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Kilonova from post-merger ejecta as an optical and near-Infrared counterpart of GW170817

Tanaka, M, Utsumi, Y, Mazzali, PA, Tominaga, N, Yoshida, M, Sekiguchi, Y, Morokuma, T, Motohara, K, Ohta, K, Kawabata, KS, Abe, F, Aoki, K, Asakura, Y, Baar, S, Barway, S, Bond, IA, Doi, M, Fujiyoshi, T, Furusawa, H, Honda, S , Itoh, Y, Kawabata, M, Kawai, N, Kim, JH, Lee, C-H, Miyazaki, S, Morihana, K, Nagashima, H, Nagayama, T, Nakaoka, T, Nakata, F, Ohsawa, R, Ohshima, T, Okita, H, Saito, T, Sumi, T, Tajitsu, A, Takahashi, J, Takayama, M, Tamura, Y, Tanaka, I, Terai, T, Tristram, PJ, Yasuda, N and Zenko, T (2017) Kilonova from post-merger ejecta as an optical and near-Infrared counterpart of GW170817. Publications of the Astronomical Society of Japan, 69 (6). ISSN 0004-6264

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Recent detection of gravitational waves from a neutron star (NS) merger event GW170817 and identification of an electromagnetic counterpart provide a unique opportunity to study the physical processes in NS mergers. To derive properties of ejected material from the NS merger, we perform radiative transfer simulations of kilonova, optical and near-infrared emissions powered by radioactive decays of r-process nuclei synthesized in the merger. We find that the observed near-infrared emission lasting for >10 d is explained by 0.03 M⊙ of ejecta containing lanthanide elements. However, the blue optical component observed at the initial phases requires an ejecta component with a relatively high electron fraction (Ye). We show that both optical and near-infrared emissions are simultaneously reproduced by the ejecta with a medium Ye of ∼0.25. We suggest that a dominant component powering the emission is post-merger ejecta, which exhibits that the mass ejection after the first dynamical ejection is quite efficient. Our results indicate that NS mergers synthesize a wide range of r-process elements and strengthen the hypothesis that NS mergers are the origin of r-process elements in the Universe.

Item Type: Article
Additional Information: This is a pre-copyedited, author-produced version of an article accepted for publication in Publications of the Astronomical Society of Japan following peer review. The version of record Masaomi Tanaka, Yousuke Utsumi, Paolo A. Mazzali, Nozomu Tominaga, Michitoshi Yoshida, Yuichiro Sekiguchi, Tomoki Morokuma, Kentaro Motohara, Kouji Ohta, Koji S. Kawabata, Fumio Abe, Kentaro Aoki, Yuichiro Asakura, Stefan Baar, Sudhanshu Barway, Ian A. Bond, Mamoru Doi, Takuya Fujiyoshi, Hisanori Furusawa, Satoshi Honda, Yoichi Itoh, Miho Kawabata, Nobuyuki Kawai, Ji Hoon Kim, Chien-Hsiu Lee, Shota Miyazaki, Kumiko Morihana, Hiroki Nagashima, Takahiro Nagayama, Tatsuya Nakaoka, Fumiaki Nakata, Ryou Ohsawa, Tomohito Ohshima, Hirofumi Okita, Tomoki Saito, Takahiro Sumi, Akito Tajitsu, Jun Takahashi, Masaki Takayama, Yoichi Tamura, Ichi Tanaka, Tsuyoshi Terai, Paul J. Tristram, Naoki Yasuda, Tetsuya Zenko; Kilonova from post-merger ejecta as an optical and near-Infrared counterpart of GW170817, Publications of the Astronomical Society of Japan, Volume 69, Issue 6, 1 December 2017, 102, is available online at: http://dx.doi.org/10.1093/pasj/psx121
Uncontrolled Keywords: 0201 Astronomical And Space Sciences
Subjects: Q Science > QB Astronomy
Q Science > QC Physics
Divisions: Astrophysics Research Institute
Publisher: Oxford University Press (OUP)
Related URLs:
Date Deposited: 30 Oct 2018 11:51
Last Modified: 04 Sep 2021 02:19
DOI or ID number: 10.1093/pasj/psx121
URI: https://researchonline.ljmu.ac.uk/id/eprint/9495
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