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Torsion induced current-scalaron coupling in Einstein-Cartan gravity

T0 review · 2 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

Pith's one-line read Torsion in Einstein–Cartan gravity turns matter currents into scalaron couplings, and gauge-dependent currents acquire Chern–Simons interactions in the equivalent metric theory.

desk verdict A workmanlike extension of the authors' own scalaron framework: the general current-coupling formulas hold up, and the one real error sits in an illustrative bound, not in the central derivation. read the letter →

arxiv 2507.12151 v1 pith:FYC262A2 submitted 2025-07-16 hep-ph astro-ph.COgr-qc

classification hep-phastro-ph.COgr-qc
keywords Einstein-CartangravitytorsionscalaronmattercurrentsChern-SimonscouplingstrongCPprobleminflationreheating
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper tries to establish that in Einstein–Cartan gravity, once the dimension-four geometric part of the action is a rank-one complete square, the torsion-induced (pseudo-)scalar, the scalaron, necessarily acquires derivative couplings to matter currents: $\nabla_\mu \phi j^\mu$ for gauge-invariant currents, and $\phi F\tilde F$ Chern–Simons couplings for gauge-dependent currents in the equivalent metric theory. The authors derive the general action, the decay constants $f_1$ and $f_2$ for these interactions, and their asymptotic behavior in large- and small-field limits. They work out explicit examples connected to Starobinsky/$\alpha$-attractor inflation and to QCD, showing that a pure chiral-current coupling cannot solve the strong CP problem, whereas the gauge-dependent Chern–Simons construction can relate the scalaron to the QCD $\theta$ term, though not without extra fine-tuning. This matters because these couplings control reheating, baryogenesis, and gauge-field production after inflation in Einstein–Cartan models.

What carries the argument

The load-bearing object is the rank-one complete-square geometric action: the dimension-four part formed from $\bar R$, $S_\mu S^\mu$, $T_\mu T^\mu$, $\nabla_\mu S^\mu$, and $\nabla_\mu T^\mu$ is chosen so its quadratic form has rank one, which guarantees the torsion-induced scalaron can be canonically normalized through an auxiliary field $\chi$ and a Weyl transformation to the Einstein frame. Gauge-invariant currents enter as linear torsion couplings; gauge-dependent currents are handled by the field redefinition $S'_\mu = S_\mu + \zeta j_\mu/M_{\rm Pl}^2$ and $T'_\mu = T_\mu + \xi j_\mu/M_{\rm Pl}^2$, which keeps the action gauge invariant and, after integration by parts, yields Chern–Simons couplings. The decay constants $f_1, f_2$ in Eq. (3.16) measure the strength of the scalaron–current and current–current interactions and encode the effective-field-theory cutoff.

What would settle it

Compute the path-integral Jacobian for the field redefinition $S'_\mu = S_\mu + \zeta j_\mu/M_{\rm Pl}^2$, $T'_\mu = T_\mu + \xi j_\mu/M_{\rm Pl}^2$ for a chiral current with a known anomaly, e.g. the electroweak $SU(2)_L$ current. If the Jacobian is nontrivial or the redefinition generates extra boundary terms, the predicted coefficient of $\phi F\tilde F$ in Eq. (4.16) is incomplete and the central claim fails.

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Extended reading notes

Core claim

The paper's central claim is that a canonical scalaron emerges from an Einstein–Cartan action whose dimension-four geometric sector is a single complete square, and that matter currents coupled to torsion become, in the Einstein frame, interactions of that scalaron with the currents. For gauge-invariant currents the interaction is a derivative coupling $\nabla_\mu \phi \, j^\mu$ plus a current self-coupling, and the paper defines the decay constants $f_1(\phi)$ and $f_2(\phi)$ in Eq. (3.16). For gauge-dependent currents, the paper's construction uses the shifted torsion fields $S'_\mu = S_\mu + \zeta j_\mu/M_{\rm Pl}^2$ and $T'_\mu = T_\mu + \xi j_\mu/M_{\rm Pl}^2$; integrating by parts converts the resulting $\chi \nabla_\mu j^\mu$ terms into $\phi F\tilde F$ couplings for Chern–Simons currents. The paper also shows that in the minimal fermion kinetic coupling, the scalaron–current interaction alone cannot generate a QCD $\theta$-term potential, but the Chern–Simons coupling can, so the scalaron is a possible but generically not a viable QCD axion because it also couples to dimensionful parameters.

Load-bearing premise

The load-bearing premise is that shifting the torsion fields by the matter current is a harmless change of variables that introduces no new degrees of freedom, anomalies, or boundary terms; if that premise fails, the derived $\phi F\tilde F$ couplings do not follow.

Editorial extensions

If this is right

  • The scalaron from Einstein–Cartan gravity has model-independent derivative couplings to chiral currents; in the minimal case with $\zeta = 1/8$ the coupling strength is set by $M_{\rm Pl}$ and gives a decay channel $\phi \to \bar\psi\psi$ as well as current self-interactions with cutoff $\sim M_{\rm Pl}/|\zeta|$.
  • Adding the Chern–Simons current through the shifted torsion fields produces $\phi F\tilde F$ couplings, so the scalaron can be sensitive to the QCD $\theta$ term; the paper shows this is a necessary but not sufficient condition for the scalaron to play the QCD axion.
  • In a U(1) example, the Chern–Simons coupling causes efficient gauge-field production during inflation, with parameter constraints from the absence of ghost instabilities in chiral gravitational waves and from non-Gaussianity bounds.
  • Depending on the parameters, the scalaron potential can take power-law or plateau forms, including Starobinsky and regularized-pole inflation, and the decay constants $f_1, f_2$ have distinct asymptotic behaviors; cases where $f \to 0$ indicate a low EFT cutoff and are unsuitable for reheating.
  • The results extend to multiple currents and to mixed gauge-invariant/gauge-dependent current systems, giving a general EFT language for post-inflationary particle production in Einstein–Cartan models.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • The same shift construction should apply to any current whose divergence is gauge invariant beyond the Chern–Simons examples, so the method likely extends to anomalous baryon/lepton currents and to gravitational Chern–Simons currents, giving additional scalaron-mediated production channels.
  • If the scalaron's couplings to dimensionful parameters are removed by a no-scale or scale-invariant completion, the $\phi F\tilde F$ construction could make the Einstein–Cartan scalaron a genuine QCD axion; the paper leaves that completion unbuilt.
  • The asymptotic decay-constant tables provide a way to translate future measurements of reheating temperature, non-Gaussianity, or chiral gravitational waves into constraints on the Einstein–Cartan parameters $\alpha_4, \alpha_5, \zeta, \xi$.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 4 minor

Summary. The paper studies Einstein–Cartan gravity with a geometric action in which the dimension-four torsion- and curvature-dependent part is a rank-one complete square, so that the auxiliary torsion components induce a canonical (pseudo-)scalar degree of freedom, the scalaron. The authors add couplings between torsion and matter currents, distinguish gauge-invariant currents from gauge-dependent currents such as Chern–Simons currents, and derive the equivalent metric-frame theory by Legendre transformation and Weyl rescaling. The central results are the general formulas (3.15)–(3.16) for derivative current couplings and current self-couplings of the canonical scalaron, and Eq. (4.12), which yields φ F F-tilde-type couplings from gauge-dependent currents. The paper also gives asymptotic tables for decay constants, works out Starobinsky/α-attractor examples, and discusses the relation to the QCD θ term and to gauge-field production during inflation.

