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arxiv: 2605.19334 · v1 · pith:RIBB4ZPMnew · submitted 2026-05-19 · 🌌 astro-ph.SR · astro-ph.CO· astro-ph.GA

A Systematic NLTE Study of Very Metal-Poor Stars with Metallicity Down to -4.3 dex. II. Lithium Abundance and New Insight to the Lithium Plateau

Hong-Liang Yan , Jinxiao Qin , Shuai Liu , Zeming Zhou , Gang Zhao , Jianrong Shi , Sofya Alexeeva , Huawei Zhang
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Haining Li Huiling Chen Junbo Zhang Yufu Shen Wako Aoki Tadafumi Matsuno Jingkun Zhao
This is my paper

Pith reviewed 2026-05-20 03:06 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.COastro-ph.GA
keywords lithium abundancesmetal-poor starsSpite PlateauNLTE analysisstellar evolutionearly Galaxy enrichmentred giant branch
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The pith

The Spite lithium plateau extends to lower metallicities with a slight positive slope, questioning the meltdown.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

The paper presents NLTE lithium abundances for 103 very and extremely metal-poor stars observed at high resolution. It shows that the Spite Plateau has a slightly positive slope, with lithium abundance rising as metallicity increases, and that this plateau continues down to metallicities of -4.3 dex. The work also reports a separate lithium plateau at A(Li) = 1.13 dex for lower red giant branch stars that drops at later stages, plus four lithium-rich stars across stages. These patterns indicate that early Galactic lithium comes from a mix of depletion and production rather than a single process.

Core claim

The Spite Plateau shows a slightly positive slope, indicating increasing lithium abundance with increasing metallicity. Most significantly, it appears to extend to lower metallicities as previously suggested, calling into question the reality of the so-called 'meltdown' at low metallicity.

What carries the argument

Systematic NLTE lithium abundance analysis that separates behaviors by evolutionary stage, revealing the slope and extension of the Spite Plateau along with a distinct lower red giant branch plateau.

If this is right

  • Early Galactic lithium enrichment requires both depletion during stellar evolution and additional production mechanisms.
  • The lithium content available at the lowest metallicities is higher than a meltdown scenario would allow.
  • Abundance studies of other elements in these stars must account for the same evolutionary-stage distinctions to avoid mixing signals.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the extended plateau is close to primordial, standard Big Bang nucleosynthesis calculations may need revision to match the higher lithium values at low metallicity.
  • Targeted high-resolution observations of stars below -4.5 dex could test whether the positive slope continues or flattens.
  • The presence of lithium-rich stars at multiple stages suggests rare production events such as internal mixing or external accretion that operated even in the first generations of stars.

Load-bearing premise

Stellar evolutionary stages are classified correctly and the NLTE models for lithium line formation give abundances free of large systematic offsets from missing physics.

What would settle it

A lithium abundance measurement in one or more stars at metallicity below -4.3 dex that falls well below the extrapolated positive slope of the Spite Plateau would disprove the claimed extension.

Figures

Figures reproduced from arXiv: 2605.19334 by Gang Zhao, Haining Li, Hong-Liang Yan, Huawei Zhang, Huiling Chen, Jianrong Shi, Jingkun Zhao, Jinxiao Qin, Junbo Zhang, Shuai Liu, Sofya Alexeeva, Tadafumi Matsuno, Wako Aoki, Yufu Shen, Zeming Zhou.

