REVIEW 3 major objections 5 minor 72 references
Correspondence between particle creation and dark components interaction in the context of $f(\mathcal{G})$ gravity
T0 review · 3 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash
Pith's one-line read The paper claims that particle creation in the late universe is described by $\dot{N}/N = 3 b^2 H/(1+\omega_m)$, which produces a phantom-crossing dark energy with $\Omega_{m0}=0.31$ and $\Omega_{de0}=0.69$.
desk verdict Fatal algebra error in Eqs. (29d)-(29e) invalidates the dark energy results; the paper is a parameter-tuned reconstruction, not a testable prediction. read the letter →
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
The reading
What carries the argument
The load-bearing object is the correspondence identity $\dot{N}/N = 3b^2 H/(1+\omega_m)$, which equates the particle-creation rate from the thermodynamic continuity equation with the energy-transfer rate built into the $f(\mathcal{G})$ gravity two-fluid equations. This single identity converts the particle number $N$ into a redshift variable, lets every geometric quantity ($H$, $\dot{H}$, the Gauss-Bonnet term $\mathcal{G}$, and derivatives of $f(\mathcal{G})$) be expressed in terms of $N$, and thereby produces closed-form expressions for $\rho_{de}$, $p_{de}$, and $\omega_{de}$ through the $f(\mathcal{G})$ field equations.
What would settle it
Compute the predicted Hubble rate $H(z)$ from the model's $\rho_{de}$ and $p_{de}$ via the Friedmann equation and compare it against the full Hubble parameter data compilation; if the fit is notably worse than the simple power-law fit, the chosen parameters are ruled out. A second, independent falsifier is a direct measurement of the matter equation of state: any determination far from $\omega_m = 12$ would contradict the assumed input.
Extended reading notes
Core claim
The central claim is that the particle production rate coincides with the interaction rate between matter and dark energy. Matching Eq. (17), the adiabatic continuity equation for a particle-creating universe, with Eq. (11a), the matter continuity equation of $f(\mathcal{G})$ gravity that includes $Q = 3b^2 H \rho_m$, gives $\dot{N}/N = 3b^2 H/(1+\omega_m)$. Consequently the particle number scales as $N \sim a^{3b^2/(1+\omega_m)}$ and the matter density as $\rho_m = \rho_{m0} a^{-3(1-b^2+\omega_m)}$. Inserting power-law expansion and the polynomial $f(\mathcal{G})$, the dark energy density and pressure become explicit functions of redshift; for the adopted parameters $\rho_{de}>0$ and $p_{de}<0$ throughout, and $\omega_{de}$ falls from the quintessence region (above $-1$) to the phantom region (below $-1$). The model also yields $\Omega_{m0}=0.31$ and $\Omega_{de0}=0.69$, which the authors take to be compatible with Planck 2018.
Load-bearing premise
The derivation depends on the specific phenomenological interaction $Q = 3b^2 H \rho_m$ with constant coupling $b$, and on the hand-picked values $b=4.5$, $\omega_m=12$, and $\rho_{m0}=4225$ that force the plotted behavior.
Editorial extensions
If this is right
- The dark energy equation of state crosses from quintessence to phantom, so the model describes the late-time accelerated expansion without a cosmological constant.
- The present matter and dark energy densities are $\Omega_{m0}=0.31$ and $\Omega_{de0}=0.69$, matching the Planck 2018 energy budget.
- The particle creation rate is set by the interaction coupling $b$ and the matter equation-of-state $\omega_m$, so measuring one of these quantities determines the other.
- The matter energy density evolves as $\rho_m = \rho_{m0} a^{-3(1-b^2+\omega_m)}$, a direct prediction of the interaction cosmology.
Reading between the lines
- The correspondence suggests that the 'matter creation' seen in the thermodynamics and the 'interaction' appearing in the Friedmann equations are two labels for the same energy flow; if so, the particle number $N$ should be treated as a dynamical observable rather than a bookkeeping device.
