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REVIEW 3 major objections 5 minor 49 references

On dark sector scalar field theories driven by cosmological $c$-fields

T0 review · 3 major / 5 minor · reviewed 2026-08-01 · deepseek-v4-flash

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Pith's one-line read Hoyle–Narlikar creation fields reduce to generalized Chaplygin scalar theory

desk verdict The algebra is internally consistent, but the advertised embedding of HN c-field dynamics into a GCG-like scalar theory is not established: the c-field wave equation is never imposed, and the free deformation is doing all the work. read the letter →

arxiv 2607.15897 v1 pith:NPY2LOUR submitted 2026-07-17 gr-qc

Alex E. Bernardini , Orfeu Bertolami This is my paper · ORCID
classification gr-qc MSC 83F05 PACS 98.80.-k04.20.-q
keywords Hoyle–NarlikarcreationfieldgeneralizedChaplygingasscalarcosmologyHamilton–JacobireconstructiondarksectorsoundspeedHubbletension
topics The Hubble Tension
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

The paper tries to show that the negative-energy creation field (c-field) of Hoyle–Narlikar cosmology is not an independent component but can be absorbed into a twin scalar field description whose background dynamics match the generalized Chaplygin gas (GCG). Using a first-order Hamiltonian reconstruction method, the authors derive a map between the original scalar field and a deformed one, with the c-field encoded in the deformation. The central identity is H²(φ) = H²(ϕ) − ċ²/3, which isolates how the creation field changes the Hubble rate. With a tanh-style deformation, the effective fluid has a strictly positive squared sound speed across the whole cosmic history. If correct, creation-field cosmologies become a subclass of GCG-like scalar dark-sector theories, relaxing standard GCG constraints and offering a unified dark-matter–dark-energy picture.

What carries the argument

The central object is the first-order Hamiltonian (Hamilton–Jacobi) reconstruction of scalar-field cosmology, in which the Hubble rate is a function H(ϕ) = y(ϕ) and the field velocity is ˙ϕ = y_ϕ. The creation field enters through a deformation map φ(ϕ) between two canonical scalar fields; all c-field effects are condensed into the single function φ_ϕ = dφ/dϕ. That function, via ċ² = (3/2) y_ϕ² (1 − φ_ϕ²), determines how much the Hubble rate is shifted from H(ϕ) to H(φ) and generates the effective energy density and pressure of the unified fluid.

What would settle it

Take the tanh and linear deformations, compute ċ(a) from the reconstructed identity ċ² = (3/2) y_ϕ² (1 − φ_ϕ²), and substitute the resulting c(t) into the Hoyle–Narlikar wave equation □c + (1/6) R c + c³ = source. If the equation is not satisfied for those solutions, the claimed embedding of creation-field cosmology into GCG-like scalar theories collapses.

Watch

Extended reading notes

Core claim

The authors claim that the HN c-field dynamics is encompassed by the GCG equation of state through an equivalent modified scalar field theory. Concretely, they construct a mapping between two scalar fields, ϕ (GCG) and φ (c-field-modified), linked by the constraints ċ² = (3/2) y_ϕ² (1 − φ_ϕ²) and H²(φ) = H²(ϕ) − ċ²/3. For a linear rescaling φ(ϕ) = ℓϕ they obtain explicit ρφ(a) and pφ(a) formulas, and for a kink-like deformation φ(ϕ) ∝ ln cosh(...) they find c_s² > 0 for the entire expansion. The paper presents this as evidence that creation-field cosmologies can be embedded in a broader scalar-field family that subtly modifies the late-time Hubble expansion rate while keeping linear perturba

Load-bearing premise

The equivalence assumes that arbitrarily chosen smooth deformations φ(ϕ) automatically give valid Hoyle–Narlikar creation-field solutions, because the full creation-field wave equation (□c + (1/6)Rc + c³ = source) is never imposed or verified after reconstruction.

