Recognition: 2 theorem links
· Lean TheoremPrimordial deuterium abundance from calculations of p(n,γ) and d(p,γ) reactions within potential-model approach
Pith reviewed 2026-05-15 08:44 UTC · model grok-4.3
The pith
A single scaling factor applied consistently in the Malfliet-Tjon potential for both p(n,γ) and d(p,γ) reactions yields a primordial deuterium abundance of 2.479 × 10^{-5} that matches observations.
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
Core claim
Within a consistent two-body potential framework based on the Malfliet-Tjon interaction that includes both E1 and M1 contributions, a single scaling factor λ is fixed by the p(n,γ) reaction and propagated without readjustment to the d(p,γ) reaction, producing D/H = 2.479^{+0.350}_{-0.177} × 10^{-5} in agreement with values inferred from metal-poor damped Lyman-α systems; modest variations of λ produce sizable shifts in the predicted deuterium and other light-element abundances.
What carries the argument
The Malfliet-Tjon potential with one overall scaling factor λ that governs the low-energy scattering wave functions for both reactions.
If this is right
- The predicted D/H ratio changes noticeably when λ is varied within its allowed range.
- The same consistent framework supplies reaction rates for other light nuclei produced in the Big Bang.
- Agreement with observed deuterium supports the use of this potential-model approach for nucleosynthesis calculations.
- Small adjustments to low-energy scattering parameters can shift the entire set of primordial abundances.
Where Pith is reading between the lines
- If the single-λ propagation works here, the same technique could be tested on additional light-element reactions without new parameters.
- Tighter experimental bounds on λ would tighten predictions for both deuterium and lithium abundances.
- The method offers a way to check whether current nuclear-data uncertainties are the dominant source of spread in Big Bang abundance calculations.
Load-bearing premise
A single scaling factor constrained by the p(n,γ) reaction can be transferred unchanged to the d(p,γ) reaction inside the same potential model.
What would settle it
A direct measurement of the d(p,γ) cross section at Big Bang energies that lies outside the band obtained when the λ value fitted to p(n,γ) data is used without further adjustment.
Figures
read the original abstract
The $p(n,\gamma)$ and $d(p,\gamma)$ reactions are key nuclear inputs for Big Bang nucleosynthesis. In this work, both reactions are analyzed within a consistent two-body potential framework based on the Malfliet-Tjon interaction, including contributions from both $E1$ and $M1$ transitions. A single scaling factor $\lambda$ controlling the low-energy scattering dynamics is constrained by the $p(n,\gamma)$ and propagated consistently to the $d(p,\gamma)$. The obtained abundance, $\mathrm{D/H} = 2.479^{+0.350}_{-0.177}\times 10^{-5}$, is in good agreement with values inferred from metal-poor damped Lyman-$\alpha$ systems. The modest variations of $\lambda$ lead to a significant change in the predicted $\mathrm{D/H}$ ratio and light-element abundances.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The manuscript calculates the p(n,γ) and d(p,γ) radiative capture reactions within a consistent two-body potential-model framework based on the Malfliet-Tjon interaction, including both E1 and M1 transitions. A single scaling factor λ is constrained by p(n,γ) data and applied without further adjustment to the d(p,γ) channel. This procedure yields a primordial deuterium abundance D/H = 2.479^{+0.350}_{-0.177}×10^{-5}, reported to be in good agreement with values inferred from metal-poor damped Lyman-α systems. The work notes that modest changes in λ produce large variations in the predicted D/H ratio and light-element abundances.
