# Systematic Opacity Calculations for Kilonovae

## TL;DR

This paper systematically calculates opacities of r-process elements in neutron star merger ejecta, revealing element-specific effects on kilonova emission and improving modeling accuracy for observed events like GW170817.

## Contribution

First systematic atomic structure calculations of r-process element opacities, showing element-dependent effects and their impact on kilonova light curves.

## Key findings

- Fewer electrons in outer shells lead to higher contributions to opacity.
- Average opacities vary significantly with electron fraction and temperature.
- Opacity in ejecta changes over time, affecting kilonova emission features.

## Abstract

Coalescence of neutron stars gives rise to kilonova, thermal emission powered by radioactive decays of freshly synthesized r-process nuclei. Although observational properties are largely affected by bound-bound opacities of r-process elements, available atomic data have been limited. In this paper, we study element-to-element variation of the opacities in the ejecta of neutron star mergers by performing systematic atomic structure calculations of r-process elements for the first time. We show that the distributions of energy levels tend to be higher as electron occupation increases for each electron shell due to the larger energy spacing caused by larger effects of spin-orbit and electron-electron interactions. As a result, elements with a fewer number of electrons in the outermost shells tend to give larger contributions to the bound-bound opacities. This implies that Fe is not representative for the opacities of light r-process elements. The average opacities for the mixture of r-process elements are found to be kappa ~ 20-30 cm^2 g^{-1} for the electron fraction of Ye < 0.20, kappa ~ 3-5 cm^2 g^{-1} for Ye = 0.25-0.35, and kappa ~ 1 cm^2 g^{-1} for Ye = 0.40 at T = 5,000-10,000 K, and they steeply decrease at lower temperature. We show that, even with the same abundance or Ye, the opacity in the ejecta changes with time by one order of magnitude from 1 to 10 days after the merger. Our radiative transfer simulations with the new opacity data confirm that ejecta with a high electron fraction (Ye >~ 0.25, with no lanthanide) are needed to explain the early, blue emission in GW170817/AT2017gfo while lanthanide-rich ejecta (with a mass fraction of lanthanides ~ 5 x 10^{-3}) reproduce the long-lasting near-infrared emission.