Astrophysics of Galaxies · arXiv:2404.08765 v1 · submitted 12 Apr 2024
Modeling the Galactic Chemical Evolution of Helium
The paper says
“Although our GCE models include many potentially complicating effects, the short enrichment time delay and mild metallicity dependence of the predicted yields makes the results quite simple: across a wide range of metallicity and age, the non-primordial 4He mass fraction ΔY = Y−YP is proportional to the abundance of promptly produced α-elements, like oxygen, with ΔY/ZO ≈ (yHeCC + yHeAGB)/yOCC.”
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Abstract
We examine the galactic chemical evolution (GCE) of 4He in one-zone and multi-zone models, with particular attention to theoretical predictions and empirical constraints on IMF-averaged yields. Published models of massive star winds and core collapse supernovae span a factor of 2 – 3 in the IMF-averaged 4He yield, yHeCC. Published models of intermediate mass, asymptotic giant branch (AGB) stars show better agreement on the IMF-averaged yield, yHeAGB, and they predict that more than half of this yield comes from stars with M = 4−8M⊙, making AGB 4He enrichment rapid compared to Fe enrichment from Type Ia supernovae. Although our GCE models include many potentially complicating effects, the short enrichment time delay and mild metallicity dependence of the predicted yields makes the results quite simple: across a wide range of metallicity and age, the non-primordial 4He mass fraction ΔY = Y−YP is proportional to the abundance of promptly produced α-elements, like oxygen, with ΔY/ZO ≈ (yHeCC + yHeAGB)/yOCC. Reproducing solar abundances with our fiducial choice of the oxygen yield yOCC = 0.0071 implies yHeCC + yHeAGB ≈ 0.022, i.e., 0.022M⊙ of net 4He production per solar mass of star formation. Our GCE models with this yield normalization are consistent with most available observations, though the implied yHeCC is low compared to most of the published massive star models. More precise measurements of ΔY in stars and gas across a wide range of metallicity and [α/Fe] ratio could test our models more stringently, either confirming the simple picture suggested by our calculations or revealing surprises in the evolution of the second most abundant element.
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abstract compiled · 2026-09-23 · no language-model review
How the main claim is stated: asserted 0.98
What the abstract itself states, as probabilities: claims first 0.03 · states limitation 0.93 · human participants 0.01 · controlled comparison 0.07 · randomized assignment 0.01 · states quantitative result 0.98 · compares with prior results 0.96 · mentions code or data availability 0.02
The abstract, sentence by sentence
This table labels the abstract only (arXiv listing abstract v1). The number is the probability the classifier gave the label.
| Sentence | Role | The authors' own work | States the main conclusion | Strength |
|---|---|---|---|---|
| We examine the galactic chemical evolution (GCE) of $^4$He in one-zone and multi-zone models, with particular attention to theoretical predictions and empirical constraints on IMF-averaged yields. | contribution 0.97 | 0.88 | 0.05 | asserted 0.74 |
| Published models of massive star winds and core collapse supernovae span a factor of 2 -- 3 in the IMF-averaged $^4$He yield, $y\mathrm{_{He}^{CC}}$. | background 0.96 | 0.04 | 0.03 | asserted 1.00 |
| Published models of intermediate mass, asymptotic giant branch (AGB) stars show better agreement on the IMF-averaged yield, $y\mathrm{_{He}^{AGB}}$, and they predict that more than half of this yield comes from stars with $M=4-8 M_\odot$, making AGB $^4$He enrichment rapid compared to Fe enrichment from Type Ia supernovae. | background 0.97 | 0.05 | 0.07 | asserted 1.00 |
| Although our GCE models include many potentially complicating effects, the short enrichment time delay and mild metallicity dependence of the predicted yields makes the results quite simple: across a wide range of metallicity and age, the non-primordial $^4$He mass fraction $\Delta Y = Y-Y_{\mathrm{P}}$ is proportional to the abundance of promptly produced $\alpha$-elements, like oxygen, with $\Delta Y/Z_{\mathrm{O}} \approx (y\mathrm{_{He}^{CC}}+y\mathrm{_{He}^{AGB}})/y\mathrm{_{O}^{CC}}$. | result 0.72 | 0.87 | 0.75 | asserted 0.98 |
