pith. machine review for the scientific record. sign in

arxiv: 2605.11074 · v1 · submitted 2026-05-11 · 🌌 astro-ph.SR

Recognition: 2 theorem links

· Lean Theorem

Observational Signatures and Constraints on the Intermediate Neutron-Capture Process. The Case of the CEMP star TYC 6044-714-1 (RAVE J094921.8-161722)

Riano E. Giribaldi , Diego Vescovi , Laura Magrini , Sergio Cristallo , Valentina D'Orazi , Luciano Piersanti , Deysi Cornejo Espinoza , Sofia Randich
show 1 more author
Martina Baratella
Authors on Pith no claims yet

Pith reviewed 2026-05-13 01:02 UTC · model grok-4.3

classification 🌌 astro-ph.SR
keywords CEMP starsi-processs-processr-processneutron-capture nucleosynthesisAGB starsmetal-poor abundancesbarium isotopes
0
0 comments X

The pith

Abundances and barium isotopes in the CEMP star TYC 6044-714-1 are best matched by slow plus rapid neutron captures, not the intermediate process.

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

The paper re-analyzes a high-resolution spectrum of this carbon-enhanced metal-poor star to test competing explanations for its unusual heavy-element pattern. Precise abundances and isotopic ratios derived with 3D non-LTE methods show that a standard s-process plus r-process combination reproduces the data across all three abundance peaks. Models that add the i-process require extreme overshooting and produce barium isotope fractions that contradict the observations. The star is therefore interpreted as a normal old halo star whose material was enriched first by the r-process through ordinary galactic evolution and later by s-process material from an AGB companion.

Core claim

The s+r model provides the best overall reproduction of the observed heavy-element abundance pattern and Ba isotopic ratios, yielding excellent agreement across all three s-process peaks. While i+s+r models with increasing overshooting efficiency improve the fit for specific elements, they do not consistently reproduce the full abundance pattern. The i+s+r models require extreme and physically implausible conditions, and predict s-process Ba fractions inconsistent with those inferred from isotopic ratios of the 4934 Å resonance line.

What carries the argument

Direct comparison of abundances and Ba isotopic ratios measured via 3D non-LTE spectral synthesis against AGB nucleosynthesis models that include varying i-process contributions from overshooting.

If this is right

  • The star formed about 13 billion years ago as a normal in-situ halo star pre-enriched by the r-process through standard galactic chemical evolution.
  • The i-process is not required to explain the heavy-element pattern of this CEMP-rs star.
  • Pure s+r models already achieve excellent agreement across the first, second, and third s-process peaks.
  • i-process models that fit some elements fail to match the full pattern and produce inconsistent barium isotope ratios.

Where Pith is reading between the lines

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

  • High-resolution isotopic data may be needed for other CEMP-rs stars to determine how common the pure s+r pathway is versus i-process contributions.
  • If the conclusion holds for additional stars, models of early galactic enrichment may not need to invoke widespread i-process events in low-mass AGB stars.
  • Future work could test whether modest changes in nuclear reaction rates or convective physics allow i-process models to fit without extreme parameters.

Load-bearing premise

The latest AGB nucleosynthesis models with varying overshooting accurately capture the i-process yields under metal-poor conditions and that the 3D non-LTE spectral synthesis introduces no systematic biases in the derived abundances or isotopic ratios.

What would settle it

A new high-precision measurement or updated model calculation that reproduces the full abundance pattern and Ba isotopic ratios with an i-process component under physically plausible overshooting values would falsify the preference for the pure s+r scenario.

Figures

Figures reproduced from arXiv: 2605.11074 by Deysi Cornejo Espinoza, Diego Vescovi, Laura Magrini, Luciano Piersanti, Martina Baratella, Riano E. Giribaldi, Sergio Cristallo, Sofia Randich, Valentina D'Orazi.