Editorial extensions

If this is right

  • If the equivalence holds, creation-field cosmologies can be studied as ordinary scalar-field dark-energy models without tracking a separate negative-energy field.
  • The GCG parameter space is effectively widened: a whole family of scalar-field deformations (not just the standard GCG) yields observationally plausible equations of state.
  • Late-time modifications to H from the c-field could be tested against the observed Hubble expansion, potentially addressing the H0 tension.
  • For the tanh deformation, linear perturbations remain stable (c_s² > 0) through the whole cosmic history, unlike the simpler linear rescaling.
  • The construction provides a route to unify dark matter and dark energy in a single dynamical component with a built-in creation mechanism.

Reading between the lines

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

  • The paper never solves the full HN wave equation for c after fixing a deformation; it only imposes the reconstructed relation ċ². A direct check of whether the selected φ(ϕ) produces a c-field satisfying the HN creation equation would settle whether the embedding is genuine or just a reparameterization of the Friedmann equations.
  • Because φ_ϕ is treated as a free function, the method could generate many new scalar-field potentials and equations of state; one could scan other deformation families besides linear and tanh for even more favorable stability or observational properties.
  • The c-field contribution identified here behaves as an early-time matter-like subtraction that fades at late times, so the framework might be adapted to models where the dark sector changes behavior at a specific redshift scale — a testable signature.
  • The identification of c_s² with the propagation speed of perturbations suggests a direct observational handle: constraints on the dark-sector sound speed from structure formation could discriminate between different φ(ϕ) choices.
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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

3 major / 5 minor

Summary. The paper proposes a formal correspondence between Hoyle-Narlikar (HN) creation-field cosmology and scalar-field dark-sector models, specifically the generalized Chaplygin gas (GCG). Starting from the Friedmann equations with a c-field, the authors define an auxiliary 'twin' scalar field φ and potential U through Eqs. (23)–(24), so that the c-field contribution is absorbed. Using a first-order Hamilton–Jacobi reconstruction with H(φ)=w(φ), they derive modified energy density and pressure for two choices of deformation, φϕ=ℓ and φϕ=tanh(√(3/2)ℓ(1+α)ϕ), and compute the equation-of-state parameter, sound speed, and cosmographic parameters q, j, s. The paper claims that HN c-field dynamics is encompassed by a GCG-like scalar-field theory and that the deformed-field case yields stable linear perturbations with positive c_s².

Significance. If the advertised embedding into full HN dynamics were established, this would provide a useful dictionary between creation-field cosmology and scalar-field dark-sector models, potentially offering a new way to generate modified Hubble-rate evolutions. The algebraic reconstruction is explicit, the analytic formulas for ρφ and pφ are given in Eqs. (57) and (60), and the two deformation families are worked out in detail. However, the central claim goes beyond what is actually demonstrated: the construction uses only the first-order Friedmann equations and never imposes the HN c-field wave equation, Eq. (6), while the stability conclusion rests on an identification of the scalar-field sound speed with the barotropic dp/dρ. The paper therefore contributes a formal reparameterization of Friedmann cosmologies, but the HN-specific dynamical content and the perturbation-stability claim require substantial additional support.