| Reproducing solar abundances with our fiducial choice of the oxygen yield $y\mathrm{_{O}^{CC}}=0.0071$ implies $y\mathrm{_{He}^{CC}}+y\mathrm{_{He}^{AGB}} \approx 0.022$, i.e., $0.022M_\odot$ of net $^4$He production per solar mass of star formation. | result 0.99 | 0.89 | 0.15 | asserted 0.96 |
| Our GCE models with this yield normalization are consistent with most available observations, though the implied $y\mathrm{_{He}^{CC}}$ is low compared to most of the published massive star models. | result 0.56 | 0.91 | 0.14 | hedged possibility 0.81 |
| More precise measurements of $\Delta Y$ in stars and gas across a wide range of metallicity and [$\alpha$/Fe] ratio could test our models more stringently, either confirming the simple picture suggested by our calculations or revealing surprises in the evolution of the second most abundant element. | future work 1.00 | 0.11 | 0.08 | hedged possibility 1.00 |
What kind of paper the classifier reports this is: simulation study 0.70 · evidence from simulation or computation 0.97
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Compiled by classifier-1.13.0 via TypeSafe API, question bank abstract-p1-20260923, 2026-09-23: 1 request, 6,341 input tokens.
Every quoted sentence on this record is the authors'. Every label is from Pith's closed vocabulary, with the probability shown beside it. This record as JSON
How the literature uses it
5 arXiv papers cite this in 17 sentences
Papers citing it · 9 sentences without a confident label
Uses its data or values 2 papers
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In this paper, we construct galactic chemical evolution (GCE) models for $$ incorporating the [ref] ( [ref] , hereafter L11) stellar yields, with methods similar to those in our recent study of $$ evolution [ref] .
Constraints on the Galactic Chemical Evolution of $^3\rm{He}$ · Introduction · 0.84
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At this scale, $y_O,MS = Z_O,⊙ = 0.00572$ based on the [ref] measurements of the composition of the solar photosphere.[This is consistent with more recent measurements of the solar oxygen abundance [ref] .] We determine the massive star yield of by computing [ref] 's recommended total yield from their Equation 12, which ensures that the model reproduces the observed relationship between elemental helium and oxygen abundances.
Towards a measurement of the primordial helium isotope ratio · Galactic Chemical Evolution of $^3$He/$^4$He · 0.99
Compares with it 1 paper
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This behavior contrasts with that of other AGB elements we have previously examined such as Sr [ref] , N [ref] , or $$ [ref] , where production is dominated by higher mass stars with shorter lifetimes.
Constraints on the Galactic Chemical Evolution of $^3\rm{He}$ · Conclusions · 0.87
Cites it as background 1 paper
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Thus, the total helium abundance can be expressed as [equation] where $Δy$ depends on the stellar Initial Mass Function (IMF), star formation rate (SFR), gas mass, evolutionary time, and other factors (e.g. [ref] ).
Cosmic evolution of the helium and oxygen abundances in type 2 Active Galactic Nuclei: Helium-loud AGNs · Introduction · 0.84
What it cites · 7 sentences without a confident label
Uses data or values from 1 paper
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For our fiducial $$ = 0.023 [ref] and $= 0.973 ×$ = 0.0071 [ref] , we infer $y_He$ = 0.022, i.e., for every solar mass of stars formed, massive stars and AGB stars return an average of 0.022 of new helium, in addition to about 0.08 $(= 0.25r)$ returned by recycling of birth helium.
The Scale of Stellar Yields: Implications of the Measured Mean Iron Yield of Core Collapse Supernovae · Summary · 1.00
Cites as background 1 paper
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More recently, [ref] studied the enrichment of extremely metal-poor galaxies (EMPGs) and the first galaxies using hydrodynamical simulations, exploring He/H-O/H relations as well as Fe/O ratios.
Probing Chemical Enrichment in Extremely Metal-Poor Galaxies · Introduction · 0.93
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