- The specific parameter values $b=4.5$, $\omega_m=12$, and $\rho_{m0}=4225$ are chosen to satisfy the sign conditions, so a natural test is to run the same derivation with other $f(\mathcal{G})$ forms or other $Q$ prescriptions to see whether the quintessence-to-phantom crossing is generic or an artifact of the tuning.
- Because the identity relates $\dot{N}/N$ directly to $H$, precise measurements of the Hubble parameter as a function of redshift could be inverted to reconstruct the particle creation history, offering an observational route to test the model.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper proposes a correspondence between adiabatic particle creation and the interaction of dark matter and dark energy in f(G) gravity. It derives the particle production rate Ndot/N = 3b^2 H/(1 + omega_m), rewrites H, the Gauss-Bonnet term G, and the function f(G) in terms of the particle number N, and, using power-law cosmology with the specific choice f(G) = C1 G + C2 sqrt(alpha G) + C3 G^m, obtains expressions for the dark-energy density and pressure. The authors then plot rho_de, p_de, and omega_de, report a quintessence-to-phantom crossing, and quote Omega_m0 = 0.31 and Omega_de0 = 0.69 as consistent with Planck 2018. The abstract also claims a fit to Hubble parameter data.
Significance. If the construction were correct, the paper would offer a unified picture in which particle creation, an interaction between the dark components, and f(G) gravity jointly produce late-time acceleration and a phantom-crossing equation of state. The formal setup up to Eq. (19) is straightforward, and the authors are transparent about their parameter choices. However, the central equations (29d) and (29e) contain a derivative error that invalidates the computed p_de and hence the phantom crossing and the quoted Omega_de0. In addition, the reported Omega_m0 agreement with Planck is enforced by hand through the choice of rho_m0. Because the main quantitative claims rest on an algebraic mistake and on parameter tuning rather than on a predictive fit, the significance of the paper as it stands is low.
major comments (3)
- [Sec. IV, Eqs. (29d)-(29e)] The quantities fGN and fGNN are not the derivatives of fG that the notation claims. From Eq. (26c), G is proportional to N^{-4(1+omega_m)/(3 n b^2)}, and Eq. (29d) is exactly G_N; it contains no fGG and no dependence on C2, C3, or m. For the adopted m=2, fG includes the term 2 C3 G, so fGN must include 2 C3 G_N; Eq. (29d) cannot be correct. Equation (29e) is likewise the second N-derivative of G, not of fG. Because Eqs. (26e)-(26f) and hence pde in Eq. (27b) are built on fGN and fGNN, the plotted pde, the phantom-crossing behavior in Fig. 2, and the quoted Omega_de0 are consequences of a miscomputed intermediate quantity rather than of the specified f(G) model. In addition, Eq. (29c) has the wrong sign for the C3 term: differentiating C3 G^m gives +C3 m(m-1) G^{m-2}, not +C3 m(1-m) G^{m-2}.
- [Sec. IV, parameter list and Table I] The reported present density parameters are not predictions. Equation (14) gives Omega_m0 = kappa^2 rho_m0/(3 H0^2); with H0 fixed at 67.4, choosing rho_m0 = 4225 fixes Omega_m0, and Omega_de0 = 1 - Omega_m0 is then automatic. The parameter set C1 = C2 = 2, C3 = -0.8, m = 2, alpha = -1, b = 4.5, omega_m = 12 is selected, in the authors' own words, to enforce rho_de > 0 and pde < 0. Agreement with the Planck value Omega_m0 = 0.315 +/- 0.007 is therefore obtained by construction, not by fitting or prediction.
- [Abstract and Sec. IV, Eq. (24c)] The abstract claims that the model is fitted to Hubble data, but no fit of the full model is performed. The only cited fit is H(z) = H0(1+z)^{1/n} with n = 0.956, taken from Refs. [63-68]; this expression is independent of the particle-creation and f(G) content. The f(G) parameters are not constrained by data, and no likelihood, chi-square, or error bars for the derived Omega values are given. The claimed observational agreement therefore reduces to the known power-law fit plus hand-picked parameters, not to a test of the proposed correspondence.
minor comments (5)
- [Sec. III, after Eq. (19)] The text says the production rate is positive 'when the energy flows from matter to dark energy', but Eqs. (11) and the preceding paragraph state that positive Q corresponds to transfer from dark energy to dark matter; please reconcile this wording.