major comments (3)
  1. [Sec. III.B and Eq. (6)] The central claim that 'the HN c-field dynamics is shown to be encompassed' by a scalar-field theory is not established because the HN c-field wave equation, Eq. (6), is never imposed or solved. The construction in Eqs. (23)–(24) uses only ˙c², and Eq. (44) determines ˙c² from an arbitrary deformation φ(ϕ). The full field equation □c+(1/6)Rc+c³=Σ is a second-order dynamical constraint that is not implied by the first-order Friedmann equations (10)–(11). Without substituting the reconstructed c(t) into Eq. (6), or otherwise fixing the source Σ, the two examples (φϕ=ℓ and the tanh deformation) are not shown to be solutions of the HN theory. The sentence in Sec. III C3 that φϕ is 'a free degree of freedom just constrained by the inclusion of the c-field DoF' explicitly concedes that this constraint is left unspecified. The authors should either impose Eq. (6) for the examples and verify con
  2. [Sec. III C2 and Conclusions] The stability claim is based on identifying the squared sound speed with c_s²=dp/dρ and asserting that c_s²>0 implies stable propagation of linear perturbations. This identification is not valid for the canonical scalar field φ constructed in the paper. For a canonical scalar field with Lagrangian X−U(φ), the propagation speed of scalar perturbations is unity (in c=1 units), not the barotropic expression dp/dρ. The quantity dp/dρ is the adiabatic speed of a fluid with p=p(ρ), but the scalar field is not barotropic; its perturbed pressure contains intrinsic entropy perturbations. Therefore the figures in Sec. III C2 showing c_s²>0 do not demonstrate stability of the φ-field perturbations. A proper perturbation analysis of the φ-field (or a clearly specified k-essence-type effective action with the corresponding sound speed) is needed to support the stability claim in the abstract and conc
  3. [Sec. III C3, Eq. (63)] The predictive content of the construction is questionable because the c-field contribution to the Hubble rate, Eq. (63), is fixed by the freely chosen deformation φ(ϕ). Since the paper states that φϕ is a free degree of freedom, the resulting modifications to the equation of state, the sign of dp/dρ, and the late-time Hubble behavior are inputs of the reconstruction rather than consequences of HN c-field dynamics. In particular, the positive sound speed in the tanh example is a property of the chosen deformation on a GCG background, not a generic feature of creation-field cosmology. The authors should clarify what physical or dynamical constraints from the HN theory (e.g., Eq. (6)) reduce this freedom; otherwise the statement that c-field cosmologies are 'encompassed' by the scalar-field framework is tautological.
minor comments (5)
  1. [Eq. (58)] In Eq. (58), the notation 'y²(a) = 2/3 ρφ(a)' is confusing: the quantity on the right is the original GCG energy density ρϕ, not the φ-field density ρφ defined in Eq. (57). Rename to avoid an apparent inconsistency.
  2. [Figures 1, 3, 5] Several figure captions contain the duplicated phrase 'Results are for for ...' (e.g., Figs. 1 and 3). Also, Fig. 5 uses ℓ values (0.02–0.2) that differ from those in Figs. 1–4; the choice of parameter range should be explained or unified.
  3. [Sec. III.A] The unit convention introduced after Eq. (36), 'κ/2 = 4πG ≡ 1', is nonstandard and could confuse readers; it implies κ=2 in the Friedmann equations. A one-sentence clarification that this is a convenient normalization would help.
  4. [Sec. II.B] The phrase 'evolves as a subtracting matter contribution' (before Eq. (64)) should read 'subtractive' or 'negative matter-like contribution'.
  5. [References] Reference [4] (Singh et al., arXiv:2510.11762) appears in the bibliography but does not seem to be cited in the text. Please check the citation list.

Circularity Check

3 steps flagged · score 8.0 of 10

The claimed embedding of HN c-field dynamics is definitional: Eq. (44) fixes the c-field contribution from an arbitrary free deformation φϕ, and the HN wave equation (6) is never imposed, so the Hubble, EoS and sound-speed outputs are inputs.

  1. self definitional [Sec. III B, Eqs. (44)-(46); Sec. III C3]
    "˙c2 = 3/2 y2ϕ(1 − φ2ϕ) (44) ... Of course, as it was emphasized, φϕ is a free degree of freedom just constrained by the inclusion of the c-field DoF in the formalism."

    Eq. (44) is only a consistency condition of the redefinitions (23)-(24), not a consequence of HN dynamics. Since φϕ is explicitly free, choosing it fixes ċ²; Eq. (46) then fixes H(φ), and Eqs. (57)-(60) fix ρφ, pφ, the EoS and c_s². The advertised 'c-field contribution to H' is therefore the chosen φϕ in disguise, not an independently derived prediction.

  2. fitted input called prediction [Sec. III C.2 (Eq. 61) and Fig. 3 discussion]
    "The above results, as it shall be discussed in the following, despite adapting to modified ΛCDM theories, are problematic in providing conditions for the stable propagation of linear perturbations ( c2 s > 0). For this reason, a more elaborate solution is proposed. ... The most relevant feature identified in Fig. 3 concerns the stability of the propagation of linear perturbations, that is c2 s > 0, for the entire universe expansion phase."

    The tanh deformation (61) is introduced specifically to cure the c_s² < 0 problem of the ℓ rescaling, and then c_s² > 0 is presented as a result. Because φϕ is admitted to be free (Sec. III C3), the stability outcome is selected by the Ansatz rather than predicted, so the stability claim reduces to a choice of input.