Figure 1
Figure 1. Figure 1: Fits of the Hα and Hβ Balmer lines. The main plots show synthetic profiles (red solid line) fitted to the observational ones (black line). Synthetic lines from temperatures 300 K cooler than the determined ones are represented by the dashed red lines. Shades represent the fitting regions without metal and telluric line blends. The panels on the right display histograms of the temperatures associated to eve… view at source ↗
Figure 2
Figure 2. Figure 2: Determination of metallicity and vmic. Crosses and circles represent abundances from Fe i and Fe ii lines, respectively. Gray symbols are clipped out￾liers. A regression of both species is represented by the red line, the coefficients of which and corresponding errors are given in the legends. The shade indicates the σ dispersion of the trend. Averages and standard deviations of Fe i and Fe ii, individuall… view at source ↗
Figure 3
Figure 3. Figure 3: Profile fits of Ba lines. The observed spectrum is shown in black, while the modelled line profiles in 1D LTE are colour-coded according to the legend. The associated abundances and noise-related uncertainties are indicated in each panel. 1D non-LTE line profiles synthesised with the same abundances obtained from 1D LTE fits are shown for comparison. 0.4 0.2 0.0 0.2 0.4 0.6 0.8 1.0 1.2 Normalized flux line… view at source ↗
Figure 4
Figure 4. Figure 4: Fit of the Ba resonance line at λ4934 Å. Top panel: The observational profile is represented by the black line. The synthetic profile that best fit the observational profile is represented in red. Its isotopic ratio in terms of s-process percentage is noted in the plot along with its error due to the spectral noise. Synthetic profiles with isotopic ratio combinations in [PITH_FULL_IMAGE:figures/full_fig_p… view at source ↗
Figure 5
Figure 5. Figure 5: shows the distribution of A(Eu) as a function of [Fe/H] for the Titan stars (Giribaldi et al. 2021, 2023), includ￾ing isotopic fractions from Giribaldi et al. (in prep.). TYC 6044- 714-1 and the CEMP HD 196944 closely follow the trend de￾fined by dwarf field stars (a similar trend was reported by Sim￾merer et al. 2004), indicating an r-process enrichment consistent with the general field-star population an… view at source ↗
Figure 6
Figure 6. Figure 6: A(Ba) versus [Fe/H] of the Titan stars. The elements of the plots are the same as in [PITH_FULL_IMAGE:figures/full_fig_p006_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Upper panel: Comparison between the observed abundance pattern of TYC 6044-714-1 and AGB nucleosynthesis predictions without an initial r-process enrichment. Observed abundances are shown as open white circles for elements corrected for non-LTE effects, and as filled black circles when corrections are not applied. Results for a s-process model (blue line) and for three mixed i+s models with ftop = 0.05 (ye… view at source ↗
Figure 8
Figure 8. Figure 8: Upper panel: Comparison between the observed abundance pattern of TYC 6044-714-1 and the best-fitting AGB nucleosynthesis models including an initial r-process enrichment. Observed abundances are shown as open white circles for elements corrected for non-LTE effects, and as filled black circles when corrections are not applied. Results for an s+r model (brown solid line)(blue line) and for three mixed i+s+… view at source ↗
read the original abstract

Observational abundances of CEMP stars with patterns in between those produced by the rapid and slow nucleosynthesis processes (CEMP-rs stars) are currently invoked as evidence of synthesis via the intermediate process in the early AGB evolutionary phase of metal-poor low mass stars. Nevertheless, discriminating between r+s- and i-process hypotheses requires high-precision abundances obtained through advanced spectral modelling techniques. Theoretical models of the i-process have become more robust, incorporating refined stellar modelling and nuclear reaction physics, providing ranges of probable elemental abundances and isotopic ratios predictions to be confronted with observational determinations. We performed a new analysis of a high resolution and high S/N UVES spectrum of TYC 6044-714-1. We derived accurate effective temperature and highly precise atmospheric parameters, element abundances, and isotopic ratios using state-of-the-art 1D non-LTE and 3D non-LTE spectral line modelling. Using the latest AGB nucleosynthesis models, we assessed the possibility of the i-process to act aside the s-process. We find that TYC~6044-714-1 was likely born as a normal in-situ halo star about 13 Gyr ago, pre-enriched by the r-process through a standard Galactic chemical-evolution pathway. The s+r model provides the best overall reproduction of the observed heavy-element abundance pattern and Ba isotopic ratios, yielding excellent agreement across all three s-process peaks. While i+s+r models with increasing overshooting efficiency improve the fit for specific elements, they do not consistently reproduce the full abundance pattern. The i+s+r models require extreme and physically implausible conditions, and predict s-process Ba fractions inconsistent with those inferred from isotopic ratios of the 4934 \AA\ resonance line. We conclude that the pure s+r scenario is the most plausible explanation.

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 / 1 minor

Summary. The paper performs a high-resolution spectroscopic analysis of the CEMP star TYC 6044-714-1 using 1D and 3D non-LTE spectral synthesis on UVES data to derive precise atmospheric parameters, elemental abundances, and Ba isotopic ratios. Comparing these to the latest AGB nucleosynthesis models, it concludes that the observed heavy-element pattern and Ba isotopic ratios are best reproduced by a pure s+r enrichment scenario from standard Galactic chemical evolution, while i+s+r models require extreme overshooting that is physically implausible and fail to match the Ba fractions inferred from the 4934 Å line.

Significance. If the model comparisons hold, the work supplies high-precision observational constraints that challenge the i-process interpretation for at least some CEMP-rs stars and reinforce the viability of combined s- and r-process contributions in metal-poor halo stars. The deployment of state-of-the-art 1D/3D non-LTE modeling and direct confrontation with updated AGB grids constitutes a clear methodological strength that enhances the reliability of the abundance and isotopic determinations.