- [Sec. I and Sec. IV] The outline promises a stability analysis, and Sec. IV says 'we explore stability analysis,' but no stability analysis appears in the paper.
- [Sec. IV and Sec. V] The value of n is quoted as 0.956 in Sec. IV and as 0.965 in the conclusion; one of these is a typo.
- [Sec. IV, parameter list] The unit of rho_m0 = 4225 is not specified; without units, the values in Fig. 1 and Table I are not reproducible.
- [Title and Sec. V] There are typographical errors, including 'compone nts' in the title and 'atter' in Sec. V, which should be corrected.
Circularity Check
Planck density parameters are fixed by the hand-picked ρm0, and the phantom-crossing pressure is built from a mislabeled derivative (dG/dN presented as dfG/dN) rather than from the stated f(G).
-
fitted input called prediction
[Sec. IV, parameter list and density-parameter subsection, around Eqs. (14), (31) and Table I]
"Now, to describe the model, we selectively test the current model with some free parameters, which are chosen here as C1 = C2 = 2, C3 = −0.8, m = 2, α = −1, b = 4.5, ω m = 12, and ρm0 = 4225. It should be noted that the corresponding choice is so sensitive and plays an important role in the evolution of the universe."
From Eq. (14), Ωm0 = κ²ρm0/(3H0²), and Eq. (31) reduces to this same algebraic identity at z = 0 (N = 1). The value ρm0 = 4225 was selected as a free parameter before the paper reports Ωm0 = 0.31 and declares the result compatible with Planck. Thus the Planck agreement is not an output of the cosmology; it is inserted by the choice of ρm0 and then read back as a confirmed density parameter.
-
renaming known result
[Sec. IV, after Eq. (26f) and Eqs. (29d)-(29e)]
"where fGN = d fG/dN and fGN N = d fGN /dN . ... fGN = 32η(1+ω m)/n2b2 N^{−4(1+ω m)/(3nb2)−1}, (29d)"
Differentiating Eq. (26c), G = −24(1−n)H0^4/n N^{−4(1+ωm)/(3nb²)}, with respect to N produces exactly Eq. (29d), with no fGG factor and no dependence on C2, C3, m, or α. For the stated f(G), dfG/dN = fGG dG/dN, so Eq. (29d) is not dfG/dN but merely dG/dN. Since Eq. (27b) constructs pde from fGN and fGNN, the plotted pressure, the quintessence-to-phantom crossing, and the inferred Ωde0 are consequences of a power-law kinematic quantity renamed as an f(G) derivative, not of the stated f(G) dynamics.
full rationale
The headline cosmological output, Ωm0 = 0.31, is not an independent prediction: it is the definition Ωm0 = κ²ρm0/(3H0²) evaluated with the hand-picked ρm0 = 4225, so the claimed Planck compatibility is forced by construction. That alone warrants a partial-circularity score in the 6 range. A second defect compounds the problem and is visible inside the paper's own equations: Eq. (29d) is labeled dfG/dN, but it is exactly the N-derivative of G from Eq. (26c), independent of the f(G) coefficients. Consequently the phantom-crossing result is not a genuine consequence of the stated f(G) model. I did not score the self-citations [67,68] heavily: the power-law fit n is also attributed to external references [63–66], and n is not the contested result. The main circularity is the parameter-selected Planck density parameter presented as a derived compatibility.