1 more flagged steps
  1. other [Sec. II B, Eq. (6), vs. Secs. III B-C]
    "□c + 1/6 Rc + c3 = X a Z Ao+δAo Ao δ4(X, A))p −g(A) dτa, (6) ... solutions for c(t) can be straightforwardly obtained from Eq. (10) once one has ρ ≡ ρ(a)."

    The equation that actually defines HN c-field dynamics is the wave equation (6), but the paper never imposes or solves it. Instead c(t) is taken from the Friedmann equation (10) or, through Eq. (44), from the freely chosen φϕ. With the RHS source unspecified in the derivation, any background satisfying the reparameterized Friedmann equations can be dressed as a 'c-field', so the claimed embedding of HN dynamics is a reparameterization, not a derivation from HN theory.

full rationale

The paper is internally consistent in constructing, for a GCG ϕ-field and any deformation φ(ϕ), a function ċ²(a) that closes the Friedmann equations (19)-(20); Eq. (44) is exactly that construction. But this is why the headline results are not predictions: the modified Hubble rate (Eqs. 46 and 63), the reconstructed ρφ and pφ (Eqs. 57 and 60), their EoS and the sign of c_s² all depend on the free function φϕ, which the manuscript explicitly calls 'a free degree of freedom'. The only link to HN cosmology proper is the c-field wave equation (6), and that equation is neither solved nor checked. The self-citations [36,39] supply the reconstruction formalism and deformation technique but are not the source of the circularity; the specific reduction is the definitional relation ċ² = (3/2)yϕ²(1−φϕ²). Because the central claim 'HN c-field dynamics is shown to be encompassed by the GCG equation of state' reduces, by the paper's own equations, to a free functional choice plus a Friedmann-level reparameterization, the score is 8.

Assumptions & free parameters 3 free parameters · 6 assumptions · 0 invented entities

The central construction treats the c-field as absorbable into a redefined scalar field via Eqs. (23)-(24). This is exact at the level of the Friedmann equations, but the paper then assumes that any chosen φ(ϕ) represents a valid HN solution, which is not checked. The free deformation φ(ϕ) and the amplitude ℓ are the main new degrees of freedom; the GCG parameters are inherited from prior fits.

free parameters (3)
  • ℓ (deformation amplitude) = varied: 0.80, 0.90, 0.95 (rescaled); 0.8, 1.0, 1.2 (deformed); 0.02–0.2 (Fig. 5)
    Controls the magnitude of the c-field contribution to H, the EoS, and the sound speed; chosen by hand and not derived from HN dynamics.
  • φ(ϕ) deformation function = ℓϕ or sqrt(2/3)[ℓ(1+α)]^{-1} ln cosh(sqrt(3/2) ℓ(1+α)ϕ)
    Free functional input; the paper explicitly says 'φϕ is a free degree of freedom'. All novel results depend on this choice.
  • GCG parameters ΩΛ, α = ΩΛ=0.6825 (Planck); α=0.2 and 0.8
    Inherited from prior fits/illustrations, not fitted here, but the central plots and the sound-speed conclusions depend on these values.
assumptions (6)
  • domain assumption Hoyle-Narlikar field equations (Eq. 7) with the c-field source are a valid description of gravitational dynamics.
    All subsequent cosmology is built on this modified Einstein equation; no independent validation is given in the paper.
  • domain assumption Flat FRW metric and homogeneous scalar fields ϕ, c, and φ, with cµ = δ0µ ċ.
    The background analysis assumes spatial homogeneity; this is standard for cosmological models but restricts the scope.
  • domain assumption The GCG equation of state and its scalar-field representation (Eqs. 28-34) are taken from prior literature.
    The paper relies on the established GCG potential and solution without re-deriving them.
  • standard math The twin field defined by φdot² = ϕdot² - (2/3)ċ² and U = V - ċ²/6 satisfies the scalar-field equation (25).
    This is a derived algebraic identity from Eqs. (21)-(24); it holds when the original field equation is satisfied.
  • ad hoc to paper Stability of linear perturbations is determined by the sign of the effective fluid sound speed c_s² = dp/dρ.
    For a canonical scalar field the perturbation sound speed is 1, not dp/dρ; the paper does not justify using the adiabatic fluid sound speed.
  • ad hoc to paper Any freely chosen deformation φ(ϕ) yields a valid HN c-field solution.
    The c-field equation (6) is never imposed after reconstruction; the paper assumes the Friedmann-level mapping is sufficient.

