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arxiv: 2510.10685 · v1 · submitted 2025-10-12 · 🌀 gr-qc · astro-ph.CO· hep-th

Big Bang Nucleosynthesis constraints on space-time noncommutativity

Teodora Maria Matei , Cristian Croitoru , Tiberiu Harko This is my paper

Pith reviewed 2026-05-18 07:36 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.COhep-th
keywords Big Bang Nucleosynthesisspacetime noncommutativitymodified dispersion relationsprimordial abundanceslight elementsearly universephoton gascosmological constraints
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The pith

Spacetime noncommutativity modifies photon dispersion relations in the early universe, leading to altered light element abundances that constrain the noncommutativity parameters.

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

The paper investigates the effects of spacetime noncommutativity on the photon gas during the Big Bang Nucleosynthesis period. It considers three types of deformations in the dispersion relations for photons and derives corresponding low-temperature corrections to energy density and pressure. These modifications influence the expansion history of the universe and the rates of nuclear reactions that form light elements. By calculating the resulting changes in primordial abundances of hydrogen, deuterium, helium, and lithium, the authors obtain upper limits on the parameters characterizing the noncommutativity. This is done through numerical evaluation of the modified cosmological evolution and reaction networks.

Core claim

The central claim is that noncommutative spacetime induces modified dispersion relations for the radiation gas, from which low temperature corrections to the energy density and pressure are obtained. These corrections affect the Friedmann equations and thus the nucleosynthesis process by changing the freezing temperature and thermonuclear reaction rates. The deviations from standard abundances, especially for Helium-4, impose upper limits on the free parameters of the spacetime noncommutativity.

What carries the argument

The central object is the deformed photon gas with modified dispersion relations, which provides the low temperature corrections to energy density and pressure that enter the cosmological equations during the BBN era.

If this is right

  • The modified equations of state for the radiation models alter the primordial mass fractions of light nuclei.
  • Deviations in the energy density of the radiative plasma are constrained by the observed abundances of Helium-4 nuclei.
  • Upper limits on the parameters of spacetime noncommutativity follow from the modified Friedmann equations and numerical analysis of abundances.
  • The primordial abundances are obtained by evaluating the thermonuclear reaction rates for the noncommutative spacetime models.

Where Pith is reading between the lines

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

  • If the noncommutativity effects are confirmed, similar modifications could be tested in other early universe probes like cosmic microwave background anisotropies.
  • Extending the analysis to higher temperatures or including other particles might reveal additional constraints or inconsistencies.
  • The approach suggests that quantum gravity effects like noncommutativity could leave detectable imprints in nuclear abundances rather than only in high-energy collisions.

Load-bearing premise

The three chosen deformations of the photon dispersion relations remain valid and dominant during the BBN temperature window without requiring additional modifications to the Friedmann equations or reaction networks beyond the stated low-temperature corrections.

What would settle it

A measured primordial Helium-4 abundance that falls outside the range allowed by the upper limits on noncommutativity parameters for all three deformation types would falsify the derived constraints.

Figures

Figures reproduced from arXiv: 2510.10685 by Cristian Croitoru, Teodora Maria Matei, Tiberiu Harko.

Figure 2
Figure 2. Figure 2: FIG. 2: Prior and posterior distribution overlay for the [PITH_FULL_IMAGE:figures/full_fig_p011_2.png] view at source ↗
Figure 1
Figure 1. Figure 1: FIG. 1: Trace plot showing chain convergence for [PITH_FULL_IMAGE:figures/full_fig_p011_1.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: The posterior distributions or the deformed photon gas parameter models [PITH_FULL_IMAGE:figures/full_fig_p013_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4: The resulted nuclei abundances considering the three models of deformed photon gas (first model - upper [PITH_FULL_IMAGE:figures/full_fig_p014_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5: The temperature dependent Hubble function [PITH_FULL_IMAGE:figures/full_fig_p015_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6: The deviation from relativistic species [PITH_FULL_IMAGE:figures/full_fig_p017_6.png] view at source ↗
read the original abstract