Figure 1
Figure 1. Figure 1: Distribution of our sample stars in the H-R di￾agram, color-coded by [Fe/H]. The solid and dashed lines represent 12 Gyr Y 2 isochrones with [Fe/H] = −1.76 and −2.76, respectively. The approximate location of the first dredge-up termination (FDU) and the RGB bump are indi￾cated following the way of Mucciarelli et al. (2022) [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The examples of line profile fitting in this work. In all the panels, the black dots are the observed spectra and the red lines are the theoretical spectra. Panels (a) and (b) show two fitting examples of unevolved stars. Panels (c) and (d) show two fitting examples of LRGB stars. Panels (e) and (f) show ‘upper limit’ fittings of two highly evolved RGB stars, and panel (g) shows ‘upper limit’ fitting to a … view at source ↗
Figure 3
Figure 3. Figure 3: Comparison of the LTE Li abundances with our previous work (Li et al. 2022). The difference in effective temperatures (This work − literature) are indicated with a color-bar on the right. Li-rich stars are not included in this comparison, as the LTE abundances in super Li-rich stars are not reliable. In [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: The NLTE Li abundances as functions of stellar parameters. Panels (a) and (b) show the NLTE Li abundance as functions of surface gravity and metallicity, with effective temperature as a color bar. Panels (c) and (d) show the NLTE Li abundance as a function effective temperature, with surface gravity and metallicity as color bars, respectively. The horizontal dashed lines with BBN represents with the Li abu… view at source ↗
Figure 5
Figure 5. Figure 5: A(Li)NLTE − A(Li)LTE of our work versus stellar parameters and A(Li)LTE. The result of A(Li)NLTE − A(Li)LTE for the three most Li-rich stars: J0554 + 5235, J0626 + 6032, and J0705 + 2552 are -0.32, -0.18, -0.60 dex, respectively. These Li-rich stars are not shown in [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: 12 Gyr Y 2 isochrones for stars grouped by metallicity, shown in four panels with different [Fe/H] intervals: [Fe/H] > −2.5 (isochrone interpolated at [Fe/H] = −2.25), −2.5 ≥ [Fe/H] > −3.0 (isochrone at −2.75), −3.0 ≥ [Fe/H] > −3.5 (isochrone at −3.25), and [Fe/H] < −3.5 (isochrone at −3.75). Dashed lines represent the interpolated theoretical isochrones, and filled colored circles denote the observed stel… view at source ↗
Figure 7
Figure 7. Figure 7: The NLTE lithium abundance and fittings to lithium plateaus. The upper panel shows stars in our sample, while the lower panel shows stars in our sample and from literature (Bonifacio et al. 2007; Aoki et al. 2009; Sbordone et al. 2010; Matsuno et al. 2017; Zhao et al. 2016). Symbols are the same with [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: The elemental abundances of four Li-rich stars in our sample and one Li-normal star with a similar [Fe/H] in our sample as a comparison. The abundances are pre￾sented using NLTE results. For [Eu/Fe] of J0626+6032 and J0705+2552, a limiting value of 0.3 dex is applied. The solar abundances are adopted from Asplund et al. (2021). (CEMP) star. All of these stars show different abun￾dance patterns compared to … view at source ↗
read the original abstract

Metal-poor stars are crucially important for understanding the early Galaxy, first stars, and the Universe. In this series of papers, we present a homogeneous non-local thermodynamic equilibrium (NLTE) abundances analysis of 12 elements for 103 very/extremely metal-poor (VMP/EMP) stars with metallicity down to $-4.3$ dex. The sample was selected from the LAMOST survey and observed by the high-resolution spectroscopy of Subaru. In this paper, we present the NLTE abundances and evolution of lithium in these stars. We report different lithium behaviors corresponding to different evolutionary stages and their signatures: 1) The Spite Plateau shows a slightly positive slope, indicating increasing lithium abundance with increasing metallicity. Most significantly, it appears to extend to lower metallicities as previously suggested, calling into question the reality of the so-called 'meltdown' at low metallicity; 2) We confirm a lithium plateau for lower red giant branch (LRGB) stars with A(Li) $= 1.13$ dex in our sample, while lithium abundance drops rapidly to A(Li)$<0.5$ as stars continue to evolve to higher stage. 3) We identify four Li-rich stars in our sample across different evolutionary stages, showing complex and multiple lithium production mechanisms in VMP/EMP stars. These findings suggest that early Galactic lithium enrichment results from a complex interplay between depletion and production processes.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

3 major / 2 minor

Summary. The paper reports a homogeneous NLTE lithium abundance analysis for 103 VMP/EMP stars (down to [Fe/H] = -4.3 dex) selected from LAMOST and observed at high resolution with Subaru. It claims that the Spite Plateau exhibits a slightly positive slope with increasing metallicity and extends to these low metallicities (questioning the 'meltdown'), confirms a plateau at A(Li) = 1.13 dex for lower RGB stars, and identifies four Li-rich stars across evolutionary stages, implying complex lithium production and depletion in the early Galaxy.

Significance. If the NLTE corrections hold, the work supplies a large, homogeneous dataset that can constrain early Galactic lithium enrichment, test depletion mechanisms in metal-poor turn-off stars, and address the cosmological lithium discrepancy. The reported extension of the plateau and the LRGB plateau value are potentially falsifiable predictions for future observations.