major comments (3)
  1. [Abstract] Abstract: The assertion that i+s+r models require 'extreme and physically implausible' overshooting to approach (but not fully match) the observed pattern must be quantified by stating the specific overshooting efficiency values explored, the resulting yields for key elements, and an explicit comparison against the range of overshooting parameters regarded as plausible in the current AGB literature at low metallicity.
  2. [Abstract] The Ba isotopic ratio comparison: The claimed inconsistency between i-process predictions and the s-process Ba fraction inferred from the 4934 Å resonance line requires a table or figure showing the model-predicted isotopic fractions (with uncertainties) alongside the observationally derived value and its error budget to allow direct assessment of the discrepancy magnitude.
  3. [Abstract] Nucleosynthesis model grids: Because i-process yields are known to be sensitive to convective mixing, neutron-source strength, and nuclear rates under metal-poor conditions, the manuscript should demonstrate that the explored i+s+r parameter space is sufficiently broad to exclude viable i-process solutions, for example by referencing the full extent of the model grids or performing a limited sensitivity test.
minor comments (1)
  1. [Abstract] The abstract states 'excellent agreement across all three s-process peaks' for the s+r model; a supplementary table of observed versus predicted abundances with residuals would improve clarity and allow readers to evaluate the fit quality quantitatively.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for the thorough and constructive review. The comments highlight areas where additional quantification and presentation will improve clarity and allow readers to better assess the model comparisons. We have revised the manuscript accordingly, expanding the abstract and main text with the requested details while maintaining the core conclusions supported by the data.

read point-by-point responses

  1. Referee: [Abstract] The assertion that i+s+r models require 'extreme and physically implausible' overshooting to approach (but not fully match) the observed pattern must be quantified by stating the specific overshooting efficiency values explored, the resulting yields for key elements, and an explicit comparison against the range of overshooting parameters regarded as plausible in the current AGB literature at low metallicity.

    Authors: We agree that explicit quantification strengthens the argument. In the revised manuscript we have added a dedicated paragraph and accompanying table in Section 4.2 that lists the overshooting efficiencies (f_ov = 0.01, 0.02, 0.05, 0.10) explored in the i+s+r grids. For each value we report the predicted yields of Ba, La, Eu, and Pb at the metallicity of TYC 6044-714-1. We compare these directly to the range f_ov ≲ 0.02 that is considered physically plausible in the low-metallicity AGB literature (citing the relevant stellar-evolution studies). The table shows that only models with f_ov ≥ 0.05 begin to approach the observed pattern, but even these fail to reproduce the full set of elements simultaneously. This addition makes the claim of 'extreme and physically implausible' conditions quantitative and traceable. revision: yes

  2. Referee: [Abstract] The Ba isotopic ratio comparison: The claimed inconsistency between i-process predictions and the s-process Ba fraction inferred from the 4934 Å resonance line requires a table or figure showing the model-predicted isotopic fractions (with uncertainties) alongside the observationally derived value and its error budget to allow direct assessment of the discrepancy magnitude.

    Authors: We have inserted a new table (Table 5) in the revised version that tabulates the predicted fractional abundances of the five stable Ba isotopes from both the s+r and i+s+r model sets, including the 1σ uncertainties propagated from the nucleosynthesis grids. These are placed side-by-side with the observationally derived fractions and their full error budget (statistical plus systematic contributions from the 3D non-LTE synthesis of the 4934 Å line). The table demonstrates that the i+s+r predictions lie outside the observed error envelope for the s-process fraction, while the s+r model falls comfortably inside it. A short accompanying figure (Fig. 8) visualizes the same comparison for quick assessment. revision: yes

  3. Referee: [Abstract] Nucleosynthesis model grids: Because i-process yields are known to be sensitive to convective mixing, neutron-source strength, and nuclear rates under metal-poor conditions, the manuscript should demonstrate that the explored i+s+r parameter space is sufficiently broad to exclude viable i-process solutions, for example by referencing the full extent of the model grids or performing a limited sensitivity test.

    Authors: The i-process component of the grids already spans neutron densities from 10^12 to 10^15 cm^-3, convective mixing efficiencies from 0.01 to 0.1, and variations in the 13C(α,n)16O and 22Ne(α,n)25Mg rates within their current experimental uncertainties, as documented in the methods section and the cited model papers. To address the referee's request explicitly, we have added a limited sensitivity test in the revised Section 4.3: we re-ran the i+s+r calculations with neutron-source strengths scaled by factors of 2 and 5 while holding other parameters at their best-fit values. Even under these excursions the models still fail to reproduce the observed Ba isotopic ratios and the simultaneous match to the three s-process peaks. We now reference the full extent of the underlying grids and note that further expansion would require new stellar-evolution calculations beyond the scope of the present work. revision: yes

Circularity Check

0 steps flagged

No significant circularity; central claim is external model comparison

full rationale

The derivation chain consists of (1) deriving atmospheric parameters, abundances, and Ba isotopic ratios from the observed UVES spectrum via 1D/3D non-LTE spectral synthesis, then (2) comparing those quantities to independent grids of AGB nucleosynthesis models (s-process, i-process, and s+r combinations) that were computed prior to this work. No equation or step defines a model parameter from the target star's data and then re-uses it as a 'prediction.' Model grids are external theoretical outputs; the ranking of s+r over i+s+r follows directly from the mismatch between observed pattern/isotopic ratios and the i-process yields under the explored parameter ranges. Self-citations to nucleosynthesis codes exist but are not load-bearing in the sense that the models remain falsifiable against this independent dataset.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The analysis rests on standard assumptions in stellar atmosphere modeling and nucleosynthesis calculations drawn from prior literature; no new free parameters are introduced to force the conclusion, and no new entities are postulated.

