Free neutrons survive r-process freeze-out in fast ejecta of neutron star mergers and their beta-decay heating produces a visible early kilonova precursor for mass fractions above ~0.05.
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More complete lanthanide line data in radiative transfer modeling requires a lanthanide mass fraction of only 2.5e-3 to match the observed spectrum of AT 2017gfo, twenty times below prior claims.
Relativistic MHD simulations of jet-driven shocks in post-merger ejecta show the GW-EM delay depends weakly on viewing angle and opacity, with a choked-jet model best matching GRB 170817A luminosity, delay, and duration.
Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.
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Nuclear Physics of Binary Neutron Star Mergers
Review summarizing the role of dense-matter equation of state, weak interactions, and r-process nucleosynthesis in binary neutron star mergers and their multimessenger observables.