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arxiv: 2604.10878 · v1 · submitted 2026-04-13 · 🌀 gr-qc

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Power law scalar potential in the Saez-Ballester like theory: Exact solutions in the Bianchi type I case

J. Socorro , A. Gil-Ocaranza , Juan Luis P\'erez
Authors on Pith no claims yet

Pith reviewed 2026-05-10 16:18 UTC · model grok-4.3

classification 🌀 gr-qc
keywords Bianchi type Ipower-law scalar potentialSaez-Ballester theorychiral multifield cosmologyquintessencephantom cosmologyexact solutionsanisotropic universe
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The pith

Power-law scalar potentials in a generalized Saez-Ballester theory produce the same universe volume function as exponential potentials in chiral multifield cosmology.

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

The paper studies an anisotropic Bianchi type I cosmological model in a generalized Saez-Ballester-K-essence-like theory that includes standard kinetic terms for two scalar fields plus a mixed coupling term. It focuses on power-law potentials of the form V(ψ1,ψ2) = V1 ψ1^{±λ1} + V2 ψ2^{±λ2} and obtains exact solutions for the negative exponent case once the mixed term enforces a constraint on its parameter. This constraint permits quintessence, quintom, and phantom regimes during primordial inflation. The central result is that the derived volume function of the universe exactly matches the volume function obtained from exponential scalar potentials in standard chiral multifield cosmology, yet the scalar fields here remain dynamically present at all times rather than freezing out.

Core claim

Within the generalized Saez-Ballester-like theory with mixed coupling, the power-law scalar potential V(ψ1,ψ2)=V1ψ1^{±λ1}+V2ψ2^{±λ2} admits exact solutions via a change of variables for the negative-sign case under the required parameter constraint. These solutions show that the universe volume function coincides with the volume function generated by exponential potentials in standard chiral multifield cosmology, while the scalar fields continue to evolve dynamically throughout cosmic history.

What carries the argument

The mixed kinetic coupling term in the action, which imposes an essential parameter constraint for negative-sign power-law potentials and enables the change of variables that produces the volume-function equivalence.

If this is right

  • Exact solutions exist for quintessence, quintom, and phantom scenarios in the context of primordial inflation.
  • The scalar fields remain dynamically active throughout the entire cosmic evolution instead of becoming constant.
  • The Bianchi type I anisotropic model is fully solvable under these power-law potentials once the constraint is satisfied.
  • The volume expansion history is identical to the one obtained from exponential potentials in the corresponding chiral multifield setup.

Where Pith is reading between the lines

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

  • The equivalence suggests that background expansion alone cannot distinguish power-law from exponential potentials in this class of models.
  • Perturbation spectra or higher-order observables would be needed to test whether the two potential families produce observationally different signatures.
  • The parameter constraint required for consistency may restrict the viable range of mixed couplings when matching to late-time dark-energy data.

Load-bearing premise

The mixed coupling term must obey a specific constraint on its associated parameter so that the negative-sign power-law potentials remain consistent with the quintessence, quintom, and phantom regimes.

What would settle it

Integrate the field equations numerically for the negative-sign potentials without imposing the mixed-term parameter constraint and check whether the volume function still matches the exponential case or whether no consistent solutions exist.

Figures

Figures reproduced from arXiv: 2604.10878 by A. Gil-Ocaranza, J. Socorro, Juan Luis P\'erez.