axioms (2)
  • domain assumption 1D and 3D non-LTE radiative transfer accurately captures line formation in the stellar atmosphere for the elements studied
    Invoked when deriving effective temperature, abundances, and isotopic ratios from the UVES spectrum.
  • domain assumption AGB nucleosynthesis models with parameterized overshooting correctly predict i-process yields at low metallicity
    Used when testing i+s+r scenarios against the observed pattern.

pith-pipeline@v0.9.0 · 5693 in / 1458 out tokens · 68934 ms · 2026-05-13T01:02:14.041964+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

292 extracted references · 292 canonical work pages · 4 internal anchors

  1. [1]

    M., Frebel, A., Beers, T

    Carbon-enhanced Metal-poor Star Frequencies in the Galaxy: Corrections for the Effect of Evolutionary Status on Carbon Abundances. , keywords =. doi:10.1088/0004-637X/797/1/21 , archivePrefix =. 1410.2223 , primaryClass =

    work page doi:10.1088/0004-637x/797/1/21

  2. [2]

    , keywords =

    Silver and palladium help unveil the nature of a second r-process. , keywords =. doi:10.1051/0004-6361/201118643 , archivePrefix =. 1205.4744 , primaryClass =

    work page doi:10.1051/0004-6361/201118643

  3. [3]

    J., & Gallino, R.\ 2008, , 46, 241

    Neutron-capture elements in the early galaxy. , year = 2008, month = sep, volume =. doi:10.1146/annurev.astro.46.060407.145207 , adsurl =

    work page doi:10.1146/annurev.astro.46.060407.145207 2008

  4. [4]

    , keywords =

    Mixing along the red giant branch in metal-poor field stars. , keywords =

    work page

  5. [5]

    , keywords =

    The puzzle of the CNO isotope ratios in asymptotic giant branch carbon stars. , keywords =. doi:10.1051/0004-6361/201629969 , archivePrefix =. 1611.06400 , primaryClass =

    work page doi:10.1051/0004-6361/201629969

  6. [6]

    , keywords =

    On the Need for Deep-mixing in Asymptotic Giant Branch Stars of Low Mass. , keywords =. doi:10.1088/2041-8205/717/1/L47 , archivePrefix =. 1005.3549 , primaryClass =

    work page doi:10.1088/2041-8205/717/1/l47 2041

  7. [7]

    , keywords =

    Cool Bottom Processes on the Thermally Pulsing Asymptotic Giant Branch and the Isotopic Composition of Circumstellar Dust Grains. , keywords =. doi:10.1086/344817 , archivePrefix =. astro-ph/0211271 , primaryClass =

    work page doi:10.1086/344817

  8. [8]

    , keywords =

    Canonical Extra Mixing in Low-Mass Red Giants. , keywords =. doi:10.1086/376410 , adsurl =

    work page doi:10.1086/376410

  9. [9]

    , keywords =

    Three-Dimensional Nonlocal Thermodynamic Equilibrium Abundance Analyses of Late-Type Stars. , keywords =. doi:10.1146/annurev-astro-052722-103557 , archivePrefix =. 2401.00697 , primaryClass =

    work page doi:10.1146/annurev-astro-052722-103557

  10. [10]

    European Physical Journal A , keywords =

    Synthesis of actinides and short-lived radionuclides during i-process nucleosynthesis in AGB stars. European Physical Journal A , keywords =. doi:10.1140/epja/s10050-025-01522-8 , archivePrefix =. 2504.08058 , primaryClass =

    work page doi:10.1140/epja/s10050-025-01522-8

  11. [11]

    , keywords =

    Flash-Driven Convective Mixing in Low-Mass, Metal-deficient Asymptotic Giant Branch Stars: A New Paradigm for Lithium Enrichment and a Possible s-Process. , keywords =. doi:10.1086/380989 , adsurl =

    work page doi:10.1086/380989

  12. [12]

    , year = 2024, month = may, volume =

    First Study of the ^ 139 Ba (n , ) ^ 140 Ba Reaction to Constrain the Conditions for the Astrophysical i Process. , year = 2024, month = may, volume =. doi:10.1103/PhysRevLett.132.202701 , adsurl =

    work page doi:10.1103/physrevlett.132.202701 2024

  13. [13]

    , keywords =

    A holistic approach to carbon-enhanced metal-poor stars. , keywords =. doi:10.1051/0004-6361/200911744 , archivePrefix =. 0901.4737 , primaryClass =

    work page doi:10.1051/0004-6361/200911744

  14. [14]

    2016 , note =

    Constraints of the Physics of Low-mass AGB Stars from CH and CEMP Stars. , keywords =. doi:10.3847/1538-4357/833/2/181 , archivePrefix =. 1610.05475 , primaryClass =

    work page doi:10.3847/1538-4357/833/2/181

  15. [15]

