Impact of Ejecta Temperature and Mass on the Strength of Heavy Element Signatures in Kilonovae

Abstract

A kilonova, the electromagnetic emission produced by compact binary mergers, is formed through a delicate interplay of physical processes, involving r-process nucleosynthesis and interactions between heavy elements and photons through radiative transfer. This complexity makes it difficult to achieve a comprehensive understanding of kilonova spectra. In this study, we aim to enhance our understanding and establish connections between physical parameters and observables through radiative-transfer simulations. Specifically, we investigate how ejecta temperature and element mass influence the resulting kilonova spectrum. For each species, the strength of its line features depends on these parameters, leading to the formation of a distinct region in the parameter space, dubbed the Resonance Island, where the line signature of that species is notably evident in the kilonova spectrum. We explore its origin and applications. Among explored r-process elements (31$\le$Z$\le$92), we find that four species -- Sr${}_{\mathrm{II}}$, Y${}_{\mathrm{II}}$, Ba${}_{\mathrm{II}}$, and Ce${}_{\mathrm{II}}$ -- exhibit large and strong resonance islands, suggesting their significant contributions to kilonova spectra at specific wavelengths. In addition, we discuss potential challenges and future perspectives in observable heavy elements and their masses in the context of the resonance island.

13 pages, 10 figures, 1 table, ApJ published

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Cited by in corpus (2)

• Emergence hour-by-hour of $r$-process features in the kilonova AT2017gfo
• Data-driven approach for modeling the temporal and spectral evolution of kilonova systematic uncertainties