Significance. If the transfer of λ is shown to be reliable, the calculation supplies a unified potential-model treatment of two key BBN reactions and produces a D/H value consistent with observation. This would constitute a useful cross-check on standard BBN inputs. The dependence on a single fitted parameter, however, reduces the independence of the prediction and makes the result sensitive to the validity of the underlying potential for the deuteron bound state.
major comments (1)
- The central D/H result rests on propagating a single scaling factor λ, fixed exclusively by p(n,γ) cross-section data, into the d(p,γ) calculation inside the same Malfliet-Tjon potential. Because the deuteron binding energy, asymptotic normalization constant, and low-energy wave functions are fixed by the potential, any mismatch after scaling directly alters the E1/M1 matrix elements at BBN energies. The abstract states that modest λ variations already produce large changes in D/H; therefore an unvalidated transfer of λ constitutes the dominant uncertainty in the claimed agreement with damped Lyman-α data.
minor comments (1)
- The abstract presents asymmetric uncertainties on D/H but does not specify how these are obtained from the λ variations or from other sources; a brief description of the error propagation would improve clarity.
Simulated Author's Rebuttal
We thank the referee for the careful review and constructive feedback on our manuscript. We address the major comment below and will incorporate revisions to clarify the uncertainties associated with our approach.
read point-by-point responses
-
Referee: The central D/H result rests on propagating a single scaling factor λ, fixed exclusively by p(n,γ) cross-section data, into the d(p,γ) calculation inside the same Malfliet-Tjon potential. Because the deuteron binding energy, asymptotic normalization constant, and low-energy wave functions are fixed by the potential, any mismatch after scaling directly alters the E1/M1 matrix elements at BBN energies. The abstract states that modest λ variations already produce large changes in D/H; therefore an unvalidated transfer of λ constitutes the dominant uncertainty in the claimed agreement with damped Lyman-α data.
Authors: We agree that transferring the scaling factor λ, determined from p(n,γ) data, to the d(p,γ) channel within the Malfliet-Tjon framework is central to our calculation and represents a significant source of uncertainty, as we already emphasize through the sensitivity analysis and the reported error bars on D/H. This transfer is performed for consistency within the same two-body potential model, where λ adjusts the low-energy scattering parameters to reproduce the relevant np data; the deuteron properties then follow directly from the scaled potential without additional tuning. We have propagated modest variations in λ into the final D/H uncertainty to reflect this sensitivity. To address the referee's concern, we will revise the manuscript by adding an expanded discussion section on the justification for this procedure, its limitations for the deuteron bound state, and how it affects the E1/M1 matrix elements at BBN energies. revision: partial
Circularity Check
λ fitted solely to p(n,γ) data is propagated to d(p,γ) to obtain D/H
specific steps
-
fitted input called prediction
[Abstract]
"A single scaling factor λ controlling the low-energy scattering dynamics is constrained by the p(n,γ) and propagated consistently to the d(p,γ). The obtained abundance, D/H = 2.479^{+0.350}_{-0.177}×10^{-5}, is in good agreement with values inferred from metal-poor damped Lyman-α systems."
λ is fixed by fitting to p(n,γ) data; the same λ is then inserted unchanged into the d(p,γ) matrix elements to produce the quoted D/H. The abundance therefore inherits its numerical value and error bars from the p(n,γ) fit by construction rather than from an independent calculation of the deuteron photodisintegration channel.
full rationale
The paper constrains a single scaling parameter λ from p(n,γ) cross-section data inside the Malfliet-Tjon potential and then applies the identical λ without further adjustment to compute the d(p,γ) rate that enters the BBN network. Because the final D/H value is obtained directly from this propagated rate, the reported abundance reduces to a quantity whose central value and uncertainty are fixed by the p(n,γ) fit rather than by an independent first-principles evaluation of both reactions. This matches the fitted-input-called-prediction pattern; the derivation chain is therefore partially circular at the level of the central result.
Axiom & Free-Parameter Ledger
free parameters (1)
- λ =
not numerically specified in abstract
axioms (1)
- domain assumption Malfliet-Tjon interaction provides an adequate two-body potential for these reactions at BBN energies
Lean theorems connected to this paper
-
IndisputableMonolith/Cost/FunctionalEquation.leanwashburn_uniqueness_aczel contradicts?
contradictsCONTRADICTS: the theorem conflicts with this paper passage, or marks a claim that would need revision before publication.
A single scaling factor λ controlling the low-energy scattering dynamics is constrained by the p(n, γ) and propagated consistently to the d(p, γ).