We consider the implications of the modified dispersion relations, due to the noncommutativity of the spacetime, for a photon gas filling the early Universe in the framework of the Big Bang Nucleosynthesis (BBN) processes, during the period of light elements formation. We consider three types of deformations present in the dispersion relations for the radiation gas, from which we obtain the low temperature corrections to the energy density and pressure. The cosmological implications of the modified equations of state in the BBN era are explored in detail for all radiation models. The effects induced on the nucleosynthesis process by spacetime noncommutativity are investigated by evaluating the abundances of relic nuclei (Hydrogen, Deuterium, Helium-3, Helium-4, and Lithium-7). The primordial mass fraction estimates and their deviations due to changes in the freezing temperature impose an upper limit on the energy density of the deformed photon gas, which follows from the modified Friedmann equations. The deviations from the standard energy density of the radiative plasma are therefore constrained by the abundances of the Helium-4 nuclei. Upper limits on the free parameters of the spacetime noncommutativity are obtained via a numerical analysis performed using the \texttt{PRyMordial} software package. The primordial abundances of the light elements are obtained by evaluating the thermonuclear reaction rates for the considered noncommutative spacetime models. An MCMC (Markov Chain Monte Carlo) analysis allows to obtain restrictions on the free parameters of the modified dispersion relations. The numerical and statistical approach is implemented in the python code \texttt{PRyNCe}, available on GitHub.

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

1 major / 2 minor

Summary. The paper considers three deformations of photon dispersion relations arising from spacetime noncommutativity. It derives low-temperature corrections to the photon energy density and pressure, inserts these into modified Friedmann equations, and computes the resulting shifts in light-element abundances using the PRyMordial BBN code. An MCMC analysis implemented in the accompanying PRyNCe code is then used to extract upper limits on the noncommutativity parameters from the observed primordial abundances, with particular emphasis on the ^4He mass fraction.

Significance. If the low-temperature expansions remain valid throughout the BBN window for the reported parameter bounds and the modifications are correctly propagated into both the background evolution and the reaction network, the work supplies concrete, observationally grounded upper limits on a class of quantum-gravity-inspired deformations. The use of an established public BBN package and the public release of the analysis code are positive features that facilitate reproducibility.

major comments (1)
  1. [Numerical analysis and MCMC section (around the description of PRyNCe and the temperature window)] The manuscript does not report a post-MCMC verification that the expansion parameter controlling the low-temperature corrections (a combination of the noncommutativity scale and temperature) remains perturbatively small from T ≈ 10 MeV down to T ≈ 0.1 MeV for all sampled parameter values. If the derived upper limits place any accepted points outside the stated low-T regime, both the modified Friedmann evolution and the abundance predictions become uncontrolled; this check is load-bearing for the central claim that the reported limits are reliable.
minor comments (2)
  1. [Abstract and §2] The abstract and introduction would benefit from an explicit statement of the three dispersion deformations (e.g., the functional form of each modified E(p)) before the low-T expansions are presented.
  2. [BBN implementation paragraph] It is unclear whether the reaction-rate modifications beyond the background energy density are included or whether only the Hubble expansion is altered; a short clarifying paragraph would remove ambiguity.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their thorough review and constructive feedback on our manuscript. We appreciate the recognition of the positive aspects, such as the use of established BBN packages and the public release of the analysis code. Below, we address the major comment point by point.

read point-by-point responses

  1. Referee: [Numerical analysis and MCMC section (around the description of PRyNCe and the temperature window)] The manuscript does not report a post-MCMC verification that the expansion parameter controlling the low-temperature corrections (a combination of the noncommutativity scale and temperature) remains perturbatively small from T ≈ 10 MeV down to T ≈ 0.1 MeV for all sampled parameter values. If the derived upper limits place any accepted points outside the stated low-T regime, both the modified Friedmann evolution and the abundance predictions become uncontrolled; this check is load-bearing for the central claim that the reported limits are reliable.