Figure 1
Figure 1. Figure 1: Behaviour of the volume function, eq. (47), and the corresponding scalar field ψ1 and ψ2 (49) for the quintessence multiscalar field scenario using as a scalar potential a power law ψ −2 1 + ψ −4 2 in the first time, it say λ1 = 2 and λ2 = 4 resulting that the ℓ parameter become ℓ = 9 16 and the corresponding values for the constants (32), also we use r1 = r2 = q1 = q2 = 1. The evolution of volume function… view at source ↗
Figure 2
Figure 2. Figure 2: Deceleration parameter using the volume function, eq. (47), and all the values that were taken in the graphing of the volume function [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Moderate inflation in the volume function, eq. (66), and the corresponding scalar field ψ1 and ψ2 (68) for the quintessence multiscalar field scenario using as a scalar potential a power law ψ −2 1 + ψ −4 2 , it say λ1 = 2 and λ2 = 4 resulting that the ℓ parameter become ℓ = 9 16 . We take small value in the anisotropic component n = 0.1, also we use r1 = r2 = 2, q1 = q2 = 1, to eliminate the imaginary cha… view at source ↗
Figure 4
Figure 4. Figure 4: Deceleration parameter using the volume function, eq. (66), and all the values that were taken in the graphing of the volume function. IV. PHANTOM MULTISCALAR FIELDS, m11 = m22 = −1 For this scenario of phantom multiscalar field, the constraint on element m12, (28), (29) are the same as in the case of quintessence multiscalar fields; we will also treat it by both solutions [PITH_FULL_IMAGE:figures/full_fi… view at source ↗
Figure 5
Figure 5. Figure 5: Behaviour of the volume function, eq. (84), and the corresponding scalar field ψ1 and ψ2 (86) for the phantom multiscalar field scenario using as a scalar potential a power law ψ −2 1 + ψ −4 2 , it say λ1 = 2 and λ2 = 4 resulting that the ℓ parameter become ℓ = 9 16 , also we use r1 = r2 = q1 = q2 = 1. 1 2 3 4 time -1.00 -0.95 -0.90 -0.85 -0.80 q(t) [PITH_FULL_IMAGE:figures/full_fig_p014_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Deceleration parameter using the volume function, eq. (84), and all the values that were taken in the graphing of the volume function [PITH_FULL_IMAGE:figures/full_fig_p014_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Moderate inflation in the volume function and the corresponding scalar field ψ1 and ψ2 for the phantom multiscalar field scenario using as a scalar potential a power law ψ −2 1 + ψ −4 2 employing m12 − , it say λ1 = 2 and λ2 = 4 resulting that the ℓ parameter become ℓ = 9 16 . Here n = 1, also we use r1 = r1 = q1 = q2 = 1, and we take negative p3 value. 1.5 2.0 2.5 3.0 3.5 4.0 time -1.00 -0.98 -0.96 -0.94 … view at source ↗
Figure 8
Figure 8. Figure 8: Deceleration parameter using the volume function, eq. (89), and all the values that were taken in the graphing of the volume function [PITH_FULL_IMAGE:figures/full_fig_p016_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Behaviour of the volume function, eq. (110), and the corresponding scalar field ψ1 and ψ2 (112) for the quintom multiscalar field scenario using as a scalar potential a power law ψ −2 1 + ψ −4 2 , it say λ1 = 2 and λ2 = 4 resulting that the ℓ parameter become ℓ = 9 16 , also we use n = r1 = r2 = q1 = q2 = 1, and we take negative p3 value. 1.2 1.4 1.6 1.8 2.0 2.2 2.4 time -1.10 -1.08 -1.06 -1.04 -1.02 q(t) … view at source ↗
Figure 10
Figure 10. Figure 10: Deceleration parameter using the volume function, eq. (110), and all the values that were taken in the graphing of the volume function. 2. m12 + case For this case, the matrix element m12 = 1 6 (1 + √ 1 − ℓ)λ1λ2, the Hamiltonian density is rewritten as, H = q a ℓ π 2 1 + qb ℓ π 2 2 + cℓ π 2 3 +  d a ℓ π1 + db ℓ π2  π3 − 6 [PITH_FULL_IMAGE:figures/full_fig_p019_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: Moderate inflation in the volume function, eq. (129), and the corresponding scalar field ψ1 and ψ2 (131) for the quintessence multiscalar field scenario using as a scalar potential a power law ψ −2 1 + ψ −4 2 , it say λ1 = 2 and λ2 = 4 resulting that the ℓ parameter become ℓ = 9 16 . We take small value in the anisotropic component n = 0.1, also we use r1 = r2 = 2, q1 = q2 = 1, to eliminate the imaginary … view at source ↗
Figure 12
Figure 12. Figure 12: Deceleration parameter using the volume function, eq. (129), and all the values that were taken in the graphing of the volume function [PITH_FULL_IMAGE:figures/full_fig_p022_12.png] view at source ↗
read the original abstract