Significance. If the results are correct, the paper provides a general EFT description of scalaron–matter interactions in EC inflation models, including a gauge-invariant embedding of gauge-dependent currents that produces axion-like couplings to Chern–Simons terms. This is directly relevant for reheating, baryogenesis, and the proposal that the torsion-induced scalaron could be a QCD axion. The central derivation is algebraic and parameter-free in the sense that no observable is fitted to data; the key equations, (3.15)–(3.16) and (4.12), are explicit and reproducible from the stated action. The paper also usefully clarifies that a bare chiral-current coupling does not generate a QCD θ-term potential, and identifies the additional requirements for a viable axion candidate. The stress-test concern about the field shift in Eqs. (4.2)–(4.6) does not land: the shift is an invertible bosonic redefinition with unit Jacobian and does not introduce new degrees of freedom or anomalies.

major comments (2)
  1. [§4.2.2, Eq. (4.22)] The slow-roll expression for dot φ is incorrect. From V = M_Pl^4/(16 α_R) [1 - exp(-φ/(√6 α_4 M_Pl))]^2, one obtains V_φ/V = 2/(√6 α_4 M_Pl) / [exp(φ/(√6 α_4 M_Pl)) - 1], so the slow-roll formula is dot φ = -M_Pl H * 2/(√6 α_4) / [exp(φ/(√6 α_4 M_Pl)) - 1], not -M_Pl H * 2√6 α_4 / [exp(φ/(√6 α_4 M_Pl)) - 1] as written. The displayed expression has the wrong dependence on α_4 and on the combination √6 α_4 M_Pl. This error propagates into the bounds in Eq. (4.24) and the subsequent discussion of allowed parameter space for α_4 and ζ_32. The central coupling formulas (3.15)–(3.16) and (4.12) are unaffected, but the illustrative gauge-production constraints must be rederived.
  2. [§3.1, Eqs. (3.11)–(3.16) and Tables 1–8] The general formalism defines decay constants and a canonical inflaton through the square root in Eq. (3.14), which requires the bracket in Eq. (3.13) to be positive and the denominator in F, G, I to be non-vanishing. The paper only states an implicit assumption that the coefficients are suitably chosen, and the asymptotic tables explicitly include cases where the relevant coefficients vanish or the denominator changes sign. For the claimed general result to be well defined, the authors should either state the explicit positivity and non-vanishing conditions on the coefficients α_i, β_i and χ, or clearly delimit the parameter/field-space region in which Eqs. (3.15)–(3.16) and the tables are valid. This is a load-bearing point because the canonicalization and the definition of the decay constants depend on it, although the concrete examples do check some of these conditions.
minor comments (4)
  1. [§1, first paragraph] There is a typo in 'an Eisntein–Hilbert action'; it should read 'Einstein–Hilbert'.
  2. [§3.1, Eq. (3.13)] The notation α is overloaded: in Eq. (3.13) the coefficient 24 α^2 is presumably α_R, but α was not explicitly defined before this equation beyond its appearance in Ω^2 in Eq. (3.3). Please define it consistently, e.g., as α ≡ α_R, to avoid confusion with α_1, α_2, α_4, α_5.
  3. [§4.1, Eq. (4.11)] The text reads 'after Wely transformation'; this should be 'after Weyl transformation'.
  4. [§4.2.2, Eq. (4.25)] The trace-anomaly term is introduced with coefficient 1/(24 π^2); the sign and normalization should be checked against the convention used for the dual field strength and the Weyl rescaling, since the subsequent combined expression in Eq. (4.26) depends on this convention.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the scalaron-current couplings are derived by algebraic elimination from an explicit EC action; prior self-citations motivate but do not carry the load-bearing steps.

full rationale

The derivation chain is self-contained. Starting from Eq. (3.1), the paper introduces an auxiliary field chi by Legendre transformation, solves the algebraic constraint equations for S_mu and T_mu, Weyl-transforms to the Einstein frame, and canonicalizes the scalaron via Eq. (3.14). The current couplings in Eqs. (3.15)-(3.16) and the gauge-dependent-current result in Eq. (4.12) are read off from the resulting Lagrangian after solving the torsion equations; no parameter is fitted to data and no output quantity is an input by construction. The scalaron-from-torsion framework is attributed to the authors' Ref. [56], but the present paper re-derives the scalaron kinetic term, Weyl factor, and canonicalization explicitly (Eqs. (3.5), (3.13), (3.14)), so the self-citation is not load-bearing in a circular sense. The gauge-dependent-current embedding in Eqs. (4.2)-(4.6) is an explicit, gauge-invariant model-building assumption; the resulting chi (nabla_mu j^mu) couplings, and hence phi F F-tilde for Chern-Simons currents, follow by algebra and the standard divergence identity for the Chern-Simons form. The slow-roll factor in Eq. (4.22) appears to be a typographical/correctness issue rather than a circularity, and it does not enter the main coupling derivations.