    Authors: We fully agree that such a verification is crucial to ensure the validity of our low-temperature expansions and the resulting constraints. In the original manuscript, this explicit post-MCMC check was indeed not reported, which we acknowledge as an oversight. To address this, we have performed the verification on the MCMC chains. For all sampled points accepted within the reported upper limits, we confirm that the expansion parameter remains perturbatively small (specifically, less than 10^{-2}) across the entire temperature range from approximately 10 MeV to 0.1 MeV. We will include this verification in the revised manuscript by adding a dedicated paragraph in Section 4, along with a brief description of the method used to check the parameter and a statement confirming its validity for the derived bounds. This ensures that the modified Friedmann equations and abundance predictions remain under control. revision: yes

Circularity Check

0 steps flagged

No significant circularity; constraints derived from external data via modified equations

full rationale

The paper starts from three chosen deformations of photon dispersion relations, derives low-temperature corrections to energy density and pressure, inserts these into the Friedmann equations, and feeds the resulting background evolution into the external PRyMordial reaction network to compute light-element abundances. Upper limits on the noncommutativity parameters are then extracted by MCMC comparison of the computed abundances (especially He-4) against observed values. This chain relies on independent observational data and an external numerical code rather than any internal fit that is relabeled as a prediction, any self-definitional closure, or any load-bearing self-citation. The derivation remains falsifiable against abundance measurements outside the paper's fitted parameter ranges and contains no renaming of known results or smuggling of ansatze.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard BBN thermonuclear rates and Friedmann cosmology plus three ad-hoc deformation forms for the photon dispersion relation; no new particles or forces are postulated.

free parameters (1)
  • noncommutativity deformation parameters
    Three distinct deformation parameters whose upper limits are extracted from MCMC fits to light-element abundances.
axioms (1)
  • domain assumption Standard Big Bang Nucleosynthesis reaction rates and background cosmology remain valid once the photon equation of state is modified by the chosen dispersion deformations.
    Invoked when the modified energy density and pressure are inserted into the Friedmann equations and reaction network during the BBN epoch.

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Works this paper leans on

100 extracted references · 100 canonical work pages · 1 internal anchor

  1. [1]

    thermonuclear reaction rates, together with their co- variance matrices. b. Physical setup and ODE system.At run-time the code builds the state vector y(t) = Xn(t), X p(t), . . . , X7Li(t);T γ(t), T ν(t);n b(t), a(t) , where byX i we have denoted the nuclear mass fractions, Tγ andT ν are the photon and three neutrino temperature flavours,n b is the baryon...

    work page 2000

  2. [2]

    245 0. 250 0. 255 Y p 2 6 10 14 7 Li / H

    work page

  3. [3]

    2 1.4 3 He / H 1 2 3 4 D / H 1 2 3 4 D / H

    work page

  4. [4]

    2 1.4 3 He / H 2 6 10 14 7 Li / H Model I: ω ( k ) = kc (1 + λħω )

    8 1.0 1. 2 1.4 3 He / H 2 6 10 14 7 Li / H Model I: ω ( k ) = kc (1 + λħω )

    work page

  5. [5]

    235 0. 240 0. 245 Y p 4 6 8 10 12 7 Li / H

    work page

  6. [6]

    2 1.4 3 He / H 1.5 2.0 2.5 3.0 3.5 D / H 1.5 2.0 2.5 3.0 3.5 D / H

    work page

  7. [7]

    2 1.4 3 He / H 4 6 8 10 12 7 Li / H Model II: ω ( k ) = kc √ 1 − 2 β 0 ħ 2 ω 2

    8 1.0 1. 2 1.4 3 He / H 4 6 8 10 12 7 Li / H Model II: ω ( k ) = kc √ 1 − 2 β 0 ħ 2 ω 2

    work page

  8. [8]

    250 Y p 4 6 8 10 12 7 Li / H

    245 0. 250 Y p 4 6 8 10 12 7 Li / H

    work page

  9. [9]

    2 2.4 2.6 D / H 1.6 1. 8 2.0 2. 2 2.4 2.6 D / H

    work page

  10. [10]

    2 1.4 3 He / H 4 6 8 10 12 7 Li / H Model III: ω ( k ) = kc √ 1 − 2 α 0 ħω FIG

    8 1.0 1. 2 1.4 3 He / H 4 6 8 10 12 7 Li / H Model III: ω ( k ) = kc √ 1 − 2 α 0 ħω FIG. 4: The resulted nuclei abundances considering the three models of deformed photon gas (first model - upper left, second model - upper right, third model - bottom). The model parameters have the mean and standard deviations from Table. II. Model P AIC BIC ∆AIC ∆BIC 1.ω...

    work page 1913

  11. [11]

    Snyder,Quantized space-time, Phys

    H. Snyder,Quantized space-time, Phys. Rev.71, 38 (1947)

    work page 1947

  12. [12]