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Cite this review

Pith. "Pith review of On dark sector scalar field theories driven by cosmological $c$-fields." pith.science (2026). https://pith.science/paper/NPY2LOUR

@misc{pith2026260715897,
  author       = {Pith},
  title        = {Pith review of: On dark sector scalar field theories driven by cosmological $c$-fields},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/NPY2LOUR}},
  note         = {Machine review of arXiv:2607.15897}
}
abstract

The interplay of Hoyle-Narlikar (HN) creation field cosmology and scalar field models for the dark sector, including the generalized Chaplygin Gas (GCG), is investigated . Though originating from distinct theoretical frameworks, both the inclusion and the non-inclusion of the creation field degree of freedom (DoF) involve a scalar DoF, which addresses some of the limitations of the standard $\Lambda$CDM model. Using a Lagrangian scalar field formulation and the first-order Hamiltonian reconstruction method, the HN $c$-field dynamics is shown to be encompassed by the GCG equation of state through an equivalent modified scalar field theory. Late-time acceleration and stability of linear perturbations are derived within this unified description. Our results suggest that creation field cosmologies may be embedded in a broader class of scalar field models which encompasses subtle modifications to the Hubble expansion rate and related physical observables.

Figures

Figures reproduced from arXiv: 2607.15897 by the authors.

Figure 1
Figure 1. FIG. 1 [PITH_FULL_IMAGE:figures/full_fig_p015_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2 [PITH_FULL_IMAGE:figures/full_fig_p016_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3 [PITH_FULL_IMAGE:figures/full_fig_p017_3.png] view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: FIG. 4 [PITH_FULL_IMAGE:figures/full_fig_p018_4.png]
Figure 5
Figure 5. Figure 5: FIG. 5 [PITH_FULL_IMAGE:figures/full_fig_p019_5.png]

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Reference graph

Works this paper leans on

49 extracted references

  1. [1]

    The simplest constraint which can be considered is given by a re-scaled scalar field, φ(ϕ) = ℓϕ, (56) where ℓ is an arbitrary constant with 0 < ℓ <1

    Results for a re-scaled scalar field: φϕ = ℓ. The simplest constraint which can be considered is given by a re-scaled scalar field, φ(ϕ) = ℓϕ, (56) where ℓ is an arbitrary constant with 0 < ℓ <1. The energy density dependence on the scale factor, ρφ(a), can be straightforwardly iden- tified from Eqs. (39) and (45), as ρφ(a) = 3 2 w2(a) = 3 2 y2(a) − 3 4 y...

  2. [2]

    More suitable results can be obtained from topologically deformed scalar field theories [39, 40] related by Eq

    Results for a deformed scalar field: φϕ = tanh( p 3/2ℓ(1 + α)ϕ). More suitable results can be obtained from topologically deformed scalar field theories [39, 40] related by Eq. (43). That is the case of a kink-like connection between φ- and ϕ- theories given by a scalar field deformation φ(ϕ) = r 2 3 1 ℓ(1 + α) ln " cosh r 3 2 ℓ(1 + α)ϕ !# , (61) which, o...

  3. [3]

    This suggests the modified scalar field theories pa- rameterized by c-fields as potential drivers of Hubble expansion rate modifications at late times

    The contribution to the Hubble expansion rate From the previous results, one notices that, for deformed scalar fields, and even for re- scaled fields, the early time dark sector contributions remains unaffected, with cosmological changes being manifest at late times. This suggests the modified scalar field theories pa- rameterized by c-fields as potential...