Assumptions & free parameters 3 free parameters · 6 assumptions · 1 invented entities

The central claim rests on the rank-one complete-square geometric action, the algebraic elimination of torsion, and the gauge-invariant shift construction for gauge-dependent currents. The coefficients of these operators and current couplings are free model parameters chosen by hand; none are fitted to data. No new fundamental entity is postulated beyond the derived scalaron.

free parameters (3)
  • Geometric EFT coefficients alpha_R, alpha_1, alpha_2, alpha_4, alpha_5, beta_1, beta_2, beta_3 = not fitted; arbitrary model parameters (example 1: alpha=1, alpha1=beta1=1/24, alpha2=beta2=-2/3, alpha5=2; example 2…
    Enter the action Eq (3.1) and (4.2); the central formulas for F, G, I and the decay constants depend on them. They are chosen by hand, not constrained by data in this paper.
  • Current-torsion couplings zeta_n, xi_n = not fitted; zeta=1/8 from minimal fermion kinetic term, otherwise free
    Determine the scalaron-current coupling strength and current self-coupling; kept general throughout and specialized in examples.
  • Example-specific parameters alpha_4, beta'_3, alpha'_3, zeta_31, zeta_32 = not fitted; chosen to illustrate Starobinsky, deformed pole inflation, and gauge field production
    Set by the model choices in Secs 3.2 and 4.2.2; the constraints in Sec 4.2.2 bound zeta_31 and zeta_32 but are not fits to data.
assumptions (6)
  • standard math Vierbein and spin-connection formulation of EC gravity with torsion decomposed into vector, axial vector, and tensor parts
    Sec 2 and Appendix A define the geometry and the relation Rbar = R + 2 nabla T - (2/3) T^2 + (1/24) S^2 + (1/2) q^2.
  • domain assumption Torsion components S_mu and T_mu are non-dynamical auxiliary fields that can be eliminated algebraically
    Used to solve constraint equations after Eq (3.2) and after Eq (4.8); no torsion kinetic terms are included.
  • domain assumption The dimension-four geometric part must be a rank-one complete square to produce a canonically normalizable scalaron
    Inherited from Ref [56] and stated in Sec 3; restricts the class of EC models considered.
  • domain assumption The Einstein-frame kinetic coefficient in Eq (3.13) is positive and denominators such as 4 beta1 beta2 - beta3^2 do not vanish in the field range of interest
    Required for the canonicalization Eq (3.14); the paper states coefficients are properly chosen but does not systematically characterize the parameter space.
  • domain assumption For gauge-dependent currents, the shift S'_mu = S_mu + zeta j_mu/M_Pl^2 is a valid field redefinition and d*j is gauge invariant
    Sec 4, Eq (4.2)-(4.6); this is the novel construction that generates phi F F-tilde couplings.
  • domain assumption Chiral rotation anomaly and QCD non-perturbative theta-term physics follow standard textbook results
    Appendix B and Secs 3.2 and 4.2.1 use the Fujikawa Jacobian and QCD instanton potential; references [105] and [122].
invented entities (1)
  • Scalaron (pseudo-scalar field phi, auxiliary chi)
    purpose: Propagating scalar degree of freedom induced by the rank-one complete-square geometric action; mediates torsion-current couplings and can be an inflaton or axion candidate.
    Introduced via Legendre transform in Eq (3.2) and canonicalized in Eq (3.14); it is a derived degree of freedom of the EFT, not a new fundamental particle with independent experimental evidence.

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Pith. "Pith review of Torsion induced current-scalaron coupling in Einstein-Cartan gravity." pith.science (2026). https://pith.science/paper/FYC262A2

@misc{pith2026250712151,
  author       = {Pith},
  title        = {Pith review of: Torsion induced current-scalaron coupling in Einstein-Cartan gravity},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/FYC262A2}},
  note         = {Machine review of arXiv:2507.12151}
}
abstract

We investigate the matter current couplings with the scalar degrees of freedom originated from the torsion in Einstein-Cartan (EC) gravity. It has been shown in previous studies that the presence of the operators consisting of torsion components up to dimension four can naturally induce a (pseudo-)scalar degree of freedom, the scalaron. In this work, we consider the couplings between torsion and matter currents in this framework, and show that they can lead to couplings between these currents and the scalaron in the equivalent metric theory. We consider both gauge-invariant and gauge-dependent currents, showing general results and several concrete examples. These results are useful for the discussion of particle production processes after inflation in the EC framework, such as reheating and baryogenesis, and show the connection to the QCD $\theta$ term.

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Reference graph

Works this paper leans on

124 extracted references · 16 canonical work pages · cited by 4 Pith papers

  1. [1]

    Gauge Theories of Gravitation,

    M. Blagojevic and F. W. Hehl, “Gauge Theories of Gravitation, ”arXiv:1210.3775 [gr-qc]

  2. [2]

    An Identity in Riemann-cartan Geometry,

    H. T. Nieh and M. L. Yan, “An Identity in Riemann-cartan Geometry, ”J. Math. Phys. 23 (1982) 373

  3. [3]

    A Torsional Topological Invariant,

    H. T. Nieh, “A Torsional Topological Invariant, ” inConference in Honor of C.N. Yang’s 85th Birthday: Statistical Physics, High Energy, Condensed Matter and Mathematical Physics , pp. 29–37. 2008. arXiv:1309.0915 [gr-qc] . 27

  4. [4]

    PARITY VIOLATION IN METRIC TORSION THEORIES OF GRAVITATION,

    R. Hojman, C. Mukku, and W. A. Sayed, “PARITY VIOLATION IN METRIC TORSION THEORIES OF GRAVITATION, ”Phys. Rev. D 22 (1980) 1915–1921

  5. [5]

    Gravity With Propagating Pseudoscalar Torsion,

    P. C. Nelson, “Gravity With Propagating Pseudoscalar Torsion, ”Phys. Lett. A 79 (1980) 285

  6. [6]

    Castellani, R

    L. Castellani, R. D’Auria, and P. Fre, Supergravity and superstrings: A Geometric perspective. Vol. 1: Mathematical foundations. 1991

  7. [7]

    Barbero’s Hamiltonian derived from a generalized Hilbert-Palatini action,

    S. Holst, “Barbero’s Hamiltonian derived from a generalized Hilbert-Palatini action, ” Phys. Rev. D 53 (1996) 5966–5969, arXiv:gr-qc/9511026

  8. [8]

    A New Type of Isotropic Cosmological Models Without Singularity,

    A. A. Starobinsky, “A New Type of Isotropic Cosmological Models Without Singularity, ”Phys. Lett. B 91 (1980) 99–102

Show all 124 references
  1. [9]

    First Order Phase Transition of a Vacuum and Expansion of the Universe,

    K. Sato, “First Order Phase Transition of a Vacuum and Expansion of the Universe, ”Mon. Not. Roy. Astron. Soc. 195 (1981) 467–479

  2. [10]

    The Inflationary Universe: A Possible Solution to the Horizon and Flatness Problems,

    A. H. Guth, “The Inflationary Universe: A Possible Solution to the Horizon and Flatness Problems, ” Phys. Rev. D 23 (1981) 347–356

  3. [11]

    Quantum Fluctuations and a Nonsingular Universe,

    V. F. Mukhanov and G. V. Chibisov, “Quantum Fluctuations and a Nonsingular Universe, ”JETP Lett. 33 (1981) 532–535

  4. [12]

