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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5 Pith papers cite this work. Polarity classification is still indexing.
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UNVERDICTED 5representative citing papers
Observational analysis of EMP stars including a new r-process enhanced star G256353 whose heavy-element pattern matches scaled solar and neutron-star-merger predictions, supporting r-process universality.
Lower BNS merger rates from GWTC-4 data produce tensions of factors 3.6-18 with SGRB rates, 0.9-4.1 with r-process rates, and 2.3-5.1 with Galactic DNS rates.
New abundance measurements confirm two stars as r-II and one as borderline r-I, with r-process material older than 10 Gyr and possible links to the Thamnos structure.
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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The \emph{R}-process Alliance: A Bright, Strongly \emph{R}-process-enhanced Extremely Metal-poor Star Observed with GHOST
Observational analysis of EMP stars including a new r-process enhanced star G256353 whose heavy-element pattern matches scaled solar and neutron-star-merger predictions, supporting r-process universality.
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Implications of low neutron star merger rates for gamma-ray bursts, r-process production and Galactic double neutron stars
Lower BNS merger rates from GWTC-4 data produce tensions of factors 3.6-18 with SGRB rates, 0.9-4.1 with r-process rates, and 2.3-5.1 with Galactic DNS rates.
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The $R$-Process Alliance: The $R$-Process Enhancement of Stars from Chemodynamically Tagged Groups in the Milky Way Halo
New abundance measurements confirm two stars as r-II and one as borderline r-I, with r-process material older than 10 Gyr and possible links to the Thamnos structure.
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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.