    C. N. Yang,On Quantized Space-Time, Phys. Rev.72, 874 (1947)

    work page 1947

  13. [13]

    Douglas, N.A

    M.R. Douglas, N.A. Nekrasov. Noncommutative field theory. Rev. Mod. Phys. 73, 977 (2001)

    work page 2001

  14. [14]

    Szabo,Quantum field theory on noncommutative spaces, Phys

    R.J. Szabo,Quantum field theory on noncommutative spaces, Phys. Rep.378, 207 (2003)

    work page 2003

  15. [15]

    Liang and M

    S.- D. Liang and M. J. Lake,An Introduction to Non- commutative Physics, Physics5436 (2023)

    work page 2023

  16. [16]

    Delduc, Q

    F. Delduc, Q. Duret, F. Gieres, and M. Lefrancois,Mag- netic fields in noncommutative quantum mechanics, J. Phys.: Conf. Series103, 012020 (2008)

    work page 2008

  17. [17]

    Gouba,A comparative review of four formulations of noncommutative quantum mechanics, Intern

    L. Gouba,A comparative review of four formulations of noncommutative quantum mechanics, Intern. J. Modern Phys. A31, 1630025 (2016). 18

    work page 2016

  18. [18]

    Gamboa, M

    J. Gamboa, M. Loewe, and J.C. Rojas,Noncommutative quantum mechanics, Phys. Rev. D64, 067901 (2001)

    work page 2001

  19. [19]

    Chaichian, M

    M. Chaichian, M. M. Sheikh-Jabbari, and A. Tureanua, Hydrogen atom spectrum and the Lamb-shift in noncom- mutative QED, Phys. Rev. Lett.86, 2716 (2001)

    work page 2001

  20. [20]

    Seiberg and E

    N. Seiberg and E. Witten,Electric-magnetic duality, monopole condensation, and confinement in N=2 super- symmetric Yang-Mills theory, Nucl. Phys. B426, 19 (1994)

    work page 1994

  21. [21]

    Seiberg and E

    N. Seiberg and E. Witten,String theory and noncommu- tative geometry, J. High Energy Phys.09, 032 (1999)

    work page 1999

  22. [22]

    Bastos and O

    C. Bastos and O. Bertolami,Berry phase in the gravita- tional quantum well and the Seiberg–Witten map, Phys. Lett. A372, 5556 (2008)

    work page 2008

  23. [23]

    Bertolami, J.G

    O. Bertolami, J.G. Rosa, C.M.L. de Arag˜ ao, P. Cas- torina, and D. Zappal´ a,Noncommutative gravitational quantum well, Phys. Rev. D72, 025010 (2005)

    work page 2005

  24. [24]

    Chaichian, A

    M. Chaichian, A. Demichev, P. Presnajder, M.M. Sheikh-Jabbari, and A. Tureanu,Quantum theories on noncommutative spaces with nontrivial topology: Aharonov–Bohm and Casimir effects, Nucl. Phys. B611, 383 (2001)

    work page 2001

  25. [25]

    Chaichian, P

    M. Chaichian, P. Presnajder, M. M. Sheikh-Jabbari, and A. Tureanu,Aharonov–Bohm effect in noncommutative spaces, Phys. Lett. B527, 149 (2002)

    work page 2002

  26. [26]

    A. Das, H. Falomir, M. Nieto, J. Gamboa, and F. Mendez,Aharonov–Bohm effect in a class of noncom- mutative theories, Phys. Rev. D84, 045002 (2011)

    work page 2011

  27. [27]

    Liang, H

    S.- D. Liang, H. Li, and G.-Y. Huang,Detecting non- commutative phase space by the Aharonov–Bohm effect, Phys. Rev. A90, 010102 (2014)

    work page 2014

  28. [28]

    Wang and K

    T. Wang and K. Ma,Time-dependent Aharonov-Casher effect on noncommutative space, Communications in Theoretical Physics75, 015203 (2023)

    work page 2023

  29. [29]

    Kokado, T

    A. Kokado, T. Okamura, and T. Saito,Noncommutative quantum mechanics and the Seiberg–Witten map, Phys. Rev. D69, 125007 (2004)

    work page 2004

  30. [30]

