On the validity of steady-state for nebular phase kilonovae

Abstract

The radioactively powered transient following a binary neutron star merger, known as a kilonova (KN), is expected to enter the steady-state nebular phase a few days after merger. Steady-state holds until thermal reprocessing time-scales become long, at which point the temperature and ionization states need to be evolved time-dependently. We study the onset and significance of time-dependent effects using the non-local thermodynamic equilibrium spectral synthesis code sumo. We employ a simple single-zone model with an elemental composition of Te, Ce, Pt, and Th, scaled to their respective solar abundances. The atomic data are generated using the Flexible Atomic Code (fac), and consist of energy levels and radiative transitions, including highly forbidden lines. We explore the KN evolution from 5 to 100 d after merger, varying ejecta mass and velocity. We also consider variations in the degree of electron magnetic field trapping, as well as radioactive power generation for alpha and beta decay (but omitting fission products). We find that the transition time, and magnitude of steady-state deviations are highly sensitive to these parameters. For typical KN ejecta, the deviations are minor within the time-frame studied. However, low density ejecta with low energy deposition show significant differences from ∼10 d. Important deviation of the ionization structure solution impacts the temperature by altering the overall line cooling. Adiabatic cooling becomes important at t ≥ 60 d which, in addition to the temperature and ionization effects, lead to the bolometric light-curve deviating from the instantaneous radioactive power deposited.