Assumptions & free parameters
free parameters (9)
- b (interaction coupling) =
4.5
- omega_m (matter equation of state) =
12
- C1 =
2
- C2 =
2
- C3 =
-0.8
- m =
2
- alpha =
-1
- rho_m0 (present matter density) =
4225
- n (power-law exponent) =
0.956
assumptions (6)
- domain assumption Flat FLRW metric (3)
- domain assumption Universe is an adiabatic open system with dE = dQ - p dV + (h/n) d(nV), and Q = 0
- domain assumption Interaction term Q = 3 b^2 H rho_m with constant b
- domain assumption Power-law scale factor a(t) = a0 (t/t0)^n
- ad hoc to paper Specific f(G) = C1 G + C2 sqrt(alpha G) + C3 G^m
- domain assumption Matter component obeys barotropic EoS p_m = omega_m rho_m with constant omega_m
Cite this review
Pith. "Pith review of Correspondence between particle creation and dark components interaction in the context of $f(\mathcal{G})$ gravity." pith.science (2026). https://pith.science/paper/IWH2FYSE
@misc{pith2026250522699,
author = {Pith},
title = {Pith review of: Correspondence between particle creation and dark components interaction in the context of $f(\mathcalG)$ gravity},
year = {2026},
howpublished = {\url{https://pith.science/paper/IWH2FYSE}},
note = {Machine review of arXiv:2505.22699}
}
abstract
In this paper, we explore the particle creation scenario in the context of $f(\mathcal{G})$ gravity in flat-FLRW metric. For this purpose, from the perspective of thermodynamics and considering an adiabatic universe, we obtain the modified continuity equation in terms of the dynamic number of particles $N$. On the other hand, we obtain Friedmann's equations in $f(\mathcal{G})$ gravity and then write down the continuity equations of the components of matter and dark energy, taking into account the interaction between them. In what follows, by establishing a correspondence between the particle production scenario and $f(\mathcal{G})$ gravity, we obtain the cosmological parameters in terms of $N$. After that, we find cosmological solutions using power-law cosmology and compare them with Hubble parameter data. Finally, we fit the current model with Hubble data and plot the best fit in terms of the redshift parameter.
Figures
Reference graph
Works this paper leans on
-
[1]
Weinberg, ”The cosmological constant problem.” Reviews of mo dern physics 61, no
S. Weinberg, ”The cosmological constant problem.” Reviews of mo dern physics 61, no. 1 (1989): 1
work page 1989
-
[2]
R. R. Caldwell, ”A phantom menace? Cosmological consequences o f a dark energy component with super-negative equation of state.” Physics Letters B, 545(1):23 , 2002
work page 2002
-
[3]
A. R. Amani, ”Stability of Quintom Model of Dark Energy in ( ω , ω ′) Phase Plane.” International Journal of Theoretical Physics, 50(10):3078, 2011
work page 2011
-
[4]
J. Sadeghi, and A. R. Amani, ”The solution of tachyon inflation in cu rved universe.” International Journal of Theoretical Physics, 48(1):14, 2009
work page 2009
-
[5]
R. A. Battye and F. Pace, ”Approximation of the potential in sca lar field dark energy models.” Physical Review D 94, no. 6 (2016): 063513
work page 2016
-
[6]
M. Li, T. Qiu, Y. Cai and X. Zhang, ”On dark energy models of single scalar field.” Journal of Cosmology and Astroparticle Physics 2012, no. 04 (2012): 003
work page 2012
-
[7]
A. R. Amani and S. L. Dehneshin, ”Interacting F (R, T ) gravity with modified Chaplygin gas.” Canadian Journal of Physics 93.12 (2015): 1453-1459
