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Modeling kilonova emission from neutron star mergers

Published online by Cambridge University Press:  27 February 2023

Masaomi Tanaka Open the ORCID record for Masaomi Tanaka [Opens in a new window] ,
Daiji Kato ,
Gediminas Gaigalas ,
Kyohei Kawaguchi ,
Laima Radžiūtė ,
Pavel Rynkun ,
Smaranika Banerjee Open the ORCID record for Smaranika Banerjee [Opens in a new window]  and
Nanae Domoto Open the ORCID record for Nanae Domoto [Opens in a new window]
Masaomi Tanaka
Affiliation:
Astronomical Institute, Tohoku University, Sendai 980-8578, Japan email: [email protected]
Daiji Kato
Affiliation:
National Institute for Fusion Science, 322-6 Oroshi-cho, Toki 509-5292, Japan Interdisciplinary Graduate School of Engineering Sciences, Kyushu University, Kasuga, Fukuoka 816-8580, Japan
Gediminas Gaigalas
Affiliation:
Institute of Theoretical Physics and Astronomy, Vilnius University, Saulėtekio Ave. 3, Vilnius, Lithuania
Kyohei Kawaguchi
Affiliation:
Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan
Laima Radžiūtė
Affiliation:
Institute of Theoretical Physics and Astronomy, Vilnius University, Saulėtekio Ave. 3, Vilnius, Lithuania
Pavel Rynkun
Affiliation:
Institute of Theoretical Physics and Astronomy, Vilnius University, Saulėtekio Ave. 3, Vilnius, Lithuania
Smaranika Banerjee
Affiliation:
Astronomical Institute, Tohoku University, Sendai 980-8578, Japan email: [email protected]
Nanae Domoto
Affiliation:
Astronomical Institute, Tohoku University, Sendai 980-8578, Japan email: [email protected]
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Abstract

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Coalescence of binary neutron stars gives rise to kilonova, thermal emission powered by radioactive decays of newly synthesized r-process nuclei. Observational properties of kilonova are largely affected by bound-bound opacities of r-process elements. It is, thus, important to understand atomic properties of heavy elements to link the observed signals with nucleosynthesis of neutron star mergers. In this paper, we introduce the latest status of kilonova modeling by focusing on the aspects of atomic physics. We perform systematic atomic structure calculations of r-process elements to understand element-to-element variation in the opacities. We demonstrate that the properties of the atomic structure of heavy elements are imprinted in the opacities of the neutron star merger ejecta and consequently in the kilonova light curves and spectra. Using this latest opacity dataset, we briefly discuss implications for GW170817, expected diversity of kilonova emission, and prospects for element identification in kilonova spectra.

Keywords

radiative transferopacitystars: neutron
Type
Contributed Paper
Information
Proceedings of the International Astronomical Union , Volume 16 , Symposium S363: Neutron Star Astrophysics at the Crossroads: Magnetars and the Multimessenger Revolution , June 2020 , pp. 127 - 134
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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