pith. machine review for the scientific record. sign in

arxiv: 2604.17017 · v1 · submitted 2026-04-18 · 🌀 gr-qc

Recognition: unknown

Transiently accelerating cosmological model with Gong-Zhang parametrization in f(T) teleparallel gravity

G. P. Singh, Khomesh R. Patle

Pith reviewed 2026-05-10 06:29 UTC · model grok-4.3

classification 🌀 gr-qc
keywords f(T) gravityteleparallel gravitydark energyGong-Zhang parametrizationtransient accelerationdeceleration parameterquintessencecosmological models
0
0 comments X

The pith

A power-law f(T) model with Gong-Zhang dark energy parametrization produces transient cosmic acceleration followed by future deceleration.

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

The paper constructs an f(T) teleparallel gravity model using the specific power-law form f(T) = α(-T)^n together with the Gong-Zhang parametrization of the dark energy equation of state. It derives the Hubble expansion rate as a function of redshift and then examines the deceleration parameter, energy density, pressure, and equation of state evolution. The central result is that the present-day acceleration is only temporary and the universe will decelerate again at later times while the dark energy component exhibits quintessence-like behavior today. The model is confronted with cosmic chronometer and Pantheon supernova data via Bayesian fitting, and it is shown to satisfy the generalized second law of thermodynamics.

Core claim

By adopting the power-law ansatz f(T) = α(-T)^n in conjunction with the Gong-Zhang parametrization of the dark energy equation of state, the derived Hubble parameter yields a deceleration parameter that changes sign twice: the universe is currently accelerating but will enter a decelerating phase in the future. Both geometrical and dynamical diagnostics indicate quintessence-like dark energy at the present epoch, while the model remains thermodynamically viable according to the generalized second law and produces an age of the universe consistent with observations.

What carries the argument

The power-law form f(T) = α(-T)^n in f(T) teleparallel gravity, combined with the Gong-Zhang parametrization of the dark energy equation of state, which together determine the redshift-dependent Hubble rate and all derived cosmological quantities.

If this is right

  • The deceleration parameter crosses zero twice, marking a finite period of acceleration between two decelerating eras.
  • The dark energy equation of state remains greater than -1 today, consistent with quintessence rather than phantom behavior.
  • Energy conditions for the dark energy component are satisfied in a manner compatible with observed expansion history.
  • The model satisfies the generalized second law of thermodynamics at all times.

Where Pith is reading between the lines

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

  • If the transient acceleration result holds, long-term cosmological forecasts would need to replace a perpetual de Sitter phase with an eventual return to matter-like deceleration.
  • The same functional forms could be applied to other modified gravity theories to test whether transient acceleration is generic or specific to this f(T) choice.
  • High-redshift surveys that tightly constrain the equation of state beyond z ≈ 2 would directly test whether the Gong-Zhang parametrization remains accurate far from the present epoch.

Load-bearing premise

The power-law ansatz for f(T) and the Gong-Zhang parametrization remain valid over the entire redshift range, including the extrapolated future.

What would settle it

Future measurements of the deceleration parameter or dark energy equation of state at low redshifts (z < 0) that show continued acceleration rather than a return to deceleration would rule out the model's central prediction.

Figures

Figures reproduced from arXiv: 2604.17017 by G. P. Singh, Khomesh R. Patle.

Figure 1
Figure 1. