Non-LTE models for He and Sr in kilonova ejecta show that ~1% He or 1-10% Sr can reproduce the 1μm absorption feature in AT2017gfo, implying low-Ye, low-entropy r-process conditions.
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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.
EP93 expansion opacities underestimate emissivity in radiative transfer; a modified bin-averaged method with expansion-adjusted line strength is proposed along with new public tables.
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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Non-LTE Ionization Modeling for Helium and Strontium in Neutron Star Merger Ejecta
Non-LTE models for He and Sr in kilonova ejecta show that ~1% He or 1-10% Sr can reproduce the 1μm absorption feature in AT2017gfo, implying low-Ye, low-entropy r-process conditions.
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Improved lanthanide constraints for the kilonova AT 2017gfo
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.
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On Atomic Line Opacities for Modeling Astrophysical Radiative Transfer
EP93 expansion opacities underestimate emissivity in radiative transfer; a modified bin-averaged method with expansion-adjusted line strength is proposed along with new public tables.
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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.