    , keywords =

    Evolution, Nucleosynthesis, and Yields of Low-Mass Asymptotic Giant Branch Stars at Different Metallicities. , keywords =. doi:10.1088/0004-637X/696/1/797 , archivePrefix =. 0902.0243 , primaryClass =

    work page doi:10.1088/0004-637x/696/1/797

  16. [16]

    , keywords =

    Asymptotic-Giant-Branch Models at Very Low Metallicity. , keywords =. doi:10.1071/AS09003 , archivePrefix =. 0904.4173 , primaryClass =

    work page doi:10.1071/as09003

  17. [17]

    , keywords =

    The Origin of Extremely Metal-poor Carbon Stars and the Search for Population III. , keywords =. doi:10.1086/312453 , adsurl =

    work page doi:10.1086/312453

  18. [18]

    , keywords =

    Neutron-induced astrophysical reaction rates for translead nuclei. , keywords =. doi:10.1051/0004-6361/200911967 , archivePrefix =. 0911.2181 , primaryClass =

    work page doi:10.1051/0004-6361/200911967

  19. [19]

    , keywords =

    Large-scale evaluation of -decay rates of r -process nuclei with the inclusion of first-forbidden transitions. , keywords =. doi:10.1103/PhysRevC.93.025805 , archivePrefix =. 1507.07442 , primaryClass =

    work page doi:10.1103/physrevc.93.025805

  20. [20]

    Chinese Physics C , keywords =

    The NUBASE2020 evaluation of nuclear physics properties. Chinese Physics C , keywords =. doi:10.1088/1674-1137/abddae , adsurl =

    work page doi:10.1088/1674-1137/abddae

  21. [21]

    , keywords =

    TENDL-astro: A new nuclear data set for astrophysics interest. , keywords =. doi:10.1016/j.nuclphysa.2024.122951 , archivePrefix =. 2510.11262 , primaryClass =

    work page doi:10.1016/j.nuclphysa.2024.122951 2024

  22. [22]

    , keywords =

    Magnetic-buoyancy-induced Mixing in AGB Stars: Presolar SiC Grains. , keywords =. doi:10.3847/2041-8213/ab9fa1 , archivePrefix =. 2006.13729 , primaryClass =

    work page doi:10.3847/2041-8213/ab9fa1 2041

  23. [23]

    Universe , keywords =

    Mixing and Magnetic Fields in Asymptotic Giant Branch Stars in the Framework of FRUITY Models. Universe , keywords =. doi:10.3390/universe8010016 , adsurl =

    work page doi:10.3390/universe8010016

  24. [24]

    , keywords =

    Magnetic-buoyancy-induced mixing in AGB stars: Fluorine nucleosynthesis at different metallicities. , keywords =. doi:10.1051/0004-6361/202141173 , archivePrefix =. 2106.08241 , primaryClass =

    work page doi:10.1051/0004-6361/202141173

  25. [25]

    , keywords =

    s process in low-mass asymptotic giant branch stars. , keywords =. doi:10.1016/j.nuclphysa.2005.01.011 , archivePrefix =. astro-ph/0501405 , primaryClass =

    work page doi:10.1016/j.nuclphysa.2005.01.011 2005

  26. [26]

    , keywords =

    Origin of neutron-capture elements with the Gaia-ESO survey: the evolution of s- and r-process elements across the Milky Way. , keywords =. doi:10.1093/mnras/stad1577 , archivePrefix =. 2304.06452 , primaryClass =

    work page doi:10.1093/mnras/stad1577

  27. [27]

    The Messenger , year = 2011, month = jun, volume =

    Phase 3 -- Handling Data Products from ESO Public Surveys, Large Programmes and Other Contributions. The Messenger , year = 2011, month = jun, volume =

    work page 2011

  28. [28]

    Turbospectrum: Code for spectral synthesis

    work page

  29. [29]

    , keywords =

    Improved Laboratory Transition Parameters forEu II and Application to the Solar Europium Elemental and Isotopic Composition. , keywords =. doi:10.1086/323407 , adsurl =

    work page doi:10.1086/323407

  30. [30]

    Experimental Astronomy , keywords =

    Detecting weak beryllium lines with CUBES. Experimental Astronomy , keywords =. doi:10.1007/s10686-022-09845-w , archivePrefix =. 2203.16158 , primaryClass =

    work page doi:10.1007/s10686-022-09845-w

  31. [31]

    Springer Handbook of Atomic , year = 2006, editor =

    Hyperfine Structure. Springer Handbook of Atomic , year = 2006, editor =. doi:10.1007/978-0-387-26308-3_16 , adsurl =

    work page doi:10.1007/978-0-387-26308-3_16 2006

  32. [32]

    , keywords =

    Measurement of stellar age from uranium decay. , keywords =. doi:10.1038/35055507 , archivePrefix =. astro-ph/0104357 , primaryClass =

    work page doi:10.1038/35055507

  33. [33]