    2022

  4. [4]

    The Early Universe ; Addison-Wesley: Redwood City, CA, USA, 1990

    Kolb, E.W.; Turner, M.S. The Early Universe ; Addison-Wesley: Redwood City, CA, USA, 1990

    1990

  5. [5]

    A New Model for the Expanding Universe

    Hoyle, F. A New Model for the Expanding Universe. Mon. Not. R. Astron. Soc. 1948, 108, 352

    1948

  6. [6]

    The Steady-State Theory of the Expanding Universe

    Bondi, H.; Gold, T. The Steady-State Theory of the Expanding Universe. Mon. Not. R. Astron. Soc. 1948, 108, 252

    1948

  7. [7]

    The cosmic consequences and the constraints on HN-gravity.arXiv 2025, arXiv:2510.11762

    Singh, J.K.; Aggarwal, S.; Shaily; Shabani, H.; Santos, J.R.L. The cosmic consequences and the constraints on HN-gravity.arXiv 2025, arXiv:2510.11762

    arXiv 2025

  8. [8]

    On the avoidance of singularities in C-field cosmology

    Hoyle, F.; Narlikar, J.V. On the avoidance of singularities in C-field cosmology. Proc. R. Soc. Lond. A 1964, 278, 465

    1964

Show all 49 references
  1. [9]

    C-field as a direct particle field

    Hoyle, F.; Narlikar, J.V. C-field as a direct particle field. Proc. Roy. Soc. A 1964, 282, 178

    1964

  2. [10]

    A new theory of gravitation

    Hoyle, F.; Narlikar, J.V. A new theory of gravitation. Proc. R. Soc. Lond. A 1964, 282, 191

    1964

  3. [11]

    A Generalized Hoyle-Narlikar Particle Theory

    Mcintosh, C.A. A Generalized Hoyle-Narlikar Particle Theory. Nature 1970, 226, 339

    1970

  4. [12]

    A conformal theory of gravitation

    Hoyle, F.; Narlikar, J.V. A conformal theory of gravitation. Proc. R. Soc. Lond. A 1966, 294, 138

    1966

  5. [13]

    P. C. W. Davies, Hoyle-Narlikar Theory of Gravitation, Nature 1970, 228, 270

    1970

  6. [14]

    Singularity and matter creation in cosmological models

    Narlikar, J.V. Singularity and matter creation in cosmological models. Nat. Phys. Sci. 1973, 242, 135

    1973

  7. [15]

    Creation-field cosmology: A possible solution to singularity, horizon, and flatness problems

    Narlikar, J.V.; Padmanabhan, T. Creation-field cosmology: A possible solution to singularity, horizon, and flatness problems. Phys. Rev. D 1985, 32, 1928. 21

    1985

  8. [16]

    C-field cosmological model in higher dimensions

    Chatterjee, S.; Banerjee, A. C-field cosmological model in higher dimensions. Gen. Rel. Grav. 2004, 36, 303

    2004

  9. [17]

    C-field cosmological model for barotropic fluid distribution with varying Λ in FR W space-time.Int

    Bali, R.; Saraf, S. C-field cosmological model for barotropic fluid distribution with varying Λ in FR W space-time.Int. J. Theor. Phys. 2013, 52, 1645

    2013

  10. [18]

    Creation field cosmological models for dust distribution and time dependent cosmo- logical term (Λ) in Bianchi type II space-time

    Bali, R. Creation field cosmological models for dust distribution and time dependent cosmo- logical term (Λ) in Bianchi type II space-time. Inter. J. Geom. Meth. Mod. Phys. 2022, 19, 2250233

    2022

  11. [19]

    LRS Bianchi Type I in C-field cosmology with varying Λ( t)

    Malekolkalami, B.; Khalafi, G.H. LRS Bianchi Type I in C-field cosmology with varying Λ( t). Bulg. J. Phys. 2018, 45, 374

    2018

  12. [20]

    Gravitational wave background in the quasi-steady state cosmology

    Narlikar, J.V.; Dhurandhar, S.V.; Vishwakarma, R.G.; Valluri, S.R.; Auddy, S. Gravitational wave background in the quasi-steady state cosmology. MNRAS 2015, 451, 1390

    2015

  13. [21]

    Mach’s principle and the creation of matter

    Hoyle, F.; Narlikar, J.V. Mach’s principle and the creation of matter. Proc. Roy. Soc. A 1962,270 , 334

    1962

  14. [22]

