Year: 2019
Type: preprint
Abstract: The kilonova associated with the neutron star merger GW170817 provides us with several hints to elucidate the nature of the r-process in the universe. In this article, we inspect the radioactive isotopes that powered the kilonova emission, provided that the merger ejecta consisted of material with a solar r-like abundance pattern. It is suggested that the early (1-10 days after merger) kilonova emission is mainly due to the beta-decay chain 66Ni -> 66Cu -> 66Zn, which can be the source of the steepening of the light curve at about 7 days. The late time (> 10 days) heaing is attributed to the alpha-decay and fission (254Cf) of trans-Pb species (in addition to beta-decay), which can be the signature of r-processing beyond the heaviest stable elements. This article summarizes a recent work by the author (Wanajo 2018) with the additional calculations of kilonova light curves by using a numerical code in Hotokezaka and Nakar (2019).
Source: arXiv (Cornell University)
Author: Wanajo, Shinya
Institution: Max Planck Society
Language: English
Subfield: Astronomy and Astrophysics
Field: Physics and Astronomy
Domain: Physical Sciences
Open Access status: green
OpenAlex ID: W2985199433