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r-process enrichment of ultra-faint dwarf galaxies by fast merging double neutron stars
High Energy Astrophysical Phenomena · Submitted 9 Oct 2018
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim Assuming that such dwarf systems have lost a significant fraction of their stellar mass through tidal stripping, we conclude that contrary to most current models, it is the DNSs with rather large natal kicks but very short merging timescales that can enrich UFD-type galaxies.
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The abstract, sentence by sentence
The recent aLIGO/aVirgo discovery of gravitational waves from the neutron star merger (NSM) GW170817 and the follow up kilonova observations have shown that NSMs produce copious amount of r-process material. However, it is difficult to reconcile the large natal kicks and long average merging times of Double Neutron Stars (DNSs), with the levels of r-process enrichment seen in ultra faint dwarf (UFD) galaxies such as Reticulum II and Tucana III. Assuming that such dwarf systems have lost a significant fraction of their stellar mass through tidal stripping, we conclude that contrary to most current models, it is the DNSs with rather large natal kicks but very short merging timescales that can enrich UFD-type galaxies. These binaries are either on highly eccentric orbits, or form with very short separations due to an additional mass-transfer between the first-born neutron star and a naked helium star, progenitor of the second-born neutron star. These DNSs are born with a frequency that agrees with the statistics of the r-process UFDs, and merge well within the virial radius of their host halos, therefore contributing significantly to their r-process enrichment.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | The recent aLIGO/aVirgo discovery of gravitational waves from the neutron star merger (NSM) GW170817 and the follow up kilonova observations have shown that NSMs produce copious amount of r-process material. | background 1.00 | 0.05 | 0.03 | asserted 1.00 |
| s1 | However, it is difficult to reconcile the large natal kicks and long average merging times of Double Neutron Stars (DNSs), with the levels of r-process enrichment seen in ultra faint dwarf (UFD) galaxies such as Reticulum II and Tucana III. | gap 0.57 | 0.10 | 0.04 | asserted 0.97 |
| s2 | Assuming that such dwarf systems have lost a significant fraction of their stellar mass through tidal stripping, we conclude that contrary to most current models, it is the DNSs with rather large natal kicks but very short merging timescales that can enrich UFD-type galaxies. | result 0.71 | 0.76 | 0.92 | asserted 0.88 |
| s3 | These binaries are either on highly eccentric orbits, or form with very short separations due to an additional mass-transfer between the first-born neutron star and a naked helium star, progenitor of the second-born neutron star. | interpretation 0.41 | 0.40 | 0.05 | asserted 0.81 |
| s4 | These DNSs are born with a frequency that agrees with the statistics of the r-process UFDs, and merge well within the virial radius of their host halos, therefore contributing significantly to their r-process enrichment. | result 0.87 | 0.72 | 0.23 | asserted 0.99 |
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Original abstract
The recent aLIGO/aVirgo discovery of gravitational waves from the neutron star merger (NSM) GW170817 and the follow up kilonova observations have shown that NSMs produce copious amount of r-process material. However, it is difficult to reconcile the large natal kicks and long average merging times of Double Neutron Stars (DNSs), with the levels of r-process enrichment seen in ultra faint dwarf (UFD) galaxies such as Reticulum II and Tucana III. Assuming that such dwarf systems have lost a significant fraction of their stellar mass through tidal stripping, we conclude that contrary to most current models, it is the DNSs with rather large natal kicks but very short merging timescales that can enrich UFD-type galaxies. These binaries are either on highly eccentric orbits, or form with very short separations due to an additional mass-transfer between the first-born neutron star and a naked helium star, progenitor of the second-born neutron star. These DNSs are born with a frequency that agrees with the statistics of the r-process UFDs, and merge well within the virial radius of their host halos, therefore contributing significantly to their r-process enrichment.
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References
How the literature uses it
5 arXiv papers cite this in 5 sentences
Papers citing it · 4 sentences without a confident label
Cites it as support 1 paper
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Though the fast-merging channel assumed has NOT been confirmed, it is well motivated by another two observation facts: GW190425 [ref] and the r-process material in the Universe [ref] .
Repeating Fast Radio Bursts from Neutron Star Binaries: Multi-band and Multi-messenger Opportunities · Introduction · 0.99
What it cites · 3 sentences without a confident label
Uses data or values from 1 paper
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For instance, the observed tidal tails around Tucana III indicate that about 80% of the stellar mass is in the process of being tidally stripped [ref] , which would make the total stellar mass of Tucana III $≈4.6×10^3$.
Stellar Streams Discovered in the Dark Energy Survey · Comparing to observations · 0.86
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