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The simulations of early kilonova emission from neutron star mergers

Published online by Cambridge University Press:  27 February 2023

Smaranika Banerjee Open the ORCID record for Smaranika Banerjee [Opens in a new window] ,
Masaomi Tanaka Open the ORCID record for Masaomi Tanaka [Opens in a new window] ,
Kyohei Kawaguchi ,
Daiji Kato  and
Gediminas Gaigalas
Smaranika Banerjee
Affiliation:
Astronomical Institute, Tohoku University, Aoba, Sendai 980-8578, Japan email: [email protected]
Masaomi Tanaka
Affiliation:
Astronomical Institute, Tohoku University, Aoba, Sendai 980-8578, Japan email: [email protected]
Kyohei Kawaguchi
Affiliation:
Institute for Cosmic Ray Research, The University of Tokyo, 5-1-5 Kashiwanoha, Kashiwa, Chiba 277-8582, Japan
Daiji Kato
Affiliation:
National Institute for Fusion Science, National Institutes of Natural Sciences, Department of Advanced Energy Engineering Science, Kyushu University, Oroshi-cho, Toki, Gifu 509-5292, Japan
Gediminas Gaigalas
Affiliation:
Institute of Theoretical Physics and Astronomy, Vilnius University, Saulėtekio av. 3, LT-10257 Vilnius, Lithuania
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Abstract

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In the neutron-star mergers, the radioactive decay of freshly synthesized heavy elements produces emissions in the ultraviolet-optical-infrared range, producing a transient called kilonova. The observational properties of the kilonova depend on the bound-bound opacity of the heavy elements, which was largely unavailable for the conditionssuitable at an early time (t < day). In this article, I share some of our recent progress on modeling the early kilonova light curve, focusing on the atomic opacity calculation.

Keywords

opacitystars: neutronradiative transfer
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. 233 - 236
Copyright
© The Author(s), 2023. Published by Cambridge University Press on behalf of International Astronomical Union

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