-
IndisputableMonolith/Foundation/AbsoluteFloorClosure.leanreality_from_one_distinction unclear?
unclearRelation between the paper passage and the cited Recognition theorem.
The MT potential parameters... yield a deuteron binding energy of Eb = −2.225 MeV.
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
-
[1]
Cooke R J, Pettini M and Steidel C C 2018 Astrophys. J. 855(2) 102
work page 2018
-
[2]
Cyburt R H, Fields B D, Olive K A and Yeh T H 2016 Rev. Mod. Phys. 88(1) 015004
work page 2016
-
[3]
Serpico P D, Esposito S, Iocco F, Mangano G, Miele G and Pisanti O 2004 J. Cosmol. Astropart. Phys. 2004(12) 010
work page 2004
-
[4]
Fields B D, Olive K A, Yeh T H and Young C 2020 J. Cosmol. Astropart. Phys. 2020(03) 010
work page 2020
-
[5]
Pisanti O, Mangano G, Miele G and Mazzella P 2021 J. Cosmol. Astropart. Phys. 2021(04) 020
work page 2021
-
[6]
(LUNA collaboration) 2002 Nucl
Casella C, Costantini H, Lemut A, Limata B, Bonetti R, Broggini C, Campajola L, Corvisiero P, Cruz J, D’Onofrio A et al. (LUNA collaboration) 2002 Nucl. Phys. A 706(1-2) 203
work page 2002
-
[7]
(LUNA collaboration) 2020 Nature 587(7833) 210
Mossa V, Stöckel K, Cavanna F, Ferraro F, Aliotta M, Barile F, Bemmerer D, Best A, Boeltzig A, Broggini C et al. (LUNA collaboration) 2020 Nature 587(7833) 210
work page 2020
-
[8]
Griffiths G M, Lal M and Scarfe C D 1963 Can. J. Phys. 41(5) 724
work page 1963
-
[9]
Warren J B, Erdman K L, Robertson L P, Axen D A and Macdonald J R 1963 Phys. Rev. 132(4) 1691
work page 1963
-
[10]
Bailey G M, Griffiths G M, Olivo M A and Helmer R L 1970 Can. J. Phys. 48(24) 3059
work page 1970
-
[11]
Schmid G J, Chasteler R M, Laymon C M, Weller H R, Prior R M and Tilley D R 1995 Phys. Rev. C 52(4) R1732
work page 1995
-
[12]
Ma L, Karwowski H J, Brune C R, Ayer Z, Black T C, Blackmon J C, Ludwig E J, Viviani M, Kievsky A and Schiavilla R 1997 Phys. Rev. C 55(2) 588
work page 1997
-
[13]
Bystritsky V M, Gazi S, Huran J, Dudkin G N, Krylov A R, Lysakov A S, Nechaev B A, Padalko V N, Sadovsky A B, Filipowicz M and Philippov A V 2015 Phys. Part. Nuclei Lett. 12(4) 550
work page 2015
-
[14]
Tišma I, Lipoglavšek M, Mihovilovič M, Markelj S, Vencelj M and Vesić J 2019 Eur. Phys. J. A 55(8) 137
work page 2019
-
[15]
Turkat S, Hammer S, Masha E, Akhmadaliev S, Bemmerer D, Grieger M, Hensel T, Julin J, Koppitz M, Ludwig F, Möckel C, Reinicke S, Schwengner R, Stöckel K, Szücs T, Wagner L and Zuber K 2021 Phys. Rev. C 103(4) 045805
work page 2021
-
[16]
Suzuki T S, Nagai Y, Shima T, Kikuchi T, Sato H, Kii T and Igashira M 1995 Astrophys. J. Lett. 439(2) L59
work page 1995
-
[17]
Nagai Y, Suzuki T S, Kikuchi T, Shima T, Kii T, Sato H and Igashira M 1997 Phys. Rev. C 56(6) 3173