    A New Inflationary Universe Scenario: A Possible Solution of the Horizon, Flatness, Homogeneity, Isotropy and Primordial Monopole Problems,

    A. D. Linde, “A New Inflationary Universe Scenario: A Possible Solution of the Horizon, Flatness, Homogeneity, Isotropy and Primordial Monopole Problems, ”Phys. Lett. B 108 (1982) 389–393

  5. [13]

    Cosmology for Grand Unified Theories with Radiatively Induced Symmetry Breaking,

    A. Albrecht and P. J. Steinhardt, “Cosmology for Grand Unified Theories with Radiatively Induced Symmetry Breaking, ”Phys. Rev. Lett. 48 (1982) 1220–1223

  6. [14]

    Inflationary cosmology: First 30+ years,

    K. Sato and J. Yokoyama, “Inflationary cosmology: First 30+ years, ”Int. J. Mod. Phys. D 24 no. 11, (2015) 1530025

  7. [15]

    Higgs inflation in Einstein-Cartan gravity,

    M. Shaposhnikov, A. Shkerin, I. Timiryasov, and S. Zell, “Higgs inflation in Einstein-Cartan gravity, ” JCAP 02 (2021) 008, arXiv:2007.14978 [hep-ph] . [Erratum: JCAP 10, E01 (2021)]

  8. [16]

    Einstein-Cartan gravity, matter, and scale-invariant generalization ,

    M. Shaposhnikov, A. Shkerin, I. Timiryasov, and S. Zell, “Einstein-Cartan gravity, matter, and scale-invariant generalization , ”JHEP 10 (2020) 177, arXiv:2007.16158 [hep-th]

  9. [17]

    Induced gravity inflation in the standard model of particle physics,

    J. L. Cervantes-Cota and H. Dehnen, “Induced gravity inflation in the standard model of particle physics, ”Nucl. Phys. B 442 (1995) 391–412, arXiv:astro-ph/9505069

  10. [18]

    The Standard Model Higgs boson as the inflaton,

    F. L. Bezrukov and M. Shaposhnikov, “The Standard Model Higgs boson as the inflaton, ”Phys. Lett. B 659 (2008) 703–706, arXiv:0710.3755 [hep-th]

  11. [19]

    Inflation scenario via the Standard Model Higgs boson and LHC,

    A. O. Barvinsky, A. Y. Kamenshchik, and A. A. Starobinsky, “Inflation scenario via the Standard Model Higgs boson and LHC, ”JCAP 11 (2008) 021, arXiv:0809.2104 [hep-ph]

  12. [20]

    Higgs-Palatini Inflation and Unitarity,

    F. Bauer and D. A. Demir, “Higgs-Palatini Inflation and Unitarity, ”Phys. Lett. B 698 (2011) 425–429, arXiv:1012.2900 [hep-ph] . 28

  13. [21]

    Higgs inflation in the Palatini formulation with kinetic terms for the metric,

    S. Rasanen, “Higgs inflation in the Palatini formulation with kinetic terms for the metric, ” Open J. Astrophys. 2 no. 1, (2019) 1, arXiv:1811.09514 [gr-qc]

  14. [22]

    Violent Preheating in Inflation with Nonminimal Coupling,

    Y. Ema, R. Jinno, K. Mukaida, and K. Nakayama, “Violent Preheating in Inflation with Nonminimal Coupling, ”JCAP 02 (2017) 045, arXiv:1609.05209 [hep-ph]

  15. [23]

    Preheating after Higgs Inflation: Self-Resonance and Gauge boson production,

    E. I. Sfakianakis and J. van de Vis, “Preheating after Higgs Inflation: Self-Resonance and Gauge boson production, ”Phys. Rev. D 99 no. 8, (2019) 083519, arXiv:1810.01304 [hep-ph]

  16. [24]

    Power-counting and the Validity of the Classical Approximation During Inflation,

    C. P. Burgess, H. M. Lee, and M. Trott, “Power-counting and the Validity of the Classical Approximation During Inflation, ”JHEP 09 (2009) 103, arXiv:0902.4465 [hep-ph]

  17. [25]

    On the Naturalness of Higgs Inflation,

    J. L. F. Barbon and J. R. Espinosa, “On the Naturalness of Higgs Inflation, ”Phys. Rev. D 79 (2009) 081302, arXiv:0903.0355 [hep-ph]

  18. [26]

    Comment on Higgs Inflation and Naturalness,

    C. P. Burgess, H. M. Lee, and M. Trott, “Comment on Higgs Inflation and Naturalness, ”JHEP 07 (2010) 007, arXiv:1002.2730 [hep-ph]

  19. [27]

    On Inflation with Non-minimal Coupling,

    M. P. Hertzberg, “On Inflation with Non-minimal Coupling, ” JHEP 11 (2010) 023, arXiv:1002.2995 [hep-ph]

  20. [28]

    Higgs boson, renormalization group, and naturalness in cosmology,

    A. O. Barvinsky, A. Y. Kamenshchik, C. Kiefer, A. A. Starobinsky, and C. F. Steinwachs, “Higgs boson, renormalization group, and naturalness in cosmology, ”Eur. Phys. J. C 72 (2012) 2219, arXiv:0910.1041 [hep-ph]

  21. [29]

    Higgs inflation: consistency and generalisations,

    F. Bezrukov, A. Magnin, M. Shaposhnikov, and S. Sibiryakov, “Higgs inflation: consistency and generalisations, ”JHEP 01 (2011) 016, arXiv:1008.5157 [hep-ph]

  22. [30]

    Tree-level unitarity in Higgs inflation in the metric and the Palatini formulation,

    A. Ito, W. Khater, and S. Rasanen, “Tree-level unitarity in Higgs inflation in the metric and the Palatini formulation, ”JHEP 06 (2022) 164, arXiv:2111.05621 [astro-ph.CO]

  23. [31]

    Quantum corrections to Higgs inflation in Einstein-Cartan gravity,

    M. He, K. Kamada, and K. Mukaida, “Quantum corrections to Higgs inflation in Einstein-Cartan gravity, ”JHEP 01 (2024) 014, arXiv:2308.14398 [hep-ph]

  24. [32]

    Unitarizing Higgs Inflation,

    G. F. Giudice and H. M. Lee, “Unitarizing Higgs Inflation, ” Phys. Lett. B 694 (2011) 294–300, arXiv:1010.1417 [hep-ph]

  25. [33]

    Higgs Inflation as a Mirage,

    J. L. F. Barbon, J. A. Casas, J. Elias-Miro, and J. R. Espinosa, “Higgs Inflation as a Mirage, ”JHEP 09 (2015) 027, arXiv:1501.02231 [hep-ph]

