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An $r-$process macronova/kilonova in GRB 060614: evidence for the merger of a neutron star-black hole binary
High Energy Astrophysical Phenomena · Submitted 14 Dec 2015
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim If this interpretation is correct, it represents the first time that a multi-epoch/band lightcurve of a Li-Paczynski macronova (also known as kilonova) has been obtained and black hole-neutron star mergers are sites of significant production of $r-$process elements.
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The abstract, sentence by sentence
After the jet break at $t\sim 1.4$ days, the optical afterglow emission of the long-short burst GRB 060614 can be divided into two components. One is the power-law decaying forward shock afterglow emission. The other is an excess of flux in several multi-band photometric observations, which emerges at $\sim$4 days after the burst, significantly earlier than that observed for a supernova associated with a long-duration GRB. At $t>13.6$ days, the F814W-band flux drops faster than $t^{-3.2}$. Moreover, the spectrum of the excess component is very soft and the luminosity is extremely low. These observed signals are incompatible with those from weak supernovae, but the ejection of $\sim 0.1~M_\odot$ of $r-$process material from a black hole-neutron star merger, as recently found in some numerical simulations, can produce it. If this interpretation is correct, it represents the first time that a multi-epoch/band lightcurve of a Li-Paczynski macronova (also known as kilonova) has been obtained and black hole-neutron star mergers are sites of significant production of $r-$process elements.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | After the jet break at $t\sim 1.4$ days, the optical afterglow emission of the long-short burst GRB 060614 can be divided into two components. | result 1.00 | 0.71 | 0.02 | asserted 1.00 |
| s1 | One is the power-law decaying forward shock afterglow emission. | result 1.00 | 0.50 | 0.02 | asserted 1.00 |
| s2 | The other is an excess of flux in several multi-band photometric observations, which emerges at $\sim$4 days after the burst, significantly earlier than that observed for a supernova associated with a long-duration GRB. | result 1.00 | 0.81 | 0.05 | asserted 1.00 |
| s3 | At $t>13.6$ days, the F814W-band flux drops faster than $t^{-3.2}$. | result 1.00 | 0.82 | 0.02 | asserted 1.00 |
| s4 | Moreover, the spectrum of the excess component is very soft and the luminosity is extremely low. | result 1.00 | 0.83 | 0.03 | asserted 1.00 |
| s5 | These observed signals are incompatible with those from weak supernovae, but the ejection of $\sim 0.1~M_\odot$ of $r-$process material from a black hole-neutron star merger, as recently found in some numerical simulations, can produce it. | interpretation 1.00 | 0.23 | 0.57 | hedged possibility 0.78 |
| s6 | If this interpretation is correct, it represents the first time that a multi-epoch/band lightcurve of a Li-Paczynski macronova (also known as kilonova) has been obtained and black hole-neutron star mergers are sites of significant production of $r-$process elements. | interpretation 0.94 | 0.53 | 0.86 | hedged possibility 0.82 |
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Original abstract
After the jet break at $t\sim 1.4$ days, the optical afterglow emission of the long-short burst GRB 060614 can be divided into two components. One is the power-law decaying forward shock afterglow emission. The other is an excess of flux in several multi-band photometric observations, which emerges at $\sim$4 days after the burst, significantly earlier than that observed for a supernova associated with a long-duration GRB. At $t>13.6$ days, the F814W-band flux drops faster than $t^{-3.2}$. Moreover, the spectrum of the excess component is very soft and the luminosity is extremely low. These observed signals are incompatible with those from weak supernovae, but the ejection of $\sim 0.1~M_\odot$ of $r-$process material from a black hole-neutron star merger, as recently found in some numerical simulations, can produce it. If this interpretation is correct, it represents the first time that a multi-epoch/band lightcurve of a Li-Paczynski macronova (also known as kilonova) has been obtained and black hole-neutron star mergers are sites of significant production of $r-$process elements.
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