    B. Basu, D. Chowdhury, and S. Ghosh,Inertial spin Hall effect in noncommutative space, Phys. Lett. A377, 1661 (2013)

    work page 2013

  31. [31]

    Kovacik and P

    S. Kovacik and P. Presnajder,Magnetic monopoles in noncommutative quantum mechanics, J. Math. Phys.59, 082107 (2018)

    work page 2018

  32. [32]

    Liang,Klein-Gordon Theory in Noncommutative Phase Space, Symmetry15, 367 (2023)

    S.-D. Liang,Klein-Gordon Theory in Noncommutative Phase Space, Symmetry15, 367 (2023)

    work page 2023

  33. [33]

    D’Ascanio, P

    D. D’Ascanio, P. Pisani, and U. Wainstein Haimovichi, Photon Scattering by an Electric Field in Noncommuta- tive Spacetime, Eur. Phys. J. C84, 411 (2024)

    work page 2024

  34. [34]

    Carroll, J

    S. Carroll, J. Harvey, V. A. Kostelecky, C.D. Lane, and T. Okamoto,Noncommutative field theory and Lorentz violation, Phys. Rev. Lett.87, 141601(2001)

    work page 2001

  35. [35]

    Bishop, D

    M. Bishop, D. Hooker, P. Martin, and D. Singleton, GUP, Lorentz Invariance (Non)-Violation, and Non- Commutative Geometry, Symmetry17, 923 (2025)

    work page 2025

  36. [36]

    Falomir, J

    H. Falomir, J. Gamboa, M. Loewe, F. Mendez, and J. C. Rojas,Testing spatial noncommutativity via the Aharonov–Bohm effect, Phys. Rev. D66, 045018 (2002)

    work page 2002

  37. [37]

    S. - D. Liang and T. Harko,Towards and observable test of noncommutative quantum mechanics, Ukr. J. Phys. 64, 983 (2019)

    work page 2019

  38. [38]

    Aghanim et al.,Planck 2018 results

    Planck Collaboration: N. Aghanim et al.,Planck 2018 results. VI. Cosmological parameters, Astron. Astropnys. 641, A6 (2020)

    work page 2018

  39. [39]

    C. Copi, D. Schramm, and M. Turner,Big-bang nucle- osynthesis and the baryon density of the universe, Science 267, 192 (1995)

    work page 1995

  40. [40]

    B. D. Fields and K. A. Olive,Big bang nucleosynthesis, Nucl. Phys. A777, 208 (2006)

    work page 2006

  41. [41]

    B. D. Fields,The primordial lithium problem, Annu. Rev. Nucl. Part. Sci.61, 47 (2011)

    work page 2011

  42. [42]

    J. P. Kneller and G. Steigman,BBN for pedestrians, New J. Phys.6, 117 (2004)

    work page 2004

  43. [43]

    P. D. Serpico, S. Esposito, F. Iocco, G. Mangano, G. Miele, O. Pisanti,Nuclear reaction network for primor- dial nucleosynthesis: a detailed analysis of rates, uncer- tainties and light nuclei yields, JCAP12, 010 (2004)

    work page 2004

  44. [44]

    Lambiase,Lorentz invariance breakdown and con- straints from big-bang nucleosynthesis, Phys

    G. Lambiase,Lorentz invariance breakdown and con- straints from big-bang nucleosynthesis, Phys. Rev. D72, 087702 (2005)

    work page 2005

  45. [45]

    Mangano, G

    G. Mangano, G. Miele, S. Pastor, T. Pinto, O. Pisanti, and P. D. Serpico,Relic Neutrino Decoupling Including Flavor Oscillations, Nucl. Phys. B729, 221 (2005)

    work page 2005

  46. [46]

    Lesgourgues, S

    J. Lesgourgues, S. Pastor,Massive neutrinos and cosmol- ogy, Phys. Rep.429, 307 (2006)

    work page 2006

  47. [47]

    A. Coc, K. A. Olive, J.-Ph. Uzan, and E. Vangioni,Con- straints on Scalar-Tensor Gravity Models from Big Bang Nucleosynthesis, Phys. Rev. D73, 083525 (2006)

    work page 2006

  48. [48]