An anisotropic Bianchi type I cosmological model with power-law scalar-field potentials of the form $V(\psi_1,\psi_2)=V_1\psi_1^{\pm\lambda_1}+V_2\psi_2^{\pm\lambda_2}$ is studied within a generalized S\'aez--Ballester--K-essence-like theory involving standard kinetic terms and a mixed coupling contribution. In order to solve the corresponding field equations, for negative sign case, the mixed term introduces an essential constraint on the associated parameter, which yields relevant contributions to quintessence, quintom, and phantom scenarios in the context of primordial inflation. Exact solutions for these regimes are obtained through an appropriate change of variables. It is shown that the volume function of the universe derived from the present power-law scalar potential coincides with that obtained from exponential scalar potentials in standard chiral multifield cosmology, while the scalar fields remain dynamically present throughout the cosmic evolution.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 1 minor

Summary. The paper studies Bianchi type I anisotropic cosmologies in a generalized Saez-Ballester theory with mixed kinetic terms and power-law scalar potentials V(ψ1,ψ2)=V1ψ1^{±λ1}+V2ψ2^{±λ2}. For the negative-exponent case an essential constraint is imposed on the mixed-coupling parameter to close the system, permitting a change of variables that yields exact solutions for quintessence, quintom and phantom regimes; the central claim is that the resulting volume function coincides with the one obtained from exponential potentials in standard chiral multifield cosmology while the scalar fields remain dynamically present.

Significance. If the volume-function identity holds under the stated conditions, the work supplies analytic links between power-law and exponential potentials in multifield anisotropic models, furnishing explicit solutions across several dark-energy regimes. The persistence of scalar-field dynamics throughout evolution is a useful feature for inflation studies.

major comments (2)
  1. [Negative-sign case and change-of-variables section] In the negative-sign derivation, the mixed term is said to force an 'essential constraint' on the coupling parameter to recover the desired regimes and enable the change of variables. No dynamical or stability argument is supplied showing that this constraint is selected by the equations or initial conditions rather than chosen to permit exact integration; relaxing it prevents reduction to the same first-order system, so the claimed volume-function coincidence with the exponential-potential case in chiral multifield cosmology is not a general property of power-law potentials but holds only on this restricted slice.
  2. [Exact solutions and verification] The abstract asserts that exact solutions are obtained and that all field equations are satisfied, yet the manuscript does not display the explicit substitution back into the original Einstein and scalar-field equations after the change of variables. Without this verification the support for the volume-function claim remains incomplete.
minor comments (1)
  1. [Introduction] The relation between the present mixed-coupling term and the original Saez-Ballester action should be stated more explicitly in the introduction to clarify the generalization.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the detailed and constructive report. The comments highlight important points regarding the scope of our results and the need for explicit verification. We address each major comment below and have revised the manuscript to improve clarity and completeness.

read point-by-point responses

  1. Referee: [Negative-sign case and change-of-variables section] In the negative-sign derivation, the mixed term is said to force an 'essential constraint' on the coupling parameter to recover the desired regimes and enable the change of variables. No dynamical or stability argument is supplied showing that this constraint is selected by the equations or initial conditions rather than chosen to permit exact integration; relaxing it prevents reduction to the same first-order system, so the claimed volume-function coincidence with the exponential-potential case in chiral multifield cosmology is not a general property of power-law potentials but holds only on this restricted slice.

    Authors: We agree that the constraint on the mixed-coupling parameter is imposed specifically to close the system and permit the change of variables that yields exact solutions. The manuscript focuses on this analytically tractable case, which allows us to obtain explicit solutions for quintessence, quintom, and phantom regimes while demonstrating the volume-function coincidence with the exponential-potential chiral multifield case. We do not claim the result holds for arbitrary coupling values; the restriction is necessary for the exact integration. In the revised version we have added explicit language clarifying that the volume coincidence and the persistence of dynamical scalar fields are properties of this constrained slice of parameter space, and we note that relaxing the constraint precludes reduction to the integrable first-order system. revision: yes

  2. Referee: [Exact solutions and verification] The abstract asserts that exact solutions are obtained and that all field equations are satisfied, yet the manuscript does not display the explicit substitution back into the original Einstein and scalar-field equations after the change of variables. Without this verification the support for the volume-function claim remains incomplete.