    On the effects of the non-conservation of baryons in cosmology

    Hoyle, F.; Narlikar, J.V. On the effects of the non-conservation of baryons in cosmology. Proc. Roy. Soc. A 1966, 290, 143

    1966

  15. [23]

    Inho- mogeneities in the Microwave Background Radiation interpreted within the framework of the Quasi-Steady State Cosmology

    Narlikar, J.V.; Vishwakarma, R.G.; Hajian, A.; Souradeep, T.; Burbidge, G.; Hoyle, F. Inho- mogeneities in the Microwave Background Radiation interpreted within the framework of the Quasi-Steady State Cosmology. Astrophys. J. 2003, 585, 1

    2003

  16. [24]

    Further astrophysical quantities expected in a quasi- steady state Universe

    Hoyle, F.; Burbidge, G.; Narlikar, J.V. Further astrophysical quantities expected in a quasi- steady state Universe. Astron. Astrophys. 1994, 289, 729

    1994

  17. [25]

    An alternative to quintessence

    Kamenshchik, A.; Moschella, U.; Pasquier, V. An alternative to quintessence. Phys. Lett. B 2001, 511, 265

    2001

  18. [26]

    Generalized Chaplygin gas, accelerated expansion, and dark-energy-matter unification

    Bento, M.C.; Bertolami, O.; Sen, A.A. Generalized Chaplygin gas, accelerated expansion, and dark-energy-matter unification. Phys. Rev. D 2002, 66, 043507

    2002

  19. [27]

    Unification of Dark Matter and Dark Energy: The Inhomogeneous Chaplygin Gas

    Bili´ c, N.; Tupper, G.B.; Viollier, R.D. Unification of Dark Matter and Dark Energy: The Inhomogeneous Chaplygin Gas. Phys. Lett. B 2002, 535, 17

    2002

  20. [28]

    WMAP constraints on the generalized Chaplygin gas 22 model

    Bento, M.C.; Bertolami, O.; Sen, A.A. WMAP constraints on the generalized Chaplygin gas 22 model. Phys. Lett. B 2003, 575, 172

    2003

  21. [29]

    Generalized Chaplygin gas and CMBR constraints

    Bento, M.C.; Bertolami, O.; Sen, A.A. Generalized Chaplygin gas and CMBR constraints. Phys. Rev. D 2003, 67, 063003

    2003

  22. [30]

    Gamma-ray bursts as dark energy-matter probes in the context of the generalized Chaplygin gas model

    Bertolami, O.; Silva, P.T. Gamma-ray bursts as dark energy-matter probes in the context of the generalized Chaplygin gas model. Mon. Not. Roy. Astron. Soc. 2006, 365, 1149

    2006

  23. [31]

    Generalized Chaplygin gas model, supernovae, and cosmic topology

    Bento, M.C.; Bertolami, O.; Rebou¸ cas, M.J.; Silva, P.T. Generalized Chaplygin gas model, supernovae, and cosmic topology. Phys. Rev. D 2006, 73, 043504

    2006

  24. [32]

    A Quasi-Steady State Cosmological Model with Cre- ation of Matter

    Hoyle, F.; Burbidge, G.; Narlikar, J.V. A Quasi-Steady State Cosmological Model with Cre- ation of Matter. Astrophys. J. 1993, 410, 437

    1993

  25. [33]

    Astrophysical Deductions from the Quasi Steadystate Cosmology

    Hoyle, F.; Burbidge, G.; Narlikar, J.V. Astrophysical Deductions from the Quasi Steadystate Cosmology. Mon. Not. R. Astron. Soc. 1994, 267, 1007

    1994

  26. [34]

    The basic theory underlying the quasisteady state cosmology

    Hoyle, F.; Burbidge, G.; Narlikar, J.V. The basic theory underlying the quasisteady state cosmology. Proc. R. Soc. Lond. A 1995, 448, 191

    1995

  27. [35]

    A Different Approach to Cosmology ; Cambridge Uni- versity Press: Cambridge, UK, 2000

    Hoyle, F.; Burbidge, G.; Narlikar, J.V. A Different Approach to Cosmology ; Cambridge Uni- versity Press: Cambridge, UK, 2000

