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REVIEW 2 major objections 5 minor 300 references

Local NLD and PSF parameter uncertainties, not model choice, dominate p-process abundance errors and are driven mainly by nearby photoneutron reactions.

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2026-07-13 04:40 UTC pith:BXM64AXE

load-bearing objection Solid BFMC extension to the p-process: parameter-driven (γ,n) uncertainties dominate (~0.7 dex), with an actionable local-driver list; the main soft spot is the 30 keV MACS filter transferred to GK photodisintegration rates. the 2 major comments →

arxiv 2607.09208 v1 pith:BXM64AXE submitted 2026-07-10 nucl-th astro-ph.SRnucl-ex

The impact of nuclear uncertainties on the p-process nucleosynthesis in Supernovae

S. Martinet , S. Goriely , A. Choplin This is my paper
classification nucl-th astro-ph.SRnucl-ex
keywords p-processnuclear level densitiesphoton strength functionsphotodisintegration ratessupernova nucleosynthesisHauser-FeshbachMonte Carlo uncertaintyneutron-deficient nuclei
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper sets out to quantify how uncertainties in nuclear level densities and photon strength functions affect the production of the 35 rare, neutron-deficient p-nuclei in type-Ia and type-II supernovae. Using a backward-forward Monte Carlo filter that keeps only parameter sets consistent with measured capture rates, then propagating the surviving extremes through full network calculations for three representative explosion models, the authors find that the abundance bands are typically about 0.7 dex wide (roughly a factor of five). These bands are almost entirely controlled by the neutron-capture and photoneutron channels; proton and alpha channels contribute little once the same nuclear inputs are shared. When modern microscopic models are compared, the correlated model-to-model spread is far smaller than the residual local parameter freedom still allowed by existing data. A statistical driver analysis further shows that, for many p-nuclei, the uncertainty is set by the photoneutron emission of the p-nucleus itself or of a neighbour on the same isotopic chain. Because a large fraction of those key reactions involve stable or near-stable targets, the work argues that better laboratory constraints on precisely those reactions would shrink the theoretical uncertainty more effectively than further model refinement alone.

Core claim

Uncorrelated local variations of NLD and PSF parameters that remain compatible with present experimental constraints dominate the p-process abundance uncertainty budget (typical span ~0.7 dex), overwhelmingly through photoneutron rates; for a large fraction of the p-nuclei the controlling reactions are the photoneutron emission of the p-nucleus itself or a nearby (γ,n) reaction on the same isotopic chain, many of which involve stable or near-stable nuclei.

What carries the argument

Backward-forward Monte Carlo (BFMC) filtering of NLD and PSF parameters against measured Maxwellian-averaged cross sections, followed by correlated propagation of the retained extreme rate sets through p-process networks and a SHAP-based main-effect / interaction decomposition that isolates core-driver reactions.

Load-bearing premise

The parameter sets kept by the low-energy capture-rate filter are assumed to adequately bound the high-temperature photodisintegration rates of neutron-deficient nuclei once detailed balance is applied.

What would settle it

Direct or inverse photoneutron measurements (or Oslo-method constraints on the relevant NLD and PSF) for a short list of the identified core-driver reactions on stable or near-stable targets that demonstrably shrink the Monte-Carlo abundance bands for the corresponding p-nuclei below the reported factor-of-five span.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 5 minor

Summary. The manuscript quantifies how nuclear level density (NLD) and photon strength function (PSF) uncertainties affect p-process yields in three supernova models (W7 SNIa, 25 M☉ solar-metallicity CCSN, and a rotating low-metallicity 25 M☉ model). Using TALYS with HFB+combinatorial NLDs and D1M+QRPA PSFs, the authors apply a Backward–Forward Monte Carlo (BFMC) filter that retains only parameter sets consistent with experimental MACS, then propagate correlated extreme (n,γ)/(p,γ)/(α,γ) rates (and their photodisintegration inverses) through full networks. They find that uncorrelated local parameter uncertainties dominate over modern model-to-model systematics, producing a typical abundance span of ~0.7 dex (factor ~5), overwhelmingly through (γ,n) channels. A multi-window ElasticNet–Random-Forest–SHAP analysis identifies core drivers that, for many p-nuclides, are the photoneutron emission of the p-nucleus itself or a nearby (γ,n) on the same isotopic chain; many of these involve stable or near-stable targets.