work page 2015
-
[8]
Faraoni, ”Turnaround radius in modified gravity.” Physics of th e Dark Universe 11 (2016): 11-15
V. Faraoni, ”Turnaround radius in modified gravity.” Physics of th e Dark Universe 11 (2016): 11-15
work page 2016
Show all 72 references
-
[9]
Wei, ”Entropy-corrected holographic dark energy.” Commun ications in Theoretical Physics, 52(4):743, 2009
H. Wei, ”Entropy-corrected holographic dark energy.” Commun ications in Theoretical Physics, 52(4):743, 2009
2009
-
[10]
A. R. Amani, and A. Samiee-Nouri, ”Logarithmic entropy correc ted holographic dark energy with F (R, T ) gravity.” Communications in Theoretical Physics, 64(4):485, 2015
2015
-
[11]
Nojiri and S
S. Nojiri and S. D. Odintsov, ”Unifying inflation with Λ CDM epoch in modified f (R) gravity consistent with Solar System tests.” Physics Letters B 657.4 (2007): 238-245
2007
-
[12]
Li, ”A model of holographic dark energy.” Physics Letters B 6 03, no
M. Li, ”A model of holographic dark energy.” Physics Letters B 6 03, no. 1 (2004): 1-5
2004
-
[13]
Del Campo, J
S. Del Campo, J. C. Fabris, R. Herrera and W. Zimdahl, ”Hologra phic dark-energy models.” Physical Review D 83, no. 12 (2011): 123006
2011
-
[14]
Y. Hu, M. Li, N. Li and Z. Zhang, ”Holographic dark energy with c osmological constant.” Journal of Cosmology and Astroparticle Physics 2015, no. 08 (2015): 012. 14
2015
-
[15]
A. R. Amani, C. Escamilla-Rivera, and H. R. Faghani, ”Interactin g closed string tachyon with modified Chaplygin gas and its stability,” Phys. Rev. D 88:124008, 2013
2013
-
[16]
Morais, M
J. Morais, M. Bouhmadi-Lopez, K. Sravan Kumar, J. Marto and Y. Tavakoli, ”Interacting 3-form dark energy models: Distinguishing interactions and avoiding the Little Siblin g of the Big Rip.” Physics of the Dark Universe 15 (2017): 7-30
2017
-
[17]
Zhang, ”Self-interacting dark matter without direct detec tion constraints.” Physics of the Dark Universe 15 (2017) 82
Y. Zhang, ”Self-interacting dark matter without direct detec tion constraints.” Physics of the Dark Universe 15 (2017) 82
2017
-
[18]
Singh, R
T. Singh, R. Chaubey and A. Singh, ”Bouncing cosmologies in Bran s–Dicke theory.” Canadian Journal of Physics 94, no. 7 (2016): 623-627
2016
-
[19]
S. D. Sadatian, and S. M. R. Hosseini, ”Bouncing universe scena rio in f (Q, T ) gravity model.” Inter- national Journal of Geometric Methods in Modern Physics 21, no. 9 (2024): 2450168-688
2024
-
[20]
G. C. Assolohou, C. A ¨ ınamon, C. D. Akowanou, M. G. Ganiou, an d M. J. S. Houndjo, ”Generat- ing f (R, G) gravity from type IV singular bouncing cosmology.” International Journal of Geometric Methods in Modern Physics 21, no. 7 (2024): 2450140-144
2024
-
[21]
Malik, Adnan, Z
A. Malik, Adnan, Z. Asghar, A. H. Alkhaldi, and M. Farasat Shamir , ”Bouncing cosmology in Chern- Simons f (R) gravity.” International Journal of Geometric Methods in Modern Physics 21, no. 4 (2024): 2450088-321
2024
-
[22]
Battista, ”Nonsingular bouncing cosmology in general relativ ity: physical analysis of the spacetime defect.” Classical and Quantum Gravity 38, no
E. Battista, ”Nonsingular bouncing cosmology in general relativ ity: physical analysis of the spacetime defect.” Classical and Quantum Gravity 38, no. 19 (2021): 195007
2021
-
[23]
Sahni, and Y
V. Sahni, and Y. Shtanov, ”Braneworld models of dark energy.” Journal of Cosmology and Astroparticle Physics, 2003(11):014, 2003