work page 1997
-
[18]
Schreiber E C, Canon R S, Crowley B T, Howell C R, Kelley J H, Litvinenko V N, Nelson S O, Park S H, Pinayev I V, Prior R M, Sabourov K, Spraker M, Tornow W, Wu Y, Wulf E A and Weller H R 2000 Phys. Rev. C 61(6) 061604
work page 2000
-
[19]
Hara K Y, Utsunomiya H, Goko S, Akimune H, Yamagata T, Ohta M, Toyokawa H, Kudo K, Uritani A, Shibata Y, Lui Y W and Ohgaki H 2003 Phys. Rev. D 68(7) 072001
work page 2003
-
[20]
Moreh R, Kennett T J and Prestwich W V 1989 Phys. Rev. C 39(4) 1247
work page 1989
-
[21]
Tornow W, Czakon N G, Howell C R, Hutcheson A, Kelley J H, Litvinenko V N, Mikhailov S F, Pinayev I V, Weisel G J and Witała H 2003 Phys. Lett. B 574(1-2) 8 11 IOP Publishing Phys. Scr. vv (yyyy) aaaaaa N Le Anh et al
work page 2003
-
[22]
Chen Y J, Hao Z R, He J J, Kajino T, Ando S I, Luo Y, Feng H R, Zhang L Y, Fan G T, Wang H W, Zhang H, Shen Z L, Liu L X, Xu H H, Zhang Y, Jiao P, Li X Y, Yang Y X, Jin S, Chen K J, Shen W Q and Ma Y G 2026 Phys. Rev. Lett. 136(5) 052701
work page 2026
-
[23]
Carlson J and Schiavilla R 1998 Rev. Mod. Phys. 70(3) 743
work page 1998
- [24]
-
[25]
Ando S, Cyburt R H, Hong S W and Hyun C H 2006 Phys. Rev. C 74(2) 025809
work page 2006
-
[26]
Johnson A S and Hale G M 2001 Nucl. Phys. A 688(1-2) 566
work page 2001
-
[27]
Rupak G 2000 Nucl. Phys. A 678(4) 405
work page 2000
-
[28]
Beane S R, Chang E, Detmold W, Orginos K, Parreño A, Savage M J and Tiburzi B C (NPLQCD collaboration) 2015 Phys. Rev. Lett. 115(13) 132001
work page 2015
-
[29]
Acharya B and Bacca S 2022 Phys. Lett. B 827 137011
work page 2022
-
[30]
Marcucci L E, Nollett K M, Schiavilla R and Wiringa R B 2006 Nucl. Phys. A 777 111
work page 2006
-
[31]
Marcucci L E, Mangano G, Kievsky A and Viviani M 2016 Phys. Rev. Lett. 116(10) 102501
work page 2016
-
[32]
Moscoso J, de Souza R S, Coc A and Iliadis C 2021 Astrophys. J. 923(1) 49
work page 2021
- [33]
-
[34]
Dubovichenko S B and Dzhazairov-Kakhramanov A V 2009 Eur. Phys. J. A 39(2) 139
work page 2009
-
[35]
Dubovichenko S B, Chechin L M, Burkova N A, Dzhazairov-Kakhramanov A V, Omarov C T, Nurakhmetova S Z, Beisenov B U, Ertaiuly A and Eleusheva B 2020 Russ. Phys. J. 63(7) 1118
work page 2020
-
[36]
Le Anh N, Nhut Anh D, Huy Tho D and Huu Nha N 2024 Phys. Scr. 99(6) 065026
work page 2024
-
[37]
Malfliet R A and Tjon J A 1969 Nucl. Phys. A 127(1) 161
work page 1969
-
[38]
Malfliet R A and Tjon J A 1970 Ann. Phys. 61(2) 425
work page 1970
-
[39]
Awasthi S and Sastri O S K S 2024 Phys. At. Nucl. 87(3) 311
work page 2024
-
[40]
Pisanti O, Cirillo A, Esposito S, Iocco F, Mangano G, Miele G and Serpico P D 2008 Comput. Phys. Commun. 178(12) 956
work page 2008
-
[41]