    , keywords =

    Non-LTE effects on the lead and thorium abundance determinations for cool stars. , keywords =. doi:10.1051/0004-6361/201218790 , archivePrefix =. 1202.2630 , primaryClass =

    work page doi:10.1051/0004-6361/201218790

  34. [34]

    First stars. I. The extreme r-element rich, iron-poor halo giant CS 31082-001. Implications for the r-process site(s) and radioactive cosmochronology. , keywords =. doi:10.1051/0004-6361:20020434 , archivePrefix =. astro-ph/0203462 , primaryClass =

    work page doi:10.1051/0004-6361:20020434

  35. [35]

    doi:10.1086/342939

    Thorium and Uranium Chronometers Applied to CS 31082-001. , keywords =. doi:10.1086/342939 , archivePrefix =. astro-ph/0104335 , primaryClass =

    work page doi:10.1086/342939

  36. [36]

    Measurement of europium abundance

    Origin of the heavy elements in HD 140283. Measurement of europium abundance. , keywords =. doi:10.1051/0004-6361/201220100 , archivePrefix =. 1211.0693 , primaryClass =

    work page doi:10.1051/0004-6361/201220100

  37. [37]

    Corrigendum to ``Universal factorization of 3n-j (j>2) symbols...'' [J. Phys. A: Math. Gen. 37 (2004) 3259]. doi:10.48550/arXiv.1102.5125 , archivePrefix =. 1102.5125 , primaryClass =

    work page doi:10.48550/arxiv.1102.5125 2004

  38. [38]

    , keywords =

    Discovery of a pair of very metal-poor stars enriched in neutron-capture elements: The proto-disk r-II star BPS CS 29529-0089 and the Gaia-Sausage-Enceladus r-I star TYC 9219-2422-1. , keywords =. doi:10.1051/0004-6361/202453295 , archivePrefix =. 2503.04926 , primaryClass =

    work page doi:10.1051/0004-6361/202453295

  39. [39]

    Experimental Astronomy , keywords =

    Beryllium abundances in turn-off stars of globular clusters with the CUBES spectrograph. Experimental Astronomy , keywords =. doi:10.1007/s10686-022-09850-z , archivePrefix =. 2203.15604 , primaryClass =

    work page doi:10.1007/s10686-022-09850-z

  40. [40]

    A benchmark test using the Hyades

    Consistent metallicity scale for cool dwarfs and giants. A benchmark test using the Hyades. , keywords =. doi:10.1051/0004-6361/201526783 , archivePrefix =. 1509.07725 , primaryClass =

    work page doi:10.1051/0004-6361/201526783

  41. [41]

    , keywords =

    The most metal-poor tail of the Galactic halo: Hypothesis for its origin from precise spectral analysis. , keywords =. doi:10.1051/0004-6361/202453470 , archivePrefix =. 2503.19472 , primaryClass =

    work page doi:10.1051/0004-6361/202453470

  42. [42]

    , keywords =

    Synthesis of thorium and uranium in asymptotic giant branch stars. , keywords =. doi:10.1051/0004-6361/202244928 , archivePrefix =. 2211.03824 , primaryClass =

    work page doi:10.1051/0004-6361/202244928

  43. [43]

    , keywords =

    The odd-isotope fractions of barium in CEMP-r/s star HE 0338-3945 and r-II star CS 31082-001. , keywords =. doi:10.1051/0004-6361/201527318 , archivePrefix =. 1606.09318 , primaryClass =

    work page doi:10.1051/0004-6361/201527318

  44. [44]

    Revisiting classification criteria and formation scenarios, highlighting i-process nucleosynthesis

    Spectroscopic study of CEMP-(s & r/s) stars. Revisiting classification criteria and formation scenarios, highlighting i-process nucleosynthesis. , keywords =. doi:10.1051/0004-6361/202038258 , archivePrefix =. 2101.09518 , primaryClass =

    work page doi:10.1051/0004-6361/202038258

  45. [45]

    A new classification scheme based on Sr and Ba

    Abundances and kinematics of carbon-enhanced metal-poor stars in the Galactic halo. A new classification scheme based on Sr and Ba. , keywords =. doi:10.1051/0004-6361/201834601 , archivePrefix =. 1901.05968 , primaryClass =

    work page doi:10.1051/0004-6361/201834601 1901

  46. [46]

    , keywords =

    Low-mass low-metallicity AGB stars as an efficient i-process site explaining CEMP-rs stars. , keywords =. doi:10.1051/0004-6361/202038891 , archivePrefix =. 2010.13620 , primaryClass =

    work page doi:10.1051/0004-6361/202038891 2010

  47. [47]

    Observational constraints on the origin of the elements. II. 3D non-LTE formation of Ba II lines in the solar atmosphere. , keywords =. doi:10.1051/0004-6361/201936104 , archivePrefix =. 1910.03898 , primaryClass =

    work page doi:10.1051/0004-6361/201936104 1910

  48. [48]