2003
-
[24]
M. R. Setare, J. Sadeghi, and A. R. Amani, ”Shape invariance me thod for quintom model in the bent brane background.” Physics Letters B, 660(4):299, 2008
2008
-
[25]
G. P. de Brito, J. M. Hoff da Silva, P. Michel LT da Silva, and A. de So uza Dutra, ”Smooth braneworld models possibility in modified gravities.” International Journal of Mod ern Physics D, 24, no. 11 (2015): 1550089
2015
-
[26]
A. R. Amani and H. Farahani, ”Phantom accretion onto the Sch warzschild anti de-Sitter black hole.” International Journal of Theoretical Physics 51, no. 5 (2012): 1498-1502
2012
-
[27]
A. R. Amani and H. Farahani, ”Phantom Accretion onto the Sch warzschild AdS Black Hole with Topological Defect.” International Journal of Theoretical Phys ics 51, no. 9 (2012): 2943-2949
2012
-
[28]
S. R. Bhoyar, V. R. Chirde and S. H. Shekh, ”Stability of Acceler ating Universe with Linear Equation of State in f (T ) Gravity Using Hybrid Expansion Law.” Astrophysics 60, no. 2 (2017 ): 259-272
2017
-
[29]
V. R. Chirde and S. H. Shekh, ”Transition between general rela tivity and quantum gravity using quark and strange quark matter with some kinematical test.” Journal of Astrophysics and Astronomy 39, no. 5 (2018): 56
2018
-
[30]
J. K. Singh, K. Bamba, R. Nagpal and S. K. J. Pacif, ”Bouncing c osmology in f (R, T ) gravity.” Physical Review D 97, no. 12 (2018): 123536. 15
2018
-
[31]
Nagpal, S
R. Nagpal, S. K. J. Pacif, J. K. Singh, Kazuharu Bamba and A. Be esham, ”Analysis with observational constraints in Λ-cosmology in f (R, T ) gravity.” The European Physical Journal C 78, no. 11 (2018): 946
2018
-
[32]
H. Wei, R. G. Cai, ”Cosmological constraints on new agegraphic d ark energy.” Phys. Lett. B 663, 1 (2008)
2008
-
[33]
Wei, R.G
H. Wei, R.G. Cai, ”Statefinder diagnostic and ω − ω ′ analysis for the agegraphic dark energy models without and with interaction.” Phys. Lett. B 665, 1 (2007)
2007
-
[34]
A. G. Riess, A. V. Filippenko, P. Challis, A. Clocchiatti, A. Diercks, P. M. Garnavich, R. L. Gilliland, and et al, ”Observational evidence from supernovae for an accele rating universe and a cosmological constant.” The Astronomical Journal 116, no. 3 (1998): 1009
1998
-
[35]
Perlmutter, G
S. Perlmutter, G. Aldering, G. Goldhaber, R. A. Knop, P. Nugen t, P. G. Castro, S. Deustua, and et al, ”Measurements of Ω and Λ from 42 high-redshift supernovae.” T he Astrophysical Journal 517, no. 2 (1999): 565
1999
-
[36]
C. L. Bennett, M. Halpern, G. Hinshaw, N. Jarosik, A. Kogut, M . Limon, S. S. Meyer et al, ”First- Year Wilkinson Microwave Anisotropy Probe (WMAP)* Observations: Preliminary Maps and Basic Results.” The Astrophysical Journal Supplement Series 148, no. 1 (2003): 1
2003
-
[37]
Tegmark, M
M. Tegmark, M. A. Strauss, M. R. Blanton, K. Abazajian, S. Do delson, H. Sandvik, X. Wang et al, ”Cosmological parameters from SDSS and WMAP.” Physical Review D 6 9, no. 10 (2004): 103501
2004
-
[38]
Parker, ”Particle creation in expanding universes.” Physical Review Letters 21, no
L. Parker, ”Particle creation in expanding universes.” Physical Review Letters 21, no. 8 (1968): 562
1968
-
[39]
Hawking, ”Particle creation by black holes.” Commun
S.W. Hawking, ”Particle creation by black holes.” Commun. Math. P hys. 43(1975)199
1975
-
[40]
