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The impact of binary stars on the dust and metal evolution of galaxies
Astrophysics of Galaxies · Submitted 23 Oct 2023
abstract compiled · 2026-09-23 · no language-model review
The authors' main claim We find that binaries have a negligible impact on the stellar masses, gas masses, and star formation rates of galaxies only if the total mass ejected by massive stars is unchanged.
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The abstract, sentence by sentence
We present detailed implementations of (a) binary stellar evolution (using binary_c) and (b) dust production and destruction into the cosmological semi-analytic galaxy evolution simulation, L-Galaxies. This new version of L-Galaxies is compared to a version assuming only single stars and to global and spatially-resolved observational data across a range of redshifts ($z$). We find that binaries have a negligible impact on the stellar masses, gas masses, and star formation rates of galaxies only if the total mass ejected by massive stars is unchanged. This is because massive stars determine the strength of supernova (SN) feedback, which in turn regulates galaxy growth. Binary effects, such as common envelope ejection and novae, affect carbon and nitrogen enrichment in galaxies, however heavier alpha elements are more affected by the choice of SN and wind yields. Unlike many other simulations, the new L-Galaxies reproduces observed dust-to-metal (DTM) and dust-to-gas (DTG) ratios at $z\sim{}0-4$. This is mainly due to shorter dust accretion timescales in dust-rich environments. However, dust masses are under-predicted at $z>4$, highlighting the need for enhanced dust production at early times in simulations, possibly accompanied by increased star formation. On sub-galactic scales, there is very good agreement between L-Galaxies and observed dust and metal radial profiles at $z=0$. A drop in DTM ratio is also found in diffuse, low-metallicity regions, contradicting the assumption of a universal value. We hope that this work serves as a useful template for binary stellar evolution implementations in other cosmological simulations in future.
background contribution method result interpretation main claim
| # | sentence | role | the authors' own work | states the main conclusion | strength |
|---|---|---|---|---|---|
| s0 | We present detailed implementations of (a) binary stellar evolution (using binary_c) and (b) dust production and destruction into the cosmological semi-analytic galaxy evolution simulation, L-Galaxies. | contribution 0.55 | 0.94 | 0.03 | asserted 0.97 |
| s1 | This new version of L-Galaxies is compared to a version assuming only single stars and to global and spatially-resolved observational data across a range of redshifts ($z$). | method 0.83 | 0.83 | 0.03 | asserted 0.95 |
| s2 | We find that binaries have a negligible impact on the stellar masses, gas masses, and star formation rates of galaxies only if the total mass ejected by massive stars is unchanged. | result 1.00 | 0.97 | 0.56 | asserted 1.00 |
| s3 | This is because massive stars determine the strength of supernova (SN) feedback, which in turn regulates galaxy growth. | interpretation 1.00 | 0.53 | 0.08 | asserted 1.00 |
| s4 | Binary effects, such as common envelope ejection and novae, affect carbon and nitrogen enrichment in galaxies, however heavier alpha elements are more affected by the choice of SN and wind yields. | result 0.96 | 0.88 | 0.08 | asserted 1.00 |
| s5 | Unlike many other simulations, the new L-Galaxies reproduces observed dust-to-metal (DTM) and dust-to-gas (DTG) ratios at $z\sim{}0-4$. | result 1.00 | 0.92 | 0.14 | asserted 1.00 |
| s6 | This is mainly due to shorter dust accretion timescales in dust-rich environments. | interpretation 0.97 | 0.79 | 0.05 | asserted 0.99 |
| s7 | However, dust masses are under-predicted at $z>4$, highlighting the need for enhanced dust production at early times in simulations, possibly accompanied by increased star formation. | limitation 0.87 | 0.92 | 0.09 | asserted 0.76 |
| s8 | On sub-galactic scales, there is very good agreement between L-Galaxies and observed dust and metal radial profiles at $z=0$. | result 1.00 | 0.92 | 0.06 | asserted 1.00 |
| s9 | A drop in DTM ratio is also found in diffuse, low-metallicity regions, contradicting the assumption of a universal value. | result 0.95 | 0.91 | 0.06 | asserted 1.00 |
| s10 | We hope that this work serves as a useful template for binary stellar evolution implementations in other cosmological simulations in future. | future work 1.00 | 0.09 | 0.03 | hedged possibility 0.50 |
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The paper
Original abstract
We present detailed implementations of (a) binary stellar evolution (using binary_c) and (b) dust production and destruction into the cosmological semi-analytic galaxy evolution simulation, L-Galaxies. This new version of L-Galaxies is compared to a version assuming only single stars and to global and spatially-resolved observational data across a range of redshifts ($z$). We find that binaries have a negligible impact on the stellar masses, gas masses, and star formation rates of galaxies only if the total mass ejected by massive stars is unchanged. This is because massive stars determine the strength of supernova (SN) feedback, which in turn regulates galaxy growth. Binary effects, such as common envelope ejection and novae, affect carbon and nitrogen enrichment in galaxies, however heavier alpha elements are more affected by the choice of SN and wind yields. Unlike many other simulations, the new L-Galaxies reproduces observed dust-to-metal (DTM) and dust-to-gas (DTG) ratios at $z\sim{}0-4$. This is mainly due to shorter dust accretion timescales in dust-rich environments. However, dust masses are under-predicted at $z>4$, highlighting the need for enhanced dust production at early times in simulations, possibly accompanied by increased star formation. On sub-galactic scales, there is very good agreement between L-Galaxies and observed dust and metal radial profiles at $z=0$. A drop in DTM ratio is also found in diffuse, low-metallicity regions, contradicting the assumption of a universal value. We hope that this work serves as a useful template for binary stellar evolution implementations in other cosmological simulations in future.
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How the literature uses it
3 arXiv papers cite this in 4 sentences
Papers citing it · 2 sentences without a confident label
Uses its method or tool 1 paper
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We add a new module for the identification and characterization of Be-XRBs to the BPS code https://binary_c.gitlab.io/ binary\_c [ref] , which simulates the evolution of stars in each binary and the binary orbit governed by binary interactions (e.g., mass transfer and tidal effects) and stellar evolution processes such as winds and supernovae (SNe).
Population synthesis of Be X-ray binaries: metallicity dependence of total X-ray outputs · Binary population synthesis · 0.99
Cites it as background 1 paper
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Many extensions to L-Galaxies have been developed, including those that focus on the gas [ref] , stars [ref] , massive black holes [ref] , and other components [ref] .
Massive Star Clusters in the Semi-Analytical Galaxy Formation Model L-Galaxies 2020 · The semi-analytical galaxy formation model · 0.95
What it cites · 4 sentences without a confident label
Compares with 2 papers
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A similar result has also been found for the CROC simulations [ref] using a simpler dust model in post-processing.
Modeling Dust Production, Growth, and Destruction in Reionization-Era Galaxies with the CROC Simulations II: Predicting the Dust Content of High-Redshift Galaxies · Dust scaling relations · 0.90
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An evolution in both the DTM and DTG ratios for metal-poor galaxies is also found, similar to that seen in GRB samples ( [ref] ; [ref] ).
The cosmic build-up of dust and metals. Accurate abundances from GRB-selected star-forming galaxies at $1.7 < z < 6.3$ · Dust scaling relations · 0.89
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