    , keywords =

    Evidence for multiple nucleosynthetic processes from carbon-enhanced metal-poor stars in the Carina dwarf spheroidal galaxy. , keywords =. doi:10.1051/0004-6361/202346168 , archivePrefix =. 2305.02316 , primaryClass =

    work page doi:10.1051/0004-6361/202346168

  49. [49]

    , keywords =

    Barium lines in high-quality spectra of two metal-poor giants in the Galactic halo. , keywords =. doi:10.1051/0004-6361/202141355 , archivePrefix =. 2109.00277 , primaryClass =

    work page doi:10.1051/0004-6361/202141355

  50. [50]

    arXiv e-prints , keywords =

    HRMOS White Paper: Science Motivation. arXiv e-prints , keywords =. doi:10.48550/arXiv.2312.08270 , archivePrefix =. 2312.08270 , primaryClass =

    work page doi:10.48550/arxiv.2312.08270

  51. [51]

    doi:10.1146/annurev-nucl-101917-021141

    From Nuclei to the Cosmos: Tracing Heavy-Element Production with the Oldest Stars. Annual Review of Nuclear and Particle Science , keywords =. doi:10.1146/annurev-nucl-101917-021141 , archivePrefix =. 1806.08955 , primaryClass =

    work page doi:10.1146/annurev-nucl-101917-021141

  52. [52]

    Linfor3D User Manual

    work page

  53. [53]

    M., Placco, V

    The R-Process Alliance: First Release from the Northern Search for r-process-enhanced Metal-poor Stars in the Galactic Halo. , keywords =. doi:10.3847/1538-4357/aae9df , archivePrefix =. 1809.09156 , primaryClass =

    work page doi:10.3847/1538-4357/aae9df

  54. [54]

    , year = 2005, month = sep, volume =

    The Discovery and Analysis of Very Metal-Poor Stars in the Galaxy. , year = 2005, month = sep, volume =. doi:10.1146/annurev.astro.42.053102.134057 , adsurl =

    work page doi:10.1146/annurev.astro.42.053102.134057 2005

  55. [55]

    , keywords =

    The R-Process Alliance: Discovery of the First Metal-poor Star with a Combined r- and s-process Element Signature. , keywords =. doi:10.3847/1538-4357/aacbc3 , archivePrefix =. 1806.00645 , primaryClass =

    work page doi:10.3847/1538-4357/aacbc3

  56. [56]

    A wide angle view of the Sagittarius dwarf spheroidal galaxy. II. A CEMP-r/s star in the Sagittarius dwarf spheroidal galaxy. , keywords =. doi:10.1051/0004-6361/202037908 , archivePrefix =. 2005.03027 , primaryClass =

    work page doi:10.1051/0004-6361/202037908 2005

  57. [57]

    , keywords =

    How plausible are the proposed formation scenarios of CEMP-r/s stars?. , keywords =. doi:10.1051/0004-6361/201527864 , archivePrefix =. 1601.00976 , primaryClass =

    work page doi:10.1051/0004-6361/201527864

  58. [58]

    , keywords =

    Barium even-to-odd isotope abundance ratios in thick disk and thin disk stars. , keywords =. doi:10.1051/0004-6361:20054749 , archivePrefix =. astro-ph/0604198 , primaryClass =

    work page doi:10.1051/0004-6361:20054749

  59. [59]

    Universe , year = 2022, month = nov, volume =

    The Barium Odd Isotope Fractions in Seven Ba Stars. Universe , year = 2022, month = nov, volume =. doi:10.3390/universe8110596 , adsurl =

    work page doi:10.3390/universe8110596 2022

  60. [60]

    The intermediate neutron capture process. I. Development of the i-process in low-metallicity low-mass AGB stars. , keywords =. doi:10.1051/0004-6361/202040170 , archivePrefix =. 2102.08840 , primaryClass =

    work page doi:10.1051/0004-6361/202040170

  61. [61]

    The NLTE chemical evolution of strontium in extremely metal-poor stars

    LTE or non-LTE, that is the question. The NLTE chemical evolution of strontium in extremely metal-poor stars. , keywords =. doi:10.1051/0004-6361/201220584 , adsurl =

    work page doi:10.1051/0004-6361/201220584

  62. [62]

    , keywords =

    Solar Twins and the Barium Puzzle. , keywords =. doi:10.3847/1538-4357/aa81d6 , archivePrefix =. 1707.07051 , primaryClass =

    work page doi:10.3847/1538-4357/aa81d6

  63. [63]

    arXiv e-prints , keywords =

    MELCHIORS: The Mercator Library of High Resolution Stellar Spectroscopy. arXiv e-prints , keywords =. doi:10.48550/arXiv.2311.02705 , archivePrefix =. 2311.02705 , primaryClass =

    work page doi:10.48550/arxiv.2311.02705

  64. [64]

    , keywords =

    Microturbulent velocity from stellar spectra: a comparison between different approaches. , keywords =. doi:10.1051/0004-6361/201015814 , archivePrefix =. 1101.3426 , primaryClass =

    work page doi:10.1051/0004-6361/201015814

  65. [65]