    Authors: We accept this criticism. The revised manuscript now includes the explicit substitution of the derived solutions back into the original Einstein and scalar-field equations, confirming that all equations are satisfied identically under the imposed constraint. This verification directly supports the volume-function identity and the continued dynamical presence of the scalar fields. revision: yes

Circularity Check

1 steps flagged

Volume-function coincidence holds only after an integrability constraint is imposed on the mixed-term parameter

specific steps
  1. fitted input called prediction [Abstract]
    "for negative sign case, the mixed term introduces an essential constraint on the associated parameter, which yields relevant contributions to quintessence, quintom, and phantom scenarios in the context of primordial inflation. Exact solutions for these regimes are obtained through an appropriate change of variables. It is shown that the volume function of the universe derived from the present power-law scalar potential coincides with that obtained from exponential scalar potentials in standard chiral multifield cosmology"

    The constraint is introduced specifically to permit exact integration and to force the volume function to match the known exponential case; the identity is therefore obtained by construction once the parameter slice is chosen, rather than derived independently from the power-law form.

full rationale

The paper states that for the negative-sign power-law potential the mixed kinetic term 'introduces an essential constraint' that is required to close the system and obtain exact solutions matching quintessence/quintom/phantom regimes. The claimed equality of the volume function to the exponential-potential case in chiral multifield cosmology is obtained only after this constraint plus a change of variables. No independent dynamical argument is supplied showing the constraint arises from initial conditions or stability; relaxing it prevents reduction to the same first-order system. This makes the central coincidence an artifact of the selected parameter slice rather than a general property of the power-law potential.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim rests on the standard field equations of the generalized Saez-Ballester-K-essence theory, the Bianchi type I metric ansatz, and the ad-hoc constraint on the mixed-coupling parameter chosen to enable the target inflationary regimes. No new particles or forces are introduced.

free parameters (2)
  • exponents λ1 and λ2
    Chosen to satisfy the negative-sign constraint and produce the desired quintessence, quintom, or phantom behavior.
  • mixed-coupling parameter
    Constrained by the mixed term to allow exact solutions for the negative-sign case.
axioms (2)
  • domain assumption Field equations of the generalized Saez-Ballester-K-essence-like theory hold
    Taken as the starting point for deriving the cosmological solutions.
  • domain assumption Bianchi type I line element is an appropriate description of the early universe
    Standard assumption for studying anisotropic cosmologies.

pith-pipeline@v0.9.0 · 5473 in / 1599 out tokens · 82164 ms · 2026-05-10T16:18:51.946131+00:00 · methodology

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Reference graph

Works this paper leans on

33 extracted references · 11 canonical work pages · 1 internal anchor

  1. [1]

    1 2 3 4 time -1.00 -0.95 -0.90 -0.85 -0.80 -0.75 -0.70 q(t) Figure 4:Deceleration parameter using the volume function, eq

    We take small value in the anisotropic componentn= 0.1, also we user 1 =r 2 = 2,q 1 =q 2 = 1, to eliminate the imaginary character of the constantp 3. 1 2 3 4 time -1.00 -0.95 -0.90 -0.85 -0.80 -0.75 -0.70 q(t) Figure 4:Deceleration parameter using the volume function, eq. (66), and all the values that were taken in the graphing of the volume function. IV...

  2. [2]

    1.5 2.0 2.5 3.0 3.5 4.0 time -1.00 -0.98 -0.96 -0.94 -0.92 q(t) Figure 8:Deceleration parameter using the volume function, eq

    Heren= 1, also we user 1 =r 1 =q 1 =q 2 = 1, and we take negativep 3 value. 1.5 2.0 2.5 3.0 3.5 4.0 time -1.00 -0.98 -0.96 -0.94 -0.92 q(t) Figure 8:Deceleration parameter using the volume function, eq. (89), and all the values that were taken in the graphing of the volume function. 17 V. QUINTOM MUL TISCALAR FIELDS,m 11 = +1, m22 =−1 For this scenario of...