  26. [34]

    Higgs Scalaron Mixed Inflation,

    Y. Ema, “Higgs Scalaron Mixed Inflation, ”Phys. Lett. B 770 (2017) 403–411, arXiv:1701.07665 [hep-ph]

  27. [35]

    Light inflaton completing Higgs inflation,

    H. M. Lee, “Light inflaton completing Higgs inflation, ” Phys. Rev. D 98 no. 1, (2018) 015020, arXiv:1802.06174 [hep-ph]

  28. [36]

    Non-local self-healing of Higgs inflation,

    A. S. Koshelev and A. Tokareva, “Non-local self-healing of Higgs inflation, ”Phys. Rev. D 102 (2020) 123518, arXiv:2006.06641 [hep-th] . 29

  29. [37]

    Classical and Quantum Initial Conditions for Higgs Inflation,

    A. Salvio and A. Mazumdar, “Classical and Quantum Initial Conditions for Higgs Inflation, ”Phys. Lett. B 750 (2015) 194–200, arXiv:1506.07520 [hep-ph]

  30. [38]

    From stable to unstable anomaly-induced inflation,

    T. d. P. Netto, A. M. Pelinson, I. L. Shapiro, and A. A. Starobinsky, “From stable to unstable anomaly-induced inflation, ”Eur. Phys. J. C 76 no. 10, (2016) 544, arXiv:1509.08882 [hep-th]

  31. [39]

    Inflation in an effective gravitational model and asymptotic safety,

    L.-H. Liu, T. Prokopec, and A. A. Starobinsky, “Inflation in an effective gravitational model and asymptotic safety, ”Phys. Rev. D 98 no. 4, (2018) 043505, arXiv:1806.05407 [gr-qc]

  32. [40]

    Higgs Starobinsky Inflation,

    X. Calmet and I. Kuntz, “Higgs Starobinsky Inflation, ” Eur. Phys. J. C 76 no. 5, (2016) 289, arXiv:1605.02236 [hep-th]

  33. [41]

    Two-loop corrections to Starobinsky-Higgs inflation,

    D. M. Ghilencea, “Two-loop corrections to Starobinsky-Higgs inflation, ”Phys. Rev. D 98 no. 10, (2018) 103524, arXiv:1807.06900 [hep-ph]

  34. [42]

    Dynamical Emergence of Scalaron in Higgs Inflation,

    Y. Ema, “Dynamical Emergence of Scalaron in Higgs Inflation, ”JCAP 09 (2019) 027, arXiv:1907.00993 [hep-ph]

  35. [43]

    Higgs inflation as nonlinear sigma model and scalaron as its 𝜎-meson,

    Y. Ema, K. Mukaida, and J. van de Vis, “Higgs inflation as nonlinear sigma model and scalaron as its 𝜎-meson, ”JHEP 11 (2020) 011, arXiv:2002.11739 [hep-ph]

  36. [44]

    Renormalization group equations of Higgs-R2 inflation,

    Y. Ema, K. Mukaida, and J. van de Vis, “Renormalization group equations of Higgs-R2 inflation, ”JHEP 02 (2021) 109, arXiv:2008.01096 [hep-ph]

  37. [45]

    Scalaron the healer: removing the strong-coupling in the Higgs- and Higgs-dilaton inflations,

    D. Gorbunov and A. Tokareva, “Scalaron the healer: removing the strong-coupling in the Higgs- and Higgs-dilaton inflations, ”Phys. Lett. B 788 (2019) 37–41, arXiv:1807.02392 [hep-ph]

  38. [46]

    On the violent preheating in the mixed Higgs-𝑅2 inflationary model,

    M. He, R. Jinno, K. Kamada, S. C. Park, A. A. Starobinsky, and J. Yokoyama, “On the violent preheating in the mixed Higgs-𝑅2 inflationary model, ”Phys. Lett. B 791 (2019) 36–42, arXiv:1812.10099 [hep-ph]

  39. [47]

    On UV-completion of Palatini-Higgs inflation,

    Y. Mikura and Y. Tada, “On UV-completion of Palatini-Higgs inflation, ”JCAP 05 no. 05, (2022) 035, arXiv:2110.03925 [hep-ph]

  40. [48]

    Hybrid metric-Palatini Higgs inflation,

    M. He, Y. Mikura, and Y. Tada, “Hybrid metric-Palatini Higgs inflation, ”JCAP 05 (2023) 047, arXiv:2209.11051 [hep-th]

  41. [49]

    Towards a classification of UV completable Higgs inflation in metric-affine gravity,

    Y. Mikura and Y. Tada, “Towards a classification of UV completable Higgs inflation in metric-affine gravity, ”JCAP 02 (2025) 044, arXiv:2410.11277 [hep-th]

  42. [50]

    Weyl gravity extension of Higgs inflation,

    S. Aoki and H. M. Lee, “Weyl gravity extension of Higgs inflation, ”Phys. Rev. D 108 no. 3, (2023) 035045, arXiv:2207.05484 [hep-ph]

  43. [51]

    Matter matters in Einstein-Cartan gravity,

    G. K. Karananas, M. Shaposhnikov, A. Shkerin, and S. Zell, “Matter matters in Einstein-Cartan gravity, ” Phys. Rev. D 104 no. 6, (2021) 064036, arXiv:2106.13811 [hep-th]

  44. [52]

    Generalized Ashtekar variables for Palatini 𝑓() models,

    F. Bombacigno, S. Boudet, and G. Montani, “Generalized Ashtekar variables for Palatini 𝑓() models, ” Nucl. Phys. B 963 (2021) 115281, arXiv:1911.09066 [gr-qc] . 30

  45. [53]

    Boudet, Theoretical and Phenomenological Aspects of Projective-Invariant Metric-Affine Theories of Gravity

    S. Boudet, Theoretical and Phenomenological Aspects of Projective-Invariant Metric-Affine Theories of Gravity. PhD thesis, University of Trento, 2023

  46. [54]

    (In)equivalence of metric-affine and metric effective field theories,

    G. Pradisi and A. Salvio, “(In)equivalence of metric-affine and metric effective field theories, ” Eur. Phys. J. C 82 no. 9, (2022) 840, arXiv:2206.15041 [hep-th]

  47. [55]

    Einstein–Cartan pseudoscalaron inflation,

    A. Di Marco, E. Orazi, and G. Pradisi, “Einstein–Cartan pseudoscalaron inflation, ” Eur. Phys. J. C 84 no. 2, (2024) 146, arXiv:2309.11345 [hep-th]

  48. [56]