    2000

  28. [36]

    Mach’s principle and the creation of matter

    Hoyle, F.; Narlikar, J.V. Mach’s principle and the creation of matter. Proc. R. Soc. Lond. A 1963, 273, 1–11

    1963

  29. [37]

    The quasi-steady state cosmology: Analytical solutions of field equations and their relationship to observations

    Sachs, R.; Narlikar, J.V.; Hoyle, F. The quasi-steady state cosmology: Analytical solutions of field equations and their relationship to observations. Astron. Astrophys. 1996, 313, 703

    1996

  30. [38]

    Cosmology and action-at-a-distance electrodynamics

    Hoyle, F.; Narlikar, J.V. Cosmology and action-at-a-distance electrodynamics. Rev. Mod. Phys. 1995, 67, 113

    1995

  31. [39]

    The Hamiltonian formalism for scalar fields coupled to gravity in a cosmological background

    Bernardini, A.E.; Bertolami, O. The Hamiltonian formalism for scalar fields coupled to gravity in a cosmological background. Ann. Phys. 2013, 338, 1

    2013

  32. [40]

    Jerk, snap, and the cosmological equation of state

    Visser, M. Jerk, snap, and the cosmological equation of state. Class. Quant. Grav. 2004, 21, 2603

    2004

  33. [41]

    Aghanim, N. et al. [Planck Collaboration.] Planck 2018 results. VI. Cosmological parameters . Astron. Astrophys. 2020, 641, A6. Erratum in Astron. Astrophys. 2021, 652, C4. 23

    2018

  34. [42]

    Equivalence between Born-Infeld tachyon and effective real scalar field theories for brane structures in warped geometry

    Bernardini, A.E.; Bertolami, O. Equivalence between Born-Infeld tachyon and effective real scalar field theories for brane structures in warped geometry. Phys. Lett. B 2013, 726, 512

    2013

  35. [43]

    Deformed Defects

    Bazeia, D.; Losano, L.; Malbouisson, J.M.C. Deformed Defects. Phys. Rev. D 2002, 66, 101701

    2002

  36. [44]

    Valentino, E.D. et al. [CosmoVerse Network Collaboration] The CosmoVerse White Paper: Addressing observational tensions in cosmology with systematics and fundamental physics. Phys. Dark Univ. 2025, 49, 101965

    2025

  37. [45]

    Abdalla, E.; Abell´ an, G.F.; Aboubrahim, A.; Agnello, A.; Akarsu, O.; Akrami, Y.; Alestas, G.; Aloni, D.; Amendola, L.; Anchordoqui, L.A.; et al.: Cosmology intertwined: A review of the particle physics, astrophysics, and cosmology associated with the cosmological tensions an...

    2022

  38. [46]

    JWST validates HST distance measurements: Selection of supernova subsample explains differences in JWST estimates of local H0

    Riess, A.G.; Scolnic, D.; Anand, G.S.; Breuval, L.; Casertano, S.; Macri, L.M.; Li, S.; Yuan, W.; Huang, C.D.; Jha, S.; et al. JWST validates HST distance measurements: Selection of supernova subsample explains differences in JWST estimates of local H0. Astrophys. J. 2024, 977, 120

    2024

  39. [47]

    Hubble tension in a nonminimally coupled curvature-matter gravity model

    Varela, M.B.; Bertolami, O. Hubble tension in a nonminimally coupled curvature-matter gravity model. JCAP 2024, 06, 025

    2024

  40. [48]

    Soft quantum back reaction to the Hubble tension: A smeared-out early time cosmological energy density, Phys

    Bernardini, A.E. Soft quantum back reaction to the Hubble tension: A smeared-out early time cosmological energy density, Phys. Lett. B 2025, 870, 139889

    2025

  41. [49]

    The Pantheon+ Analysis: The Full Data Set and Light curve Release

    Scolnic, D.; Brout, D.; Carr, A.; Riess, A.G.; Davis, T.M.; Dwomoh, A.; Jones, D.O.; Ali, N.; Charvu, P.; Chen, R.; et al. The Pantheon+ Analysis: The Full Data Set and Light curve Release. Astrophys. J. 2022, 938, 113. 24

    2022

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