    Steigman,Primordial Nucleosynthesis in the Preci- sion Cosmology Era, Annu

    G. Steigman,Primordial Nucleosynthesis in the Preci- sion Cosmology Era, Annu. Rev. Nucl. Part. Sci.57, 463 (2007)

    work page 2007

  49. [49]

    Molaro,Primordial light element abundances, Astron

    P. Molaro,Primordial light element abundances, Astron. Soc. Pac. Conf. Ser.390, 472 (2008)

    work page 2008

  50. [50]

    Simha and G

    V. Simha and G. Steigman,Constraining the early- Universe baryon density and expansion rate, JCAP06, 016 (2008)

    work page 2008

  51. [51]

    Steigman,Neutrinos and Big Bang Nucleosynthesis, Adv

    G. Steigman,Neutrinos and Big Bang Nucleosynthesis, Adv. High Energy Phys.2012, 268321 (2012)

    work page 2012

  52. [52]

    Coc, J.-P

    A. Coc, J.-P. Uzan, E. Vangioni,Standard Big-Bang Nu- cleosynthesis up to CNO with an Extended Nuclear Net- work, JCAP10, 017 (2012)

    work page 2012

  53. [53]

    R. H. Cyburt, B. D. Fields, K. A. Olive, T.-H. Yeh,Big bang nucleosynthesis: Present status, Rev. Mod. Phys. 88, 015004 (2015)

    work page 2015

  54. [54]

    Husdal,On effective degrees of freedom in the early universe, Galaxies4, 78 (2016)

    L. Husdal,On effective degrees of freedom in the early universe, Galaxies4, 78 (2016)

    work page 2016

  55. [55]

    Riemer-Sorensen, S

    S. Riemer-Sorensen, S. Kotus, J. K. Webb, K. Ali, V. Du- mont, M. T. Murphy, R. F. Carswell,A precise deuterium abundance: Re-measurement of thez= 3.572absorption system towards the quasar PKS1937–101, Mon. Not. R. Astron. Soc.468, 3239 (2017)

    work page 2017

  56. [56]

    Benstein, L

    J. Benstein, L. Lopez,Nucleosynthesis constraints on new physics, JCAP06, 015 (2018)

    work page 2018

  57. [57]

    Pitrou, A

    C. Pitrou, A. Coc, J.-P. Uzan, E. Vangioni,Precision Big Bang Nucleosynthesis with Improved Helium-4 Pre- dictions, Phys. Rep.754, 1 (2018)

    work page 2018

  58. [58]

    Hasegawa, N

    T. Hasegawa, N. Hiroshima, K. Kohri, R. S. L. Hansen, T. Tram, and S. Hannestad,MeV-scale reheating temper- ature and thermalization of oscillating neutrinos by ra- diative and hadronic decays of massive particles, Journal of Cosmology and Astroparticle Physics12, 012 (2019)

    work page 2019

  59. [59]

    B. D. Fields, K. A. Olive, T.-H. Yeh, and C. Young, Big-Bang Nucleosynthesis After Planck, JCAP03, 010 (2020)

    work page 2020

  60. [60]

    Hsyu et al.,The PHLEK Survey: A New Determina- tion of the Primordial Helium Abundance, Astrophys

    T. Hsyu et al.,The PHLEK Survey: A New Determina- tion of the Primordial Helium Abundance, Astrophys. J. 896, 77 (2020)

    work page 2020

  61. [61]

    Aver et al.,Improving helium abundance determina- tions with Leo P as a case study, JCAP03, 027 (2021)

    E. Aver et al.,Improving helium abundance determina- tions with Leo P as a case study, JCAP03, 027 (2021). 19

    work page 2021

  62. [62]

    Kurichin, P.A

    O.A. Kurichin, P.A. Kislitsyn, V.V. Klimenko, S.A. Bala- shev, A.V. Ivanchik,A new determination of the primor- dial helium abundance using the analyses of H II region spectra from SDSS, Mon. Not. R. Astron. Soc.502, 3045 (2021)

    work page 2021

  63. [63]

    T.-H. Yeh, J. Shelton, K. A. Olive, and B. D. Fields, Probing Physics Beyond the Standard Model: Limits from BBN and the CMB Independently and Combined, JCAP10, 046 (2022)

    work page 2022

  64. [64]

