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Evidence for $\gtrsim{4}$ Gyr timescales of neutron star mergers from Galactic archaeology
Astrophysics of Galaxies · Submitted 10 Jan 2020
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Now for the first time, we combine all the available observational evidence of the Milky Way and its dwarf galaxy satellites to show that the data can only be explained if there are (at least) two distinct $r$-process sites: a quick source with timescales comparable to core-collapse supernovae, $t_{quick}\lesssim10^8$ yr, and a delayed source with characteristic timescales $t_{delayed}\gtrsim4$ Gyr.
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The abstract, sentence by sentence
The nucleosynthetic site of the rapid ($r$) neutron-capture process is currently being debated. The direct detection of the neutron star merger GW170817, through gravitational waves and electromagnetic radiation, has confirmed such events as important sources of the $r$-process elements. However, chemical evolution models are not able to reproduce the observed chemical abundances in the Milky Way when neutron star mergers are assumed to be the only $r$-process site and realistic time distributions of such events are taken into account. Now for the first time, we combine all the available observational evidence of the Milky Way and its dwarf galaxy satellites to show that the data can only be explained if there are (at least) two distinct $r$-process sites: a quick source with timescales comparable to core-collapse supernovae, $t_{quick}\lesssim10^8$ yr, and a delayed source with characteristic timescales $t_{delayed}\gtrsim4$ Gyr. The delayed $r$-process source most probably originates in neutron star mergers, as the timescale fits well with that estimated for GW170817. Given the short timescales of the quick source, it is likely associated with massive stars, though a specific fast-track channel for compact object mergers cannot be excluded at this point. Our approach demonstrates that only by looking at all the available data will we be able to solve the puzzle that is the $r$-process.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The nucleosynthetic site of the rapid ($r$) neutron-capture process is currently being debated. | background 0.96 | 0.03 | 0.01 | asserted 0.79 |
| s1 | The direct detection of the neutron star merger GW170817, through gravitational waves and electromagnetic radiation, has confirmed such events as important sources of the $r$-process elements. | background 1.00 | 0.05 | 0.02 | asserted 1.00 |
| s2 | However, chemical evolution models are not able to reproduce the observed chemical abundances in the Milky Way when neutron star mergers are assumed to be the only $r$-process site and realistic time distributions of such events are taken into account. | gap 0.66 | 0.12 | 0.04 | asserted 1.00 |
| s3 | Now for the first time, we combine all the available observational evidence of the Milky Way and its dwarf galaxy satellites to show that the data can only be explained if there are (at least) two distinct $r$-process sites: a quick source with timescales comparable to core-collapse supernovae, $t_{quick}\lesssim10^8$ yr, and a delayed source with characteristic timescales $t_{delayed}\gtrsim4$ Gyr. | result 0.87 | 0.95 | 0.94 | asserted 1.00 |
| s4 | The delayed $r$-process source most probably originates in neutron star mergers, as the timescale fits well with that estimated for GW170817. | interpretation 0.99 | 0.43 | 0.10 | hedged possibility 0.99 |
| s5 | Given the short timescales of the quick source, it is likely associated with massive stars, though a specific fast-track channel for compact object mergers cannot be excluded at this point. | interpretation 0.99 | 0.31 | 0.04 | hedged possibility 1.00 |
| s6 | Our approach demonstrates that only by looking at all the available data will we be able to solve the puzzle that is the $r$-process. | interpretation 0.72 | 0.58 | 0.06 | asserted 0.99 |
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Original abstract
The nucleosynthetic site of the rapid ($r$) neutron-capture process is currently being debated. The direct detection of the neutron star merger GW170817, through gravitational waves and electromagnetic radiation, has confirmed such events as important sources of the $r$-process elements. However, chemical evolution models are not able to reproduce the observed chemical abundances in the Milky Way when neutron star mergers are assumed to be the only $r$-process site and realistic time distributions of such events are taken into account. Now for the first time, we combine all the available observational evidence of the Milky Way and its dwarf galaxy satellites to show that the data can only be explained if there are (at least) two distinct $r$-process sites: a quick source with timescales comparable to core-collapse supernovae, $t_{quick}\lesssim10^8$ yr, and a delayed source with characteristic timescales $t_{delayed}\gtrsim4$ Gyr. The delayed $r$-process source most probably originates in neutron star mergers, as the timescale fits well with that estimated for GW170817. Given the short timescales of the quick source, it is likely associated with massive stars, though a specific fast-track channel for compact object mergers cannot be excluded at this point. Our approach demonstrates that only by looking at all the available data will we be able to solve the puzzle that is the $r$-process.
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References
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1 arXiv paper cite this in 1 sentence
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Uses data or values from 1 paper
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A recent study by [ref] provides ages of $≈6600$ stars in the Sagittarius nuclear star cluster, M54, which we use as a proxy of its SFH in Fig. [ref] (dark green solid line).
A deep view into the nucleus of the Sagittarius Dwarf Spheroidal Galaxy with MUSE. I. Data and stellar population characterization · Star formation histories · 1.00
Cites as support 1 paper
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On the other hand, if short timescales of NSMs are assumed ($≲10^8$ yr), the abundance trend of the Milky Way disks can be readily explained (e.g. [ref] ).
Modelling the chemical evolution of Zr, La, Ce and Eu in the Galactic discs and bulge · Introduction · 0.96
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