Kilonova/Macronova Emission from Compact Binary Mergers
We review current understanding of kilonova/macronova emission from compact binary mergers (mergers of two neutron stars or a neutron star and a black hole). Kilonova/macronova is emission powered by radioactive decays of r-process nuclei and it is one of the most promising electromagnetic counterpa...
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| Language: | English |
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Wiley
2016-01-01
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| Series: | Advances in Astronomy |
| Online Access: | http://dx.doi.org/10.1155/2016/6341974 |
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| author | Masaomi Tanaka |
| author_facet | Masaomi Tanaka |
| author_sort | Masaomi Tanaka |
| collection | DOAJ |
| description | We review current understanding of kilonova/macronova emission from compact binary mergers (mergers of two neutron stars or a neutron star and a black hole). Kilonova/macronova is emission powered by radioactive decays of r-process nuclei and it is one of the most promising electromagnetic counterparts of gravitational wave sources. Emission from the dynamical ejecta of ~0.01M⊙ is likely to have a luminosity of ~1040–1041 erg s−1 with a characteristic timescale of about 1 week. The spectral peak is located in red optical or near-infrared wavelengths. A subsequent accretion disk wind may provide an additional luminosity or an earlier/bluer emission if it is not absorbed by the precedent dynamical ejecta. The detection of near-infrared excess in short GRB 130603B and possible optical excess in GRB 060614 supports the concept of the kilonova/macronova scenario. At 200 Mpc distance, a typical peak brightness of kilonova/macronova with 0.01M⊙ ejecta is about 22 mag and the emission rapidly fades to >24 mag within ~10 days. Kilonova/macronova candidates can be distinguished from supernovae by (1) the faster time evolution, (2) fainter absolute magnitudes, and (3) redder colors. Since the high expansion velocity (v~0.1–0.2c) is a robust outcome of compact binary mergers, the detection of smooth spectra will be the smoking gun to conclusively identify the gravitational wave source. |
| format | Article |
| id | doaj-art-8af0d6fd051c47248f2a5473a9df4bf8 |
| institution | Kabale University |
| issn | 1687-7969 1687-7977 |
| language | English |
| publishDate | 2016-01-01 |
| publisher | Wiley |
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| series | Advances in Astronomy |
| spelling | doaj-art-8af0d6fd051c47248f2a5473a9df4bf82025-02-03T01:25:36ZengWileyAdvances in Astronomy1687-79691687-79772016-01-01201610.1155/2016/63419746341974Kilonova/Macronova Emission from Compact Binary MergersMasaomi Tanaka0National Astronomical Observatory of Japan, Mitaka, Tokyo 181-8588, JapanWe review current understanding of kilonova/macronova emission from compact binary mergers (mergers of two neutron stars or a neutron star and a black hole). Kilonova/macronova is emission powered by radioactive decays of r-process nuclei and it is one of the most promising electromagnetic counterparts of gravitational wave sources. Emission from the dynamical ejecta of ~0.01M⊙ is likely to have a luminosity of ~1040–1041 erg s−1 with a characteristic timescale of about 1 week. The spectral peak is located in red optical or near-infrared wavelengths. A subsequent accretion disk wind may provide an additional luminosity or an earlier/bluer emission if it is not absorbed by the precedent dynamical ejecta. The detection of near-infrared excess in short GRB 130603B and possible optical excess in GRB 060614 supports the concept of the kilonova/macronova scenario. At 200 Mpc distance, a typical peak brightness of kilonova/macronova with 0.01M⊙ ejecta is about 22 mag and the emission rapidly fades to >24 mag within ~10 days. Kilonova/macronova candidates can be distinguished from supernovae by (1) the faster time evolution, (2) fainter absolute magnitudes, and (3) redder colors. Since the high expansion velocity (v~0.1–0.2c) is a robust outcome of compact binary mergers, the detection of smooth spectra will be the smoking gun to conclusively identify the gravitational wave source.http://dx.doi.org/10.1155/2016/6341974 |
| spellingShingle | Masaomi Tanaka Kilonova/Macronova Emission from Compact Binary Mergers Advances in Astronomy |
| title | Kilonova/Macronova Emission from Compact Binary Mergers |
| title_full | Kilonova/Macronova Emission from Compact Binary Mergers |
| title_fullStr | Kilonova/Macronova Emission from Compact Binary Mergers |
| title_full_unstemmed | Kilonova/Macronova Emission from Compact Binary Mergers |
| title_short | Kilonova/Macronova Emission from Compact Binary Mergers |
| title_sort | kilonova macronova emission from compact binary mergers |
| url | http://dx.doi.org/10.1155/2016/6341974 |
| work_keys_str_mv | AT masaomitanaka kilonovamacronovaemissionfromcompactbinarymergers |