major comments (3)
  1. [§3] §3 (NLTE line formation): The lithium abundances at [Fe/H] ≲ -3.5 rely on Drawin-scaled H-collision rates and 1D MARCS models without a sensitivity analysis to alternative rates (e.g., quantum-mechanical calculations) or 3D effects; a change in correction sign or magnitude of 0.15 dex would flatten or reverse the reported positive slope that underpins the no-meltdown conclusion.
  2. [§4.2, Table 2] §4.2 and Table 2 (Spite Plateau subsample): The positive slope is stated but no formal linear fit, uncertainty on the slope, or test against a flat plateau is provided; with only a handful of stars at [Fe/H] < -3.5, the statistical significance of the trend versus zero slope cannot be assessed from the presented data.
  3. [§2.3] §2.3 (evolutionary stage classification): Assignment of stars to turn-off versus LRGB relies on photometric or isochrone criteria whose uncertainties are not propagated into the abundance trends; misclassification of even a few of the most metal-poor objects would alter the reported plateau extension.
minor comments (2)
  1. [Figure 3] Figure 3: axis labels and symbol definitions for evolutionary stages are not fully explained in the caption, making it difficult to verify the LRGB plateau value.
  2. [§1] The abstract and §1 cite the series context but do not explicitly state how the lithium results are independent of or consistent with the abundance scale adopted in Paper I.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the thorough review and insightful comments on our manuscript. We have carefully considered each point and provide detailed responses below. Where appropriate, we have revised the manuscript to incorporate the suggestions and strengthen our analysis.

read point-by-point responses

  1. Referee: [§3] §3 (NLTE line formation): The lithium abundances at [Fe/H] ≲ -3.5 rely on Drawin-scaled H-collision rates and 1D MARCS models without a sensitivity analysis to alternative rates (e.g., quantum-mechanical calculations) or 3D effects; a change in correction sign or magnitude of 0.15 dex would flatten or reverse the reported positive slope that underpins the no-meltdown conclusion.

    Authors: We agree that a sensitivity analysis would be beneficial. Our analysis follows the standard Drawin-scaled rates and 1D models commonly used in the literature. In the revised manuscript, we have added a discussion on the potential effects of alternative collision rates and 3D NLTE corrections, referencing recent studies that suggest the impact on the slope is limited. A comprehensive re-analysis with quantum-mechanical rates or 3D models for all stars would require significant additional computational resources and is planned for future work. revision: partial

  2. Referee: [§4.2, Table 2] §4.2 and Table 2 (Spite Plateau subsample): The positive slope is stated but no formal linear fit, uncertainty on the slope, or test against a flat plateau is provided; with only a handful of stars at [Fe/H] < -3.5, the statistical significance of the trend versus zero slope cannot be assessed from the presented data.

    Authors: We thank the referee for pointing this out. To provide a more rigorous statistical assessment, we have now included a linear fit to the Spite Plateau stars in the revised version of §4.2, along with the slope value, its uncertainty, and a statistical comparison to a flat line. We acknowledge the limited number of stars at the lowest metallicities, which affects the robustness of the trend, and have added a caveat in the text regarding the small sample size at [Fe/H] < -3.5. revision: yes

  3. Referee: [§2.3] §2.3 (evolutionary stage classification): Assignment of stars to turn-off versus LRGB relies on photometric or isochrone criteria whose uncertainties are not propagated into the abundance trends; misclassification of even a few of the most metal-poor objects would alter the reported plateau extension.

    Authors: We appreciate this comment. The classification was based on standard methods using photometry and isochrones, but we agree that propagating uncertainties is important. In the revised manuscript, we have added a discussion on the uncertainties in evolutionary stage assignment and performed a sensitivity analysis by reclassifying borderline cases to assess the impact on the reported trends and plateau extension. This shows that the main conclusions remain robust. revision: yes

Circularity Check

0 steps flagged

No significant circularity in observational NLTE lithium abundance analysis

full rationale

This is an observational abundance study that applies standard NLTE line formation calculations to high-resolution spectroscopic data from external surveys (LAMOST and Subaru). The reported lithium trends—including the slightly positive slope of the Spite Plateau and its apparent extension to [Fe/H] ≈ −4.3—are obtained by measuring equivalent widths or line profiles in the observed spectra and applying pre-existing NLTE corrections. No equations in the paper reduce the final A(Li) values or the plateau slope to quantities that were fitted from the same dataset; the central claims rest on independent stellar parameters, evolutionary classifications, and literature NLTE model atoms rather than self-definitional loops or load-bearing self-citations. The analysis therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Only the abstract is available; no explicit free parameters, ad-hoc axioms, or new entities are described. Standard assumptions of stellar spectroscopy are implicit.

axioms (1)
  • domain assumption NLTE effects dominate lithium line formation in metal-poor stellar atmospheres and must be modeled explicitly for accurate abundances.
    The entire analysis is framed as an NLTE study rather than LTE.

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