Y. B. ZelDovich, and A. A. Starobinskii, ”Particle production and vacuum polarization in an anisotropic gravitational field.” Soviet Journal of Experimental and Theoretic al Physics 34 (1972): 1159
1972
-
[41]
Prigogine, ”Thermodynamics and cosmology.” International journal of theoretical physics 28, no
I. Prigogine, ”Thermodynamics and cosmology.” International journal of theoretical physics 28, no. 9 (1989): 927-933
1989
-
[42]
Parker, ”Particle creation and particle number in an expandin g universe.” Journal of Physics A: Mathematical and Theoretical 45, no
L. Parker, ”Particle creation and particle number in an expandin g universe.” Journal of Physics A: Mathematical and Theoretical 45, no. 37 (2012): 374023
2012
-
[43]
V. H. Cardenas, ”Dark energy, matter creation and curvatu re.” The European Physical Journal C 72, no. 9 (2012): 1-6
2012
-
[44]
J. C. Fabris, J. A. de Freitas Pacheco, and O. F. Piattella, ”Is t he continuous matter creation cosmology an alternative to Λ CDM ?.” Journal of Cosmology and Astroparticle Physics 2014, no. 06 (2 014): 038
2014
-
[45]
S. K. Biswas, W. Khyllep, J. Dutta, and S. Chakraborty, ”Dyna mical analysis of an interacting dark energy model in the framework of a particle creation mechanism.” Ph ysical Review D 95, no. 10 (2017): 103009
2017
-
[46]
Rashidi, F
R. Rashidi, F. Ahmadi, and M. R. Setare, ”Particle creation in the framework of f (G) gravity.” Astro- physics and Space Science 363, no. 9 (2018): 196
2018
-
[47]
Mandal, and P
S. Mandal, and P. K. Sahoo, ”On the temporal evolution of part icle production in f (T ) gravity.” Modern Physics Letters A 35, no. 40 (2020): 2050328. 16
2020
-
[48]
Nojiri, S
S. Nojiri, S. D. Odintsov, and M. Sasaki. ”Gauss-Bonnet dark e nergy.” Physical Review D 71, no. 12 (2005): 123509
2005
-
[49]
Nojiri, and S
S. Nojiri, and S. D. Odintsov. ”Modified Gauss–Bonnet theory a s gravitational alternative for dark energy.” Physics Letters B 631, no. 1-2 (2005): 1-6
2005
-
[50]
Guo, Zong-Kuan, and D. J. Schwarz. ”Power spectra from an inflaton coupled to the Gauss-Bonnet term.” Physical Review D 80, no. 6 (2009): 063523
2009
-
[51]
Bamba, Kazuharu, S. D. Odintsov, L. Sebastiani, and Sergio Ze rbini, ”Finite-time future singularities in modified Gauss–Bonnet and F (R, G ) gravity and singularity avoidance.” The European Physical Journal C 67, no. 1 (2010): 295-310
2010
-
[52]
N. M. Garcia, T. Harko, F. S. N. Lobo, and J. P. Mimoso, ”Energ y conditions in modified Gauss-Bonnet gravity.” Physical Review D 83, no. 10 (2011): 104032
2011
-
[53]
Bamba, M
K. Bamba, M. Ilyas, M. Z. Bhatti, and Z. Yousaf, ”Energy cond itions in modified f (G) gravity.” General Relativity and Gravitation 49, no. 8 (2017): 1-17
2017
-
[54]
Carloni, and J
S. Carloni, and J. P. Mimoso, ”Phase space of modified Gauss–Bo nnet gravity.” The European Physical Journal C 77, no. 8 (2017): 1-10
2017
-
[55]
Glavan, and C
D. Glavan, and C. Lin, ”Einstein-Gauss-Bonnet gravity in four- dimensional spacetime.” Physical review letters 124, no. 8 (2020): 081301
2020
-
[56]
S. D. Odintsov, V. K. Oikonomou, F. P. Fronimos, and K. V. Faso ulakos, ”Unification of a bounce with a viable dark energy era in Gauss-Bonnet gravity.” Physical Review D 102, no. 10 (2020): 104042
2020
-
[57]
Chern, ”A simple intrinsic proof of the Gauss-Bonnet formula for closed Riemannian manifolds.” Annals of mathematics Vol
S. Chern, ”A simple intrinsic proof of the Gauss-Bonnet formula for closed Riemannian manifolds.” Annals of mathematics Vol. 45, No. 4 (1944): 747-752