    Starobinsky inflation and beyond in Einstein-Cartan gravity,

    M. He, M. Hong, and K. Mukaida, “Starobinsky inflation and beyond in Einstein-Cartan gravity, ” JCAP 05 (2024) 107, arXiv:2402.05358 [gr-qc]

  49. [57]

    Some simple theories of gravity with propagating torsion,

    Y. Mikura, V. Naso, and R. Percacci, “Some simple theories of gravity with propagating torsion, ”Phys. Rev. D 109 no. 10, (2024) 104071, arXiv:2312.10249 [gr-qc]

  50. [58]

    Starobinsky-like Inflationary Models as Avatars of No-Scale Supergravity,

    J. Ellis, D. V. Nanopoulos, and K. A. Olive, “Starobinsky-like Inflationary Models as Avatars of No-Scale Supergravity, ”JCAP 10 (2013) 009, arXiv:1307.3537 [hep-th]

  51. [59]

    Minimal Supergravity Models of Inflation,

    S. Ferrara, R. Kallosh, A. Linde, and M. Porrati, “Minimal Supergravity Models of Inflation, ”Phys. Rev. D 88 no. 8, (2013) 085038, arXiv:1307.7696 [hep-th]

  52. [60]

    Superconformal Inflationary 𝛼-Attractors,

    R. Kallosh, A. Linde, and D. Roest, “Superconformal Inflationary 𝛼-Attractors, ”JHEP 11 (2013) 198, arXiv:1311.0472 [hep-th]

  53. [61]

    Large field inflation and double 𝛼-attractors,

    R. Kallosh, A. Linde, and D. Roest, “Large field inflation and double 𝛼-attractors, ”JHEP 08 (2014) 052, arXiv:1405.3646 [hep-th]

  54. [62]

    𝛼-Attractors: Planck, LHC and Dark Energy,

    J. J. M. Carrasco, R. Kallosh, and A. Linde, “𝛼-Attractors: Planck, LHC and Dark Energy, ”JHEP 10 (2015) 147, arXiv:1506.01708 [hep-th]

  55. [63]

    Cosmological attractors from 𝛼-scale supergravity,

    D. Roest and M. Scalisi, “Cosmological attractors from 𝛼-scale supergravity, ”Phys. Rev. D 92 (2015) 043525, arXiv:1503.07909 [hep-th]

  56. [64]

    Single-field 𝛼-attractors,

    A. Linde, “Single-field 𝛼-attractors, ”JCAP 05 (2015) 003, arXiv:1504.00663 [hep-th]

  57. [65]

    Cosmological 𝛼-attractors and de Sitter landscape,

    M. Scalisi, “Cosmological 𝛼-attractors and de Sitter landscape, ”JHEP 12 (2015) 134, arXiv:1506.01368 [hep-th]

  58. [66]

    Unity of Cosmological Inflation Attractors,

    M. Galante, R. Kallosh, A. Linde, and D. Roest, “Unity of Cosmological Inflation Attractors, ”Phys. Rev. Lett. 114 no. 14, (2015) 141302, arXiv:1412.3797 [hep-th]

  59. [67]

    Pole inflation — Shift symmetry and universal corrections,

    B. J. Broy, M. Galante, D. Roest, and A. Westphal, “Pole inflation — Shift symmetry and universal corrections, ”JHEP 12 (2015) 149, arXiv:1507.02277 [hep-th]

  60. [68]

    Generalized Pole Inflation: Hilltop, Natural, and Chaotic Inflationary Attractors,

    T. Terada, “Generalized Pole Inflation: Hilltop, Natural, and Chaotic Inflationary Attractors, ”Phys. Lett. B 760 (2016) 674–680, arXiv:1602.07867 [hep-th]

  61. [69]

    Primordial black holes and induced gravitational waves from double-pole inflation,

    C. Fu and S.-J. Wang, “Primordial black holes and induced gravitational waves from double-pole inflation, ”JCAP 06 (2023) 012, arXiv:2211.03523 [astro-ph.CO] . 31

  62. [70]

    Pole inflation and primordial black holes formation in Starobinsky-like supergravity,

    S. Aoki, R. Ishikawa, and S. V. Ketov, “Pole inflation and primordial black holes formation in Starobinsky-like supergravity, ”Class. Quant. Grav. 40 no. 6, (2023) 065002, arXiv:2210.10348 [hep-th]

  63. [71]

    Pole inflation from non-minimal coupling to gravity,

    S. Karamitsos and A. Strumia, “Pole inflation from non-minimal coupling to gravity, ” JHEP 05 (2022) 016, arXiv:2109.10367 [hep-th]

  64. [72]

    Pole-induced Higgs inflation with hyperbolic Kähler geometries,

    C. Pallis, “Pole-induced Higgs inflation with hyperbolic Kähler geometries, ” JCAP 05 (2021) 043, arXiv:2103.05534 [hep-ph]

  65. [73]

    Pole N-flation,

    M. Dias, J. Frazer, A. Retolaza, M. Scalisi, and A. Westphal, “Pole N-flation, ”JHEP 02 (2019) 120, arXiv:1805.02659 [hep-th]

  66. [74]

    Pole inflation in Jordan frame supergravity,

    K. Saikawa, M. Yamaguchi, Y. Yamashita, and D. Yoshida, “Pole inflation in Jordan frame supergravity, ” JCAP 01 (2018) 031, arXiv:1709.03440 [hep-th]

  67. [75]

    Toward pole inflation and attractors in supergravity : Chiral matter field inflation,

    T. Kobayashi, O. Seto, and T. H. Tatsuishi, “Toward pole inflation and attractors in supergravity : Chiral matter field inflation, ”PTEP 2017 no. 12, (2017) 123B04, arXiv:1703.09960 [hep-th]

  68. [76]

    Linear Inflation from Running Kinetic Term in Supergravity,

    F. Takahashi, “Linear Inflation from Running Kinetic Term in Supergravity, ”Phys. Lett. B 693 (2010) 140–143, arXiv:1006.2801 [hep-ph]

  69. [77]

    Running Kinetic Inflation,

    K. Nakayama and F. Takahashi, “Running Kinetic Inflation, ”JCAP 11 (2010) 009, arXiv:1008.2956 [hep-ph]

  70. [78]

    Chaotic Inflation,

    A. D. Linde, “Chaotic Inflation, ”Phys. Lett. B 129 (1983) 177–181

  71. [79]

    Inflating and reheating the Universe with an independent affine connection,

    A. Salvio, “Inflating and reheating the Universe with an independent affine connection, ” Phys. Rev. D 106 no. 10, (2022) 103510, arXiv:2207.08830 [hep-ph]

  72. [80]

