Nebular Spectra of Kilonovae with Detailed Recombination Rates. I. Light <i>r</i>-process Composition

Abstract To investigate spectra of kilonovae in the nonlocal thermal equilibrium phase ( t ≳ 1 week), we perform atomic calculations for dielectronic recombination (DR) rates for the light r -process elements Se ( Z = 34), Rb ( Z = 37), Sr ( Z = 38), Y ( Z = 39), and Zr ( Z = 40) using the HULLAC code. For the different elements, our results for the DR rate coefficients for recombining from the ionization states of II to I, III to II, and IV to III vary between 2 × 10 −12 –5 × 10 −11 cm 3 s −1 , 10 −13 –5 × 10 −11 cm 3 s −1 , and 2 × 10 −15 –10 −11 cm 3 s −1 , respectively, at a temperature of T = 10,000 K. Using this new atomic data (DR), we study the impact on kilonova model spectra at phases of t = 10 days and t = 25 days after the merger using the spectral synthesis code SUMO . Compared to models using the previous treatment of recombination as a constant rate, the new models show significant changes in ionization and temperature, and, correspondingly, in emergent spectra. With the new rates, we find that Zr ( Z = 40) plays a yet more dominant role in kilonova spectra for light r -process compositions. Furthermore, we show that previously predicted mid-infrared (e.g., [Se III ] 4.55 μ m) and optical (e.g., Rb I 7802, 7949 Å) lines weaken in the new model. Instead, [Se I ] 5.03 μ m emerges as a signature. These results demonstrate the importance of considering the detailed microphysics for modelling and interpreting the late-time kilonova spectra.