Consiglio R, de Salas P, Mangano G, Miele G, Pastor S and Pisanti O 2018 Comput. Phys. Commun. 233 237
work page 2018
-
[42]
Gariazzo S, de Salas P F, Pisanti O and Consiglio R 2022 Comput. Phys. Commun. 271 108205
work page 2022
-
[43]
Le Anh N and Minh Loc B 2022 Phys. Rev. C 106(1) 014605
work page 2022
-
[44]
Olive K A 2014 Chin. Phys. C 38(9) 090001
work page 2014
-
[45]
Angulo C, Arnould M, Rayet M, Descouvemont P, Baye D, Leclercq-Willain C, Coc A, Barhoumi S, Aguer P, Rolfs C, Kunz R, Hammer J, Mayer A, Paradellis T, Kossionides S, Chronidou C, Spyrou K, Degl’Innocenti S, Fiorentini G, Ricci B, Zavatarelli S, Providencia C, Wolters H, Soares J, Grama C, Rahighi J, Shotter A and Lamehi Rachti M 1999 Nucl. Phys. A 656(1) 3
work page 1999
-
[46]
Acharya B, Aliotta M, Balantekin A B, Bemmerer D, Bertulani C A, Best A, Brune C R, Buompane R, Gialanella L, Cavanna F, Chen J W, Colgan J, Czarnecki A, Davids B, deBoer R J, Delahaye F, Depalo R, Guglielmetti A, García A, Robertson R G H, Gatu Johnson M, Gazit D, Greife U, Guffanti D, Hambleton K, Haxton W C, Herrera Y, Serenelli A, Huang M, Iliadis C, K...
work page 2025
-
[47]
Stoks V G J, Klomp R A M, Rentmeester M C M and de Swart J J 1993 Phys. Rev. C 48(2) 792
work page 1993
-
[48]
Blackston M A, Ahmed M W, Perdue B A, Weller H R, Bewer B, Pywell R E, Wurtz W A, Igarashi R, Kucuker S, Norum B, Wang K, Li J, Mikhailov S F, Popov V G, Wu Y K and Sawatzky B D 2008 Phys. Rev. C 78(3) 034003
work page 2008
-
[49]
Pitrou C, Coc A, Uzan J P and Vangioni E 2021 Mon. Not. R. Astron. Soc. 502(2) 2474
work page 2021
-
[50]
Yeh T H, Olive K A and Fields B D 2021 J. Cosmol. Astropart. Phys. 2021(03) 046
work page 2021
-
[51]
Shen Z L and He J J 2024 Nucl. Sci. Tech. 35(3) 63
work page 2024
-
[52]
(Particle Data Group) 2020 Prog
Zyla P A, Barnett R M, Beringer J, Dahl O, Dwyer D A, Groom D E, Lin C J, Lugovsky K S, Pianori E, Robinson D J et al. (Particle Data Group) 2020 Prog. Theor. Exp. Phys. 2020(8) 083C01
work page 2020
-
[53]
(Planck collaboration) 2020 Astron
Aghanim N, Akrami Y, Ashdown M, Aumont J, Baccigalupi C, Ballardini M, Banday A J, Barreiro R B, Bartolo N, Basak S et al. (Planck collaboration) 2020 Astron. Astrophys. 641 A6
work page 2020
-
[54]
Pitrou C, Coc A, Uzan J P and Vangioni E 2018 Phys. Rep. 754 1
work page 2018
-
[55]
Fields B D 2011 Annu. Rev. Nucl. Part. Sci. 61(1) 47
work page 2011
-
[56]
Cyburt R H and Davids B 2008 Phys. Rev. C 78(6) 064614
work page 2008
-
[57]
Awasthi S, Kant I, Khachi A and Sastri O S K S 2025 Indian J. Phys. 99 347
work page 2025
-
[58]
Voronchev V T 2026 J. Cosmol. Astropart. Phys. 2026(02) 025 13
work page 2026
discussion (0)
Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.