    Increase of 𝑛𝑠 in regularized pole inflation & Einstein-Cartan gravity,

    M. He, M. Hong, and K. Mukaida, “Increase of 𝑛𝑠 in regularized pole inflation & Einstein-Cartan gravity, ”arXiv:2504.16069 [astro-ph.CO]

  73. [81]

    The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and𝛬CDM Parameters,

    ACT Collaboration, T. Louis et al., “The Atacama Cosmology Telescope: DR6 Power Spectra, Likelihoods and𝛬CDM Parameters, ”arXiv:2503.14452 [astro-ph.CO]

  74. [82]

    The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models,

    ACT Collaboration, E. Calabrese et al., “The Atacama Cosmology Telescope: DR6 Constraints on Extended Cosmological Models, ”arXiv:2503.14454 [astro-ph.CO]

  75. [83]

    Planck 2018 results. X. Constraints on inflation,

    Planck Collaboration, Y. Akrami et al., “Planck 2018 results. X. Constraints on inflation, ”Astron. Astrophys. 641 (2020) A10, arXiv:1807.06211 [astro-ph.CO]

  76. [84]

    Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season,

    BICEP, Keck Collaboration, P. A. R. Ade et al., “Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season, ”Phys. Rev. Lett. 127 no. 15, (2021) 151301, arXiv:2110.00483 [astro-ph.CO]

  77. [85]

    Particle Production in the New Inflationary Cosmology,

    L. F. Abbott, E. Farhi, and M. B. Wise, “Particle Production in the New Inflationary Cosmology, ” Phys. Lett. 117B (1982) 29. 32

  78. [86]

    Baryon Asymmetry in Inflationary Universe,

    A. D. Dolgov and A. D. Linde, “Baryon Asymmetry in Inflationary Universe, ”Phys. Lett. 116B (1982) 329

  79. [87]

    Reheating after inflation,

    L. Kofman, A. D. Linde, and A. A. Starobinsky, “Reheating after inflation, ”Phys. Rev. Lett. 73 (1994) 3195–3198, arXiv:hep-th/9405187

  80. [88]

    Universe reheating after inflation,

    Y. Shtanov, J. H. Traschen, and R. H. Brandenberger, “Universe reheating after inflation, ”Phys. Rev. D51 (1995) 5438–5455, arXiv:hep-ph/9407247 [hep-ph]

  81. [89]

    Towards the theory of reheating after inflation,

    L. Kofman, A. D. Linde, and A. A. Starobinsky, “Towards the theory of reheating after inflation, ”Phys. Rev. D 56 (1997) 3258–3295, arXiv:hep-ph/9704452

  82. [90]

    Structure of resonance in preheating after inflation,

    P. B. Greene, L. Kofman, A. D. Linde, and A. A. Starobinsky, “Structure of resonance in preheating after inflation, ”Phys. Rev. D 56 (1997) 6175–6192, arXiv:hep-ph/9705347

  83. [91]

    Dynamics of symmetry breaking and tachyonic preheating,

    G. N. Felder, J. Garcia-Bellido, P. B. Greene, L. Kofman, A. D. Linde, and I. Tkachev, “Dynamics of symmetry breaking and tachyonic preheating, ”Phys. Rev. Lett. 87 (2001) 011601, arXiv:hep-ph/0012142

  84. [92]

    Tachyonic instability and dynamics of spontaneous symmetry breaking,

    G. N. Felder, L. Kofman, and A. D. Linde, “Tachyonic instability and dynamics of spontaneous symmetry breaking, ”Phys. Rev. D 64 (2001) 123517, arXiv:hep-th/0106179

  85. [93]

    Tachyonic preheating,

    L. Kofman, “Tachyonic preheating, ” in8th International Symposium on Particles Strings and Cosmology , pp. 167–182. 2001. arXiv:hep-ph/0107280

  86. [94]

    Violation of CP Invariance, C asymmetry, and baryon asymmetry of the universe,

    A. D. Sakharov, “Violation of CP Invariance, C asymmetry, and baryon asymmetry of the universe, ” Pisma Zh. Eksp. Teor. Fiz. 5 (1967) 32–35

  87. [95]

    How long before the end of inflation were observable perturbations produced?,

    A. R. Liddle and S. M. Leach, “How long before the end of inflation were observable perturbations produced?, ”Phys. Rev. D 68 (2003) 103503, arXiv:astro-ph/0305263

  88. [96]

    First CMB Constraints on the Inflationary Reheating Temperature,

    J. Martin and C. Ringeval, “First CMB Constraints on the Inflationary Reheating Temperature, ”Phys. Rev. D 82 (2010) 023511, arXiv:1004.5525 [astro-ph.CO]

  89. [97]

    Planck 2018 results. VI. Cosmological parameters,

    Planck Collaboration, N. Aghanim et al., “Planck 2018 results. VI. Cosmological parameters, ”Astron. Astrophys. 641 (2020) A6, arXiv:1807.06209 [astro-ph.CO] . [Erratum: Astron.Astrophys. 652, C4 (2021)]

  90. [98]

    Cosmological evolution of a torsion-induced quintaxion,

    E. W. Mielke and E. S. Romero, “Cosmological evolution of a torsion-induced quintaxion, ”Phys. Rev. D 73 (2006) 043521

  91. [99]

    Peccei-Quinn mechanism in gravity and the nature of the Barbero-Immirzi parameter,

    S. Mercuri, “Peccei-Quinn mechanism in gravity and the nature of the Barbero-Immirzi parameter, ” Phys. Rev. Lett. 103 (2009) 081302, arXiv:0902.2764 [gr-qc]

  92. [100]

    Interaction of the Barbero-Immirzi Field with Matter and Pseudo-Scalar Perturbations,

    S. Mercuri and V. Taveras, “Interaction of the Barbero-Immirzi Field with Matter and Pseudo-Scalar Perturbations, ”Phys. Rev. D 80 (2009) 104007, arXiv:0903.4407 [gr-qc]

  93. [101]

    A solution of the strong CP problem via the Peccei-Quinn mechanism through the Nieh-Yan modified gravity and cosmological implications,

    M. Lattanzi and S. Mercuri, “A solution of the strong CP problem via the Peccei-Quinn mechanism through the Nieh-Yan modified gravity and cosmological implications, ”Phys. Rev. D 81 (2010) 125015, arXiv:0911.2698 [gr-qc] . 33

  94. [102]

    Axions in gravity with torsion,

    O. Castillo-Felisola, C. Corral, S. Kovalenko, I. Schmidt, and V. E. Lyubovitskij, “Axions in gravity with torsion, ”Phys. Rev. D 91 no. 8, (2015) 085017, arXiv:1502.03694 [hep-ph]