  3. [3]

    We take small value in the anisotropic componentn= 0.1, also we user 1 =r 2 = 2,q 1 =q 2 = 1, to eliminate the imaginary character of the constantp 3. Finally, the deceleration parameter q(t), (30), for this case, using the volume functionV(t) =η 3 (129), can be see in the figure 12, where this tend to -1, characteristic of accelerated growth. 1 2 3 4 tim...

  4. [4]

    Jean-Philippe Uzan, Phys. Rev. D59, 123510 (1999),Cosmological scaling solutions of nonminimally coupled scalar fields

    1999

  5. [5]

    Lobo, M.K

    Tiberiu Harko, Francisco S.N. Lobo, M.K. Mak, Eur. Phys. J. C74, 2784 (2014),Arbitrary scalar-field and quintessence cosmological models

    2014

  6. [6]

    Murli Manohar Verma and Shankar Dayal Pathak, Astrophysics Space Sci.350, 381 (2014),Cosmic expansion driven by real scalar field for different forms of potential

    2014

  7. [7]

    Leon and Emmanuel N Saridakis, Classical and Quantum Grav31, 075018 (2014),Dynamical analysis of anisotropic scalar-field cosmologies for a wide range of potentials

    C.R Fadragas, G. Leon and Emmanuel N Saridakis, Classical and Quantum Grav31, 075018 (2014),Dynamical analysis of anisotropic scalar-field cosmologies for a wide range of potentials

    2014

  8. [8]

    Paliathanasis, Class

    A. Paliathanasis, Class. Quant. Grav.37, 19 (2020),Dynamics of a chiral cosmology

    2020

  9. [9]

    Dutta, W

    J. Dutta, W. Khyllep and N. Tamanini, Phys. Rev. D95, 023515 (2017),Scalar-Fluid interacting dark energy: cosmological dynamics beyond the exponential potential, [arXiv:1701.00744]

    work page arXiv 2017

  10. [10]

    Genly Leon, Alan Coley, Andronikos Paliathanasis, Jonathan Tot and Balkar Yildirim, Physics of the Dark Universe45, 101503 (2024),Global dynamics of two models for Quintom Friedman-Lemaitre-Robertson-Walker universes

    2024

  11. [11]

    Socorro and Luis O

    Abraham Espinoza Garc´ ıa, J. Socorro and Luis O. Pimentel, Int. J. of Theor. Phys.53(9), 3066-3077 (2014),Quantum Bianchi type IX cosmology in K-essence theory.DOI: 10.1007/s10773-014-2102-0

    work page doi:10.1007/s10773-014-2102-0 2014

  12. [12]

    Linder,Astropart

    Roland de Putter and Eric V. Linder,Astropart. Phys.28, 263 (2007).Kinetic k-essence and Quintessence. [arXiv:0705.0400]

    work page arXiv 2007

  13. [13]

    Chiba, S

    T. Chiba, S. Dutta and R.J. Scherrer,Phys. Rev. D80, 043517 (2009).Slow-roll k-essence, [arXiv:0906.0628]

    work page arXiv 2009

  14. [14]

    Bose and A.S

    N. Bose and A.S. Majumdar,Phys. Rev. D79, 103517 (2009).A k-essence model of inflation, dark matter and dark energy, [arXiv:0812.4131]

    work page arXiv 2009

  15. [15]

    Arroja and M

    F. Arroja and M. Sasaki,Phys. Rev. D81, 107301 (2010).A note on the equivalence of a barotropic perfect fluid with a k-essence scalar field, [arXiv:1002.1376]

    work page arXiv 2010

  16. [16]

    Garc´ ıa, J.M

    L.A. Garc´ ıa, J.M. Tejeiro and L. Casta˜ neda,K-essence scalar field as dynamical dark energy, [arXiv:1210.5259]

    work page arXiv

  17. [17]

    Socorro, Luis O

    J. Socorro, Luis O. Pimentel and Abraham Espinoza Garc´ ıa, Advances in High Energy Phys. 805164 (2014),Classical Bianchi type I cosmology in K-essence theory

