnetorotational r-process best explains lighter elements and CEJSN explains the third peak based on scatter and iron correlations in early metal-poor stars.
citing papers explorer
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Double Neutron Star Delay Times Across Cosmic Metallicities: The Role of Helium Star Progenitors
Simulations show double neutron star mergers peak 80-250 million years after star formation across metallicities, with 15% quick mergers and over 20% delayed over a billion years.
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Distinct First-to-Second Peak Yield Ratios and Timescales Reveal a Sub-dominant Prompt Channel
A one-zone model shows that observed [Y/Eu] and [Sr/Eu] trends require a prompt first-peak channel, delayed BNS mergers dominating Eu, and delayed AGB s-process with t_min > 0.3 Gyr.
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Wide Jets or Low Rates: Reconciling Short GRB and Gravitational-Wave Neutron Star Merger Rates
Latest GW neutron star merger rates are consistent with short GRBs being produced by BNS mergers if jets are wide or rates low, with NSBH mergers subdominant.
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The early r-process nucleosynthesis scenarios
Magnetorotational r-process best explains lighter elements and CEJSN explains the third peak based on scatter and iron correlations in early metal-poor stars.