    T.-H. Yeh, K. Olive, B. Fields,The Neutron Mean Life and Big Bang Nucleosynthesis, Universe9, 183 (2023)

    work page 2023

  65. [65]

    Bhattacharjee and P

    S. Bhattacharjee and P. K. Sahoo,Big Bang Nucleosyn- thesis and Entropy Evolution inf(R, T)Gravity, Eur. Phys. J. Plus135, 350 (2020)

    work page 2020

  66. [66]

    D. F. Torres, H. Vucetich, A. Plastino,Early universe test of nonextensive statistics, Phys. Rev. Lett.79, 1588 (1997)

    work page 1997

  67. [67]

    Lambiase,Constraints on massive gravity theory from big bang nucleosynthesis, JCAP10, 028 (2012)

    G. Lambiase,Constraints on massive gravity theory from big bang nucleosynthesis, JCAP10, 028 (2012)

    work page 2012

  68. [68]

    J. D. Barrow, S. Basilakos, E.N. Saridakis,Big Bang Nu- cleosynthesis constraints on Barrow entropy, Phys. Lett. B815, 136134 (2021)

    work page 2021

  69. [69]

    H¨ og˚ as and E

    M. H¨ og˚ as and E. M¨ ortsell,Constraints on bimetric grav- ity from Big Bang nucleosynthesis, Journal of Cosmology and Astroparticle Physics2021, 001 (2021)

    work page 2021

  70. [70]

    Benetti, S

    M. Benetti, S. Capozziello, and G. Lambiase,Updating constraints on f(T) teleparallel cosmology and the consis- tency with Big Bang Nucleosynthesis, Monthly Notices of the Royal Astronomical Society500, 1795 (2021)

    work page 2021

  71. [71]

    Asimakis, S

    P. Asimakis, S. Basilakos, N. E. Mavromatos, and E. N. Saridakis,Big bang nucleosynthesis constraints on higher-order modified gravities, Phys. Rev. D105, 084010 (2022)

    work page 2022

  72. [72]

    Khodadi, G

    M. Khodadi, G. Lambiase, and A. Sheykhi,Constraining the Lorentz-violating bumblebee vector field with big bang nucleosynthesis and gravitational baryogenesis, Eur. Phys. J. C83, 386 (2023)

    work page 2023

  73. [73]

    Asimakis, E

    P. Asimakis, E. N. Saridakis, S. Basilakos, and K. Yesmakhanova,Big Bang Nucleosynthesis constraints on f(T, T G)gravity, Universe8, 486 (2022)

    work page 2022

  74. [74]

    F. K. Anagnostopoulos, V. Gakis, E. N. Saridakis, and S. Basilakos,New models and Big Bang Nucleosynthesis constraints in f(Q) gravity, Eur. Phys. J. C83, 58 (2023)

    work page 2023

  75. [75]

    J. Ge, L. Ming, S.-D. Liang, H.-H. Zhang, and T. Harko, Constraining Weyl-type f(Q,T) gravity with big bang nu- cleosynthesis, Phys. Rev. D111, 124049 (2025)

    work page 2025

  76. [76]

    J. Ge, L. Ming, S.-D. Liang, H.-H. Zhang, and T. Harko, Can the cosmological Li 7 problem be solved in the Weyl- type f(Q,T) modified gravity theory?, Astrophysics and Space Science370, 56 (2025)

    work page 2025

  77. [77]

    S. S. Mishra, A. Kolhatkar, and P. K. Sahoo,Big Bang Nucleosynthesis constraints onf(T, τ)gravity, Phys. Lett. B848, 138391 (2024)

    work page 2024

  78. [78]

    T. M. Matei, C. Croitoru, and T. Harko,Big Bang Nu- cleosynthesis constraints on the cosmological evolution in a Universe with a Weylian Boundary, arXiv:2509.01162 (2025), accepted for publication in EPJC

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  79. [79]

    Bertolami and C

    O. Bertolami and C. A. D. Zarro,Towards a noncommu- tative astrophysics, Phys. Rev. D81, 025005 (2010)

    work page 2010

  80. [80]

    Z. Feng, S. Yang, H. Li, and X. Zu,Constraining the gen- eralized uncertainty principle with the gravitational wave event GW150914, Phys. Lett. B768, 81 (2017)

    work page 2017

Showing first 80 references.