Significance. If the results hold, the work supplies a concrete, experimentally actionable prioritization for reducing p-process nuclear uncertainties: photoneutron rates on stable/near-stable nuclei and their immediate isotopic neighbours control a large fraction of the abundance budget. The combination of BFMC-constrained extrema, channel-isolation tests (Fig. 3), model-versus-parameter comparison (Fig. 4), multi-window robustness (Appendix B), and tabulated effect sizes (Tables C.1–C.2) is a clear methodological advance over earlier sensitivity studies and is of direct interest to both nuclear experimentalists and nucleosynthesis modellers. The interactive nuclear-chart maps further increase the paper’s utility.

major comments (2)
  1. The load-bearing transfer assumption (Secs. 2.1–2.2, 3.2) is that BFMC parameter sets filtered against experimental MACS (largely ~30 keV, reused from the authors’ prior i-process study) adequately bound stellar photodisintegration rates at p-process temperatures (1.7–3.3 GK) for neutron-deficient nuclei. High-T rates weight different regions of the PSF/NLD than the low-energy capture data; the manuscript should quantify residual temperature-transfer uncertainty (e.g., by comparing BFMC bands against any available higher-energy capture or photoneutron data, or by a controlled variation of the high-energy PSF tail) and state explicitly how this residual affects the reported 0.7 dex abundance spans and the driver lists in Tables C.1–C.2.
  2. Optical-model potential (OMP) uncertainties for protons and alphas are deferred (Sec. 2). While Fig. 3 and Appendix A show that NLD/PSF variations alone leave (p,γ) and (α,γ) rates almost unchanged on the proton-rich side, the claim that photoneutron uncertainties “strongly dominate the overall uncertainty budget” (abstract, Sec. 5) is strictly valid only within the NLD/PSF sector. A short quantitative estimate or literature bound on the missing OMP contribution is needed so that the dominance statement is not over-read as covering all nuclear-physics uncertainties.
minor comments (5)
  1. Fig. 1 caption and colour bar: clarify that the ratio is evaluated at a representative temperature (or state the temperature range) so that the map can be compared with the stellar rates used later.
  2. Sec. 3.2: the choice N=30 Monte-Carlo realisations is justified by a prior convergence study; a one-sentence reminder of that test (or a short appendix plot) would help the reader.
  3. Appendix B: the SHAP core-driver thresholds (M_i ≥ 0.8 and I_i ≥ 0.8) are stated but not motivated; a brief sensitivity check or reference to standard practice would strengthen the classification.
  4. Tables C.1–C.2 are dense; an online interactive version is already provided—mentioning the URL more prominently in the main text would improve accessibility.
  5. A few typographical slips remain (e.g., “the the p-process”, inconsistent spacing around × and GK). A careful proof-read is recommended.

Circularity Check

0 steps flagged

No load-bearing circularity: BFMC filters against external MACS, abundances and SHAP drivers are forward-propagated responses, not fitted to solar p-abundances or defined by the target result.

full rationale

The derivation chain is self-contained against external experimental benchmarks. NLD/PSF parameters are sampled and retained only if they reproduce measured MACS (reused from the authors’ prior i-process BFMC study but constrained by independent laboratory data, not by p-process yields). Extreme correlated rate sets are then forward-propagated through independent SN network calculations; the resulting abundance spreads and SHAP main/interaction decompositions are responses of those networks, not quantities fitted to solar p-abundances or defined in terms of the drivers. Model-to-model comparisons use published alternative NLD/PSF combinations and show smaller spread than the BFMC parameter band. Self-citations (BFMC method, D1M+QRPA/HFB models) are methodological reuse of tools previously applied to a different process; they do not import a uniqueness theorem or force the abundance-uncertainty or driver conclusions by construction. No self-definitional loop, no fitted-input-called-prediction, and no renaming of a known empirical pattern as a first-principles result is present. Minor residual risk is only the ordinary reuse of the same nuclear-model family for both rate generation and systematic comparison, which does not reduce the central claims to their inputs.

