Using newly computed dielectronic recombination rates for Se, Rb, Sr, Y, and Zr in kilonova spectral models dramatically changes the predicted ionization, temperature, and line identities at 10 and 25 days after a neutron star merger.
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Nebular spectra of kilonovae with detailed recombination rates -- I. Light r-process composition
Using newly computed dielectronic recombination rates for Se, Rb, Sr, Y, and Zr in kilonova spectral models dramatically changes the predicted ionization, temperature, and line identities at 10 and 25 days after a neutron star merger.