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A low-mass binary neutron star: long-term ejecta evolution and kilonovae with weak blue emission

Kawaguchi, K., Fujibayashi, S., Shibata, M., Tanaka, M., & Wanajo, S. (2021). A low-mass binary neutron star: long-term ejecta evolution and kilonovae with weak blue emission. The Astrophysical Journal, 913(2): 100. doi:10.3847/1538-4357/abf3bc.

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Creators:
Kawaguchi, Kyohei, Author
Fujibayashi, Sho1, Author
Shibata, Masaru1, Author
Tanaka, Masaomi, Author
Wanajo, Shinya1, Author
Affiliations:
1Computational Relativistic Astrophysics, AEI-Golm, MPI for Gravitational Physics, Max Planck Society, ou_2541714

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Free keywords: Astrophysics, High Energy Astrophysical Phenomena, astro-ph.HE,General Relativity and Quantum Cosmology, gr-qc
Abstract: We study the long-term evolution of ejecta formed in a binary neutron star (BNS) merger that results in a long-lived remnant NS by performing a hydrodynamics simulation with the outflow data of a numerical relativity simulation as the initial condition. At the homologously expanding phase, the total ejecta mass reaches $\approx0.1\,M_\odot$ with an average velocity of $\approx0.1\,c$ and lanthanide fraction of $\approx 0.005$. We further perform the radiative transfer simulation employing the obtained ejecta profile. We find that, contrary to a naive expectation from the large ejecta mass and low lanthanide fraction, the optical emission is not as bright as that in GW170817/AT2017gfo, while the infrared emission can be brighter. This light curve property is attributed to preferential diffusion of photons toward the equatorial direction due to the prolate ejecta morphology, large opacity contribution of Zr, Y, and lanthanides, and low specific heating rate of the ejecta. Our results suggest that these light curve features could be used as an indicator for the presence of a long-lived remnant NS. We also found that the bright optical emission broadly consistent with GW170817/AT2017gfo is realized for the case that the high-velocity ejecta components in the polar region are suppressed. These results suggest that the remnant in GW170817/AT2017gfo is unlikely to be a long-lived NS, but might have collapsed to a black hole within ${\cal O}(0.1)$ s.

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Dates: 2020-12-292021
Publication Status: Published in print
Pages: 24 pages, 21 figures, submitted to ApJ
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Rev. Type: -
Identifiers: arXiv: 2012.14711
DOI: 10.3847/1538-4357/abf3bc
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Title: The Astrophysical Journal
Source Genre: Journal
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Pages: - Volume / Issue: 913 (2) Sequence Number: 100 Start / End Page: - Identifier: -