Axiom & Free-Parameter Ledger

6 free parameters · 6 axioms · 0 invented entities

The central claim rests on standard Hauser–Feshbach/detailed-balance nuclear reaction theory, a small set of local NLD/PSF scale parameters constrained by capture data, and three published supernova trajectories. No new physical entities are postulated; ‘core drivers’ is a statistical label. Free parameters are the four local nuclear knobs varied inside BFMC bounds, not abundance-fit constants.

free parameters (6)
  • NLD scale α (HFB+combinatorial)
    Local multiplicative scale of the level density; varied jointly with other knobs and retained only when MACS constraints are met (Sec. 2).
  • NLD energy shift δ
    Local excitation-energy shift in the NLD spectrum; same BFMC filtering as α (Sec. 2).
  • PSF centroid multiplier δE (D1M+QRPA)
    Multiplicative shift of GDR centroid energy; constrained by experimental systematics via BFMC (Sec. 2).
  • PSF width multiplier δΓ
    Multiplicative GDR width factor; co-varied and filtered with δE (Sec. 2).
  • Monte Carlo ensemble size N=30 min/max rate combinations
    Number of random extreme-rate realizations used for abundance bands; justified by prior convergence study rather than re-derived here (Sec. 3.2).
  • SHAP core-driver thresholds (M_i≥0.8 and I_i≥0.8)
    Classification cut defining ‘core drivers’ in normalized main-effect vs interaction plane (Appendix B.5); analysis choice affecting which rates enter the priority list.
axioms (6)
  • domain assumption Hauser–Feshbach statistical model with TALYS is adequate for the radiative capture and inverse photodisintegration rates of interest.
    All rates are computed in TALYS under this framework (Sec. 2); no direct validation for every neutron-deficient target.
  • domain assumption Photodisintegration rates follow from capture rates via detailed balance.
    Stated explicitly as the link from (n,γ)/(p,γ)/(α,γ) to (γ,n)/(γ,p)/(γ,α) (Introduction and Sec. 2).
  • ad hoc to paper BFMC-filtered parameter sets that reproduce experimental MACS remain valid uncertainty bounds for unmeasured proton-rich nuclei at p-process temperatures.
    Core of the uncertainty method; reuses filtered sets from Martinet et al. 2024 (Sec. 2.1).
  • ad hoc to paper Channels sharing a nucleus share one NLD/PSF parameter set (correlated), while different nuclei are independent.
    Propagation design in Sec. 2.2 and 3.2; controls how extrema are combined across the network.
  • domain assumption W7 SNIa and the two 25 M⊙ CCSN trajectories adequately sample p-process thermodynamic conditions for uncertainty ranking.
    Site selection in Sec. 3.1; results are compared across sites but not a full multi-D explosion suite.
  • ad hoc to paper Optical-model potential uncertainties for protons and alphas can be postponed without changing the dominance conclusion for NLD/PSF-driven errors.
    Explicitly deferred to future work (Sec. 2); authors argue NLD/PSF impact on (p,γ)/(α,γ) is already small on the proton-rich side.

pith-pipeline@v1.1.0-grok45 · 32885 in / 3669 out tokens · 48952 ms · 2026-07-13T04:40:03.314233+00:00 · methodology

