The thermalization of γ-rays in radioactive expanding ejecta: a simple model and its application for Kilonovae and Ia SNe: a simple model and its application for Kilonovae and Ia SNe

A semi-analytic approximation is derived for the time-dependent fraction fγ (t) of the energy deposited by radioactive decay γ -rays in a homologously expanding plasma of general structure. An analytic approximation is given for spherically symmetric plasma distributions. Applied to Kilonovae (KNe) associated with neutron stars mergers and Type Ia supernovae, our semianalytic and analytic approximations reproduce, with a few per cent and 10 per cent accuracy, respectively, the energy deposition rates, Q˙ _dep, obtained in numeric Monte Carlo calculations. The time t_γ beyond which γ -ray deposition is inefficient is determined by an effective frequency-independent γ -ray opacity κ_{γ ,eff}, t_γ = κγ ,efft 2, where ∝ t−2 is the average plasma column density. For β-decay dominated energy release, κγ ,eff is typically close to the effective Compton scattering opacity, κγ ,eff ≈ 0.025 cm2 g−1 with a weak dependence on composition. For KNe, κγ ,eff depends mainly on the initial electron fraction Ye, κγ ,eff ≈0.03(0.05) cm2 g−1 for Ye ()0.25 (in contrast with earlier work that found κγ ,eff larger by 1–2 orders of magnitude for low Ye), and is insensitive to the (large) nuclear physics uncertainties. Determining tγ from observations will therefore measure the ejecta t 2, providing a stringent test of models. For t 2 = 2 × 1011 g cm−2 s2, a typical value expected for KNe, tγ ≈ 1 d.