Origin of the heavy elements in binary neutron-star mergers from a gravitational-wave event
2017/10/16 by Daniel Kasen, Brian Metzger, Brian D. Metzger +4 · 1,193 citations
Physics and Astronomy · #Astronomy #Astrophysics #Ejecta #Gamma-ray bursts and supernovae #Gravitational wave #Kilonova #Laser-Plasma Interactions and Diagnostics #Neutron star #Nucleosynthesis #Physics #Pulsars and Gravitational Waves Research #Stars #Supernova #astro-ph.HE #r-process
paper · pdf · doi:10.1038/nature24453
published in Nature 551(7678), 80-84 (Nature Portfolio) · Nature
arxiv created 2017/10/16 · openalex publication_date 2017/10/16 · arxiv updated 2017/10/17 · openalex created_date 2025/10/10 · openalex updated_date 2026/08/05
Abstract
The cosmic origin of the elements heavier than iron has long been uncertain. Theoretical modelling shows that the matter that is expelled in the violent merger of two neutron stars can assemble into heavy elements such as gold and platinum in a process known as rapid neutron capture (r-process) nucleosynthesis. The radioactive decay of isotopes of the heavy elements is predicted to power a distinctive thermal glow (a 'kilonova'). The discovery of an electromagnetic counterpart to the gravitational-wave source GW170817 represents the first opportunity to detect and scrutinize a sample of freshly synthesized r-process elements. Here we report models that predict the detailed electromagnetic emission of kilonovae and enable the mass, velocity and composition of ejecta to be derived from the observations. We compare the models to the optical and infrared radiation associated with GW170817 event to argue that the observed source is a kilonova. We infer the presence of two distinct components of ejecta, one composed primarily of light (atomic mass number less than 140) and one of heavy (atomic mass number greater than 140) r-process elements. Inferring the ejected mass and a merger rate from GW170817 implies that such mergers are a dominant mode of r-process production in the Universe.
Cited by
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