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read the original abstract

The p-process is responsible for the production of the stable neutron-deficient nuclei heavier than iron observed in the solar system. However, important nuclear uncertainties still limit our understanding of this nucleosynthesis process. Among the most significant are the nuclear level densities (NLDs) and photon strength functions (PSFs) entering the calculation of photodisintegration rates under supernova conditions. We investigate both model (systematic) and parameter (statistical) uncertainties affecting NLDs and PSFs and quantify their impact on p-process nucleosynthesis in type-Ia and type-II supernovae. Correlated model uncertainties are estimated using several NLD and PSF models that reproduce available experimental observables. Uncorrelated parameter uncertainties are evaluated with a backward-forward Monte Carlo approach, in which parameter variations are constrained by measured reaction rates before being propagated to unknown cross sections of neutron-deficient nuclei. The resulting uncertainties are propagated through p-process calculations while preserving model correlations. To identify the reactions driving abundance uncertainties, we combine regularized linear-response modeling, stability analysis, and contribution and interaction decompositions. We find that photoneutron-emission uncertainties dominate the overall uncertainty budget. The leading source of uncertainty arises from local parameter variations still compatible with current experimental constraints, highlighting the lack of constraining nuclear data in the neutron-deficient region. For many p-nuclei, the dominant contribution originates either from the photoneutron emission of the p-nucleus itself or from a nearby $(\gamma,n)$ reaction along the same isotopic chain. While improved nuclear models remain important, many key reactions involve stable or near-stable nuclei and should be experimentally accessible.

Figures

Figures reproduced from arXiv: 2607.09208 by A. Choplin, S. Goriely, S. Martinet.

Figure 1
Figure 1. Figure 1: Representation in the (N,Z) plane of the nuclear parameter uncertainties on the (n, γ) reaction rates for the p-process. The color-code depicts the ratio between the maximum and minimum rate obtained for each nuclei with the BFMC method 10 1 10 0 10 1 10 2 10 3 X/Xsol W7 M25z14 M25z01S4 74Se 78Kr 84Sr 92Mo 94Mo 96Ru 98Ru 102Pd 106Cd 108Cd 113 In 112Sn 114Sn 115Sn 120Te 124Xe 126Xe 130Ba 132Ba 138La 136Ce 1… view at source ↗
Figure 2
Figure 2. Figure 2: Final p-nuclide abundances obtained for the three astrophysical sites considered in this work: the W7 Type Ia supernova model, a 25 M⊙ massive star at solar metallicity, and a rotating 25 M⊙ model at low metallicity. The shaded regions represent the abundance uncertainty ranges resulting from the propagation of nuclear parameter uncertainties. the same nucleus while still exploring the broader uncer￾tainty… view at source ↗
Figure 3
Figure 3. Figure 3: Final abundance uncertainty in the W7 model with all three channels correlated and with each isolated channels 10 1 10 0 10 1 10 2 X/Xsol D1M+QRPA & HFB+comb (Model A) SMLO & HFB+comb RMF+cQRPA & HFB+comb BSk27+QRPA & HFB+comb D1M+QRPA & THFB+comb D1M+QRPA & Cst-T D1M+QRPA & BSFG Parameter uncertainties from Model A 74Se 78Kr 84Sr 92Mo 94Mo 96Ru 98Ru 102Pd 106Cd 108Cd 113 In 112Sn 114Sn 115Sn 120Te 124Xe 1… view at source ↗
Figure 4
Figure 4. Figure 4: Comparison between statistical (parameter) and systematic (model) uncertainties for (n, γ) reaction rates relevant to the p-process in the M25z01S4 model. The shaded region corresponds to the parameter uncertainty band obtained with the BFMC approach for the reference model A (D1M+QRPA & HFB+comb). The colored lines represent the rates predicted by different combinations of PSF and NLD models. the adopted … view at source ↗
Figure 5
Figure 5. Figure 5: Distribution of all reaction rates in the normalized SHAP main-effect (Mi) versus interaction-strength (Ii) plane. The main effect quantifies the average direct contribution of a reaction rate to the abundance variation, while the interaction strength measures its contribution through coupled effects with other reaction rates. The thresholds used to define the Core Driver, High Main, High Interaction, and … view at source ↗
Figure 6
Figure 6. Figure 6: Zoomed view of the core-driver representation in the (N, Z) plane for three light p-nuclides in the W7 model: 74Se, 78Kr, and 84Sr. Colored squares mark the p-nuclides, while circles indicate the photodisintegration reactions identified as core drivers of their abundance uncertainties. Each driver is connected to the p-nucleus whose abundance it affects, and the sign along the connection indicates whether … view at source ↗
Figure 7
Figure 7. Figure 7: Same graphical representation as in [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Same graphical representation as in [PITH_FULL_IMAGE:figures/full_fig_p012_8.png] view at source ↗

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