    2014

  18. [18]

    Socorro and J

    J. Socorro and J. Juan Rosales, Universe9, 185 (2023),Quantum fractionary cosmology: K-essence theory

    2023

  19. [19]

    Socorro, J

    J. Socorro, J. Juan Rosales and L. Toledo-Sesma, Fractal Fract.7, 814 (2023),Anisotropic fractional cosmology: K-essence theory

    2023

  20. [20]

    Socorro, J

    J. Socorro, J. Juan Rosales and Leonel Toledo-Sesma, Universe10, 192 (2024),Non commutative classical and Quantum fractionary Cosmology: FRW case

    2024

  21. [21]

    Socorro, J

    J. Socorro, J. Juan Rosales and Leonel Toledo-Sesma, General Relativity and Gravitation57, 23 (2025),Noncommutative classical and Quantum fractionary Cosmology: Anisotropic Bianchi Type I case

    2025

  22. [22]

    Saez and V.J

    D. Saez and V.J. Ballester, Phys. Lett. A113, 467 (1986)

    1986

  23. [23]

    Sabido, J

    M. Sabido, J. Socorro and L. Arturo Ure˜ na-L´ opez, Fizika B,19(4), 177-186 (2010),Classical and quantum Cosmology of the S´ aez-Ballester theory, [arXiv:0904.0422] 24

    work page arXiv 2010

  24. [24]

    Socorro, M

    J. Socorro, M. Sabido, M.A. S´ anchez G. and M.G. Fr´ ıas Palos, Rev. Mex. F´ ıs.56(2), 166-171 (2010),Anisotropic cosmology in S´ aez-Ballester theory: classical and quantum solutions, [arxiv:1007.3306]

    work page arXiv 2010

  25. [25]

    Abbyazov and S.V

    R.R. Abbyazov and S.V. Chervon, Grav. Cosmol.18, 262 (2012)

    2012

  26. [26]

    Chervon, Quantum matter2, 71 (2013)

    S.V. Chervon, Quantum matter2, 71 (2013)

    2013

  27. [27]

    Dimakis and A

    N. Dimakis and A. Paliathanasis, Class. Quant. Grav.38, (2021),Crossing the phantom divide line as a effect of quantum transistions

    2021

  28. [28]

    Chimento, Phys

    Luis P. Chimento, Phys. Rev. D69, 123517 (2004), Extended tachyon field, Chaplygin gas, and solvable k-essence cos- mologies

    2004

  29. [29]

    Socorro, S

    J. Socorro, S. P´ erez-Pay´ an, Rafael Hern´ andez-Jim´ enez, Abraham Espinoza-Garc´ ıa and Luis Rey D´ ıaz-Barr´ on, Class. Quan- tum Grav.38, 135027 (2021),Classical and quantum exact solutions for a FRW in chiral like cosmology.[arXiv:2012.11108, (gr-qc)]

    work page arXiv 2021

  30. [30]

    P´ erez-Pay´ an, Abraham Espinoza-Garc´ ıa and J

    Luis Rey D´ ıaz-Barr´ on, S. P´ erez-Pay´ an, Abraham Espinoza-Garc´ ıa and J. Socorro, Int. J. Mod. Phys. D30(11), 2150080 (2021),Anisotropic chiral cosmology: exact solutions

    2021

  31. [31]

    Paliathanasis, Universe8, 199 (2022),Hyperbolic inflation in the Jordan frame

    A. Paliathanasis, Universe8, 199 (2022),Hyperbolic inflation in the Jordan frame

    2022

  32. [32]

    Tripathy, Astrophys

    S.K. Tripathy, Astrophys. Sp. Sci.340, (2012) 211

    2012

  33. [33]

    J. Socorro, Juan Luis P´ erez, Luis Rey D´ ıaz-Barr´ on, Abraham Espinoza Garc´ ıa, Sinuh´ e P´ erez Pay´ an,F(R,..) theo- ries from the point of view of the Hamiltonian approach: non-vacuum Anisotropic Bianchi type I cosmological model, [arXiv:2512.10850 [gr-qc]]

    work page internal anchor Pith review Pith/arXiv arXiv