1944
-
[58]
B. Li, J. D. Barrow, and D. F. Mota, ”Cosmology of modified Gaus s-Bonnet gravity.” Physical Review D 76, no. 4 (2007): 044027
2007
-
[59]
Pav´ on, and B
D. Pav´ on, and B. Wang, ”Le Chˆ atelier–Braun principle in cosmo logical physics.” General Relativity and Gravitation 41, no. 1 (2009): 1-5
2009
-
[60]
Zimdahl, D
W. Zimdahl, D. Pav´ on, and L. P. Chimento, ”Interacting quinte ssence.” Physics Letters B 521, no. 3-4 (2001): 133-138
2001
-
[61]
Dutta, W
J. Dutta, W. Khyllep, and N. Tamanini, ”Dark energy with a gradie nt coupling to the dark matter fluid: cosmological dynamics and structure formation.” Journal of Cosmology and Astroparticle Physics 2018, no. 01 (2018): 038
2018
-
[62]
Aghanim and et al, ”Planck 2018 results-VI
N. Aghanim and et al, ”Planck 2018 results-VI. Cosmological par ameters.” Astronomy and Astro- physics, 641 (2020): A6
2020
-
[63]
Moresco, L
M. Moresco, L. Pozzetti, A. Cimatti and et al, ”A 6% measureme nt of the Hubble parameter at z ∼ 0. 45: direct evidence of the epoch of cosmic re-acceleration.” Journal o f Cosmology and Astroparticle Physics 2016, no. 05 (2016): 014
2016
-
[64]
Farooq, F
O. Farooq, F. R. Madiyar, S. Crandall and B. Ratra, ”Hubble Pa rameter Measurement Constraints on the Redshift of the Deceleration–acceleration Transition, Dynamic al Dark Energy, and Space Curva- 17 ture.” The Astrophysical Journal, 835, no. 1 (2017): 26
2017
-
[65]
S. K. J. Pacif, R. Myrzakulov and S. Myrzakul, ”Reconstructio n of cosmic history from a simple parametrization of H.” International Journal of Geometric Methods in Modern Physics 1 4, no. 07 (2017): 1750111
2017
-
[66]
Magana, M
J. Magana, M. H. Amante, M. A. Garcia-Aspeitia and V. Motta, ” The Cardassian expansion revisited: constraints from updated Hubble parameter measurements and t ype Ia supernova data.” Monthly Notices of the Royal Astronomical Society 476, no. 1 (2018): 103 6-1049
2018
-
[67]
Pourbagher and A
A. Pourbagher and A. Amani, Thermodynamics of the viscous f (T, B ) gravity in the new agegraphic dark energy model. Modern Physics Letters A 35, no. 20 (2020): 2 050166
2020
-
[68]
Mahichi, A
E. Mahichi, A. Amani, and M. A. Ramzanpour, ”Extended Bose-E instein condensate dark matter in viscous Gauss-Bonnet gravity.” Modern Physics Letters A 37, no. 35n36 (2022): 2250228
2022
-
[69]
Goheer, R
N. Goheer, R. Goswami, P. K. S. Dunsby, and K. Ananda, ”Coex istence of matter dominated and accelerating solutions in f (G) gravity.” Physical Review D 79, no. 12 (2009): 121301
2009
-
[70]
A. R. Rastkar, M. R. Setare, and F. Darabi, ”Phantom phase p ower-law solution in f (G) gravity.” Astrophysics and Space Science 337 (2012): 487-491
2012
-
[71]
Munyeshyaka, A
A. Munyeshyaka, A. Ayirwanda, F. Twagirayezu, B. Murorunk were, and J. Ntahompagaze, ”Multifluid cosmology in f (G) gravity.” International Journal of Geometric Methods in Modern Physics 20, no. 02 (2023): 2350031
2023
-
[72]
D. M. Scolnic, D. O. Jones, A. Rest, Y. C. Pan, R. Chornock, R. J. Foley, M. E. Huber et al, ”The complete light-curve sample of spectroscopically confirmed SNe Ia f rom Pan-STARRS1 and cosmological constraints from the combined pantheon sample.” The Astrophysic al Journal 859,...
2018
Reviewed August 7, 2026 · model on record in the stance chip above.
Discussion (0). Sign in to comment.