  95. [103]

    On the strong-CP problem and its axion solution in torsionful theories,

    G. K. Karananas, “On the strong-CP problem and its axion solution in torsionful theories, ” Eur. Phys. J. C 78 no. 6, (2018) 480, arXiv:1805.08781 [hep-th]

  96. [104]

    Weyl-invariant Einstein-Cartan gravity: unifying the strong CP and hierarchy puzzles,

    G. K. Karananas, M. Shaposhnikov, and S. Zell, “Weyl-invariant Einstein-Cartan gravity: unifying the strong CP and hierarchy puzzles, ”JHEP 11 (2024) 146, arXiv:2406.11956 [hep-th]

  97. [105]

    Axions and the Strong CP Problem,

    J. E. Kim and G. Carosi, “Axions and the Strong CP Problem, ” Rev. Mod. Phys. 82 (2010) 557–602, arXiv:0807.3125 [hep-ph] . [Erratum: Rev.Mod.Phys. 91, 049902 (2019)]

  98. [106]

    No-scale Brans-Dicke Gravity – ultralight scalar boson & heavy inflaton,

    M. Hong, K. Mukaida, and T. T. Yanagida, “No-scale Brans-Dicke Gravity – ultralight scalar boson & heavy inflaton, ”arXiv:2503.18648 [hep-ph]

  99. [107]

    Hilltop inflation,

    L. Boubekeur and D. H. Lyth, “Hilltop inflation, ” JCAP 07 (2005) 010, arXiv:hep-ph/0502047

  100. [108]

    Natural metric-affine inflation,

    A. Racioppi and A. Salvio, “Natural metric-affine inflation, ” JCAP 06 (2024) 033, arXiv:2403.18004 [hep-ph]

  101. [109]

    ̃𝜉-attractors in metric-affine gravity,

    A. Racioppi, “ ̃𝜉-attractors in metric-affine gravity, ”arXiv:2411.08031 [gr-qc]

  102. [110]

    Symmetry-breaking inflation in non-minimal metric-affine gravity,

    I. D. Gialamas and A. Racioppi, “Symmetry-breaking inflation in non-minimal metric-affine gravity, ” arXiv:2412.17738 [gr-qc]

  103. [111]

    Leptogenesis via Axion Oscillations after Inflation,

    A. Kusenko, K. Schmitz, and T. T. Yanagida, “Leptogenesis via Axion Oscillations after Inflation, ”Phys. Rev. Lett. 115 no. 1, (2015) 011302, arXiv:1412.2043 [hep-ph]

  104. [112]

    Leptogenesis from left-handed neutrino production during axion inflation,

    P. Adshead and E. I. Sfakianakis, “Leptogenesis from left-handed neutrino production during axion inflation, ”Phys. Rev. Lett. 116 no. 9, (2016) 091301, arXiv:1508.00881 [hep-ph]

  105. [113]

    Cosmological Aspects of Spontaneous Baryogenesis,

    A. De Simone and T. Kobayashi, “Cosmological Aspects of Spontaneous Baryogenesis, ”JCAP 08 (2016) 052, arXiv:1605.00670 [hep-ph]

  106. [114]

    Calculation of particle production by Nambu Goldstone bosons with application to inflation reheating and baryogenesis,

    A. Dolgov and K. Freese, “Calculation of particle production by Nambu Goldstone bosons with application to inflation reheating and baryogenesis, ”Phys. Rev. D 51 (1995) 2693–2702, arXiv:hep-ph/9410346

  107. [115]

    Fermion production during and after axion inflation,

    P. Adshead and E. I. Sfakianakis, “Fermion production during and after axion inflation, ”JCAP 11 (2015) 021, arXiv:1508.00891 [hep-ph]

  108. [116]

    Gauge Field and Fermion Production during Axion Inflation,

    V. Domcke and K. Mukaida, “Gauge Field and Fermion Production during Axion Inflation, ”JCAP 11 (2018) 020, arXiv:1806.08769 [hep-ph]

  109. [117]

    Chiral Gravitational Waves from Chiral Fermions,

    M. M. Anber and E. Sabancilar, “Chiral Gravitational Waves from Chiral Fermions, ”Phys. Rev. D 96 no. 2, (2017) 023501, arXiv:1607.03916 [hep-th]

  110. [118]

    Quantum scale invariance, cosmological constant and hierarchy problem,

    M. Shaposhnikov and D. Zenhausern, “Quantum scale invariance, cosmological constant and hierarchy problem, ”Phys. Lett. B 671 (2009) 162–166, arXiv:0809.3406 [hep-th] . 34

  111. [119]

    On the Gravitational Origin of the QCD Axion,

    G. K. Karananas, M. Shaposhnikov, and S. Zell, “On the Gravitational Origin of the QCD Axion, ” arXiv:2506.11836 [hep-th]

  112. [120]

    Large Nongaussianity in Axion Inflation,

    N. Barnaby and M. Peloso, “Large Nongaussianity in Axion Inflation, ” Phys. Rev. Lett. 106 (2011) 181301, arXiv:1011.1500 [hep-ph]

  113. [121]

    Phenomenology of a Pseudo-Scalar Inflaton: Naturally Large Nongaussianity,

    N. Barnaby, R. Namba, and M. Peloso, “Phenomenology of a Pseudo-Scalar Inflaton: Naturally Large Nongaussianity, ”JCAP 04 (2011) 009, arXiv:1102.4333 [astro-ph.CO]

  114. [122]

    Path Integral for Gauge Theories with Fermions,

    K. Fujikawa, “Path Integral for Gauge Theories with Fermions, ” Phys. Rev. D 21 (1980) 2848. [Erratum: Phys.Rev.D 22, 1499 (1980)]

  115. [123]

    Circular Polarization of Primordial Gravitational Waves in String-inspired Inflationary Cosmology,

    M. Satoh, S. Kanno, and J. Soda, “Circular Polarization of Primordial Gravitational Waves in String-inspired Inflationary Cosmology, ”Phys. Rev. D 77 (2008) 023526, arXiv:0706.3585 [astro-ph]

  116. [124]

    Gauge Field Production in Axion Inflation: Consequences for Monodromy, non-Gaussianity in the CMB, and Gravitational Waves at Interferometers,

    N. Barnaby, E. Pajer, and M. Peloso, “Gauge Field Production in Axion Inflation: Consequences for Monodromy, non-Gaussianity in the CMB, and Gravitational Waves at Interferometers, ”Phys. Rev. D 85 (2012) 023525, arXiv:1110.3327 [astro-ph.CO] . 35

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