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- W3013320005 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)." @default.
- W3013320005 created "2020-04-03" @default.
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- W3013320005 date "2020-03-26" @default.
- W3013320005 modified "2023-09-27" @default.
- W3013320005 title "r-Process and Kilonovae" @default.
- W3013320005 doi "https://doi.org/10.7566/jpscp.31.011006" @default.
- W3013320005 hasPublicationYear "2020" @default.
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