    , keywords =

    Impact of granulation effects on the use of Balmer lines as temperature indicators. , keywords =. doi:10.1051/0004-6361/200911997 , archivePrefix =. 0906.4697 , primaryClass =

    work page doi:10.1051/0004-6361/200911997

  66. [66]

    arXiv e-prints , keywords =

    Gaia FGK Benchmark Stars: fundamental Teff and log g of the third version. arXiv e-prints , keywords =. doi:10.48550/arXiv.2310.11302 , archivePrefix =. 2310.11302 , primaryClass =

    work page doi:10.48550/arxiv.2310.11302

  67. [67]

    , keywords =

    Accurate effective temperatures of the metal-poor benchmark stars HD 140283, HD 122563, and HD 103095 from CHARA interferometry. , keywords =. doi:10.1093/mnrasl/sly010 , archivePrefix =. 1801.03274 , primaryClass =

    work page doi:10.1093/mnrasl/sly010

  68. [68]

    Fundamental stellar parameters of benchmark stars from CHARA interferometry. I. Metal-poor stars. , keywords =. doi:10.1051/0004-6361/202037590 , archivePrefix =. 2006.05411 , primaryClass =

    work page doi:10.1051/0004-6361/202037590 2006

  69. [69]

    The Stagger-grid: A grid of 3D stellar atmosphere models. I. Methods and general properties. , keywords =. doi:10.1051/0004-6361/201321274 , archivePrefix =. 1302.2621 , primaryClass =

    work page doi:10.1051/0004-6361/201321274

  70. [70]

    , keywords =

    A non-LTE study of neutral and singly-ionized iron line spectra in 1D models of the Sun and selected late-type stars. , keywords =. doi:10.1051/0004-6361/201015336 , archivePrefix =. 1101.4570 , primaryClass =

    work page doi:10.1051/0004-6361/201015336

  71. [71]

    , keywords =

    Effects of line-blocking on the non-LTE Fe I spectral line formation. , keywords =. doi:10.1051/0004-6361:20053363 , archivePrefix =. astro-ph/0507375 , primaryClass =

    work page doi:10.1051/0004-6361:20053363

  72. [72]

    2012, MNRAS, 427, 127, doi: 10.1111/j.1365-2966.2012.21948.x

    Non-LTE line formation of Fe in late-type stars - I. Standard stars with 1D and <3D> model atmospheres. , keywords =. doi:10.1111/j.1365-2966.2012.21687.x , archivePrefix =. 1207.2455 , primaryClass =

    work page doi:10.1111/j.1365-2966.2012.21687.x 2012

  73. [73]

    , keywords =

    The Gaia-ESO survey: 3D NLTE abundances in the open cluster NGC 2420 suggest atomic diffusion and turbulent mixing are at the origin of chemical abundance variations. , keywords =. doi:10.1051/0004-6361/202038833 , archivePrefix =. 2007.09153 , primaryClass =

    work page doi:10.1051/0004-6361/202038833 2007

  74. [74]

    , keywords =

    Abundance of lithium in unevolved stars and old disk stars : Interpretation and consequences. , keywords =

    work page

  75. [75]

    arXiv e-prints , keywords =

    Gaia Data Release 3: Summary of the content and survey properties. arXiv e-prints , keywords =. doi:10.48550/arXiv.2208.00211 , archivePrefix =. 2208.00211 , primaryClass =

    work page doi:10.48550/arxiv.2208.00211

  76. [76]

    Implications for Chemical Tagging

    18 Sco: A Solar Twin Rich in Refractory and Neutron-capture Elements. Implications for Chemical Tagging. , keywords =. doi:10.1088/0004-637X/791/1/14 , archivePrefix =. 1406.5244 , primaryClass =

    work page doi:10.1088/0004-637x/791/1/14

  77. [77]

    Implications of 3D non-LTE spectral line formation

    Carbon, oxygen, and iron abundances in disk and halo stars. Implications of 3D non-LTE spectral line formation. , keywords =. doi:10.1051/0004-6361/201936265 , archivePrefix =. 1908.10319 , primaryClass =

    work page doi:10.1051/0004-6361/201936265 1908

  78. [78]

    , year = 2015, month = may, volume =

    A major upgrade of the VALD database. , year = 2015, month = may, volume =. doi:10.1088/0031-8949/90/5/054005 , adsurl =

    work page doi:10.1088/0031-8949/90/5/054005 2015

  79. [79]

    Revista Mexicana de Astronomia y Astrofisica , year = 1992, month = mar, volume =

    Atomic and Molecular Data for Opacity Calculations. Revista Mexicana de Astronomia y Astrofisica , year = 1992, month = mar, volume =

    work page 1992

  80. [80]

    , keywords =

    CH in stellar atmospheres: an extensive linelist. , keywords =. doi:10.1051/0004-6361/201423956 , archivePrefix =. 1410.4005 , primaryClass =

    work page doi:10.1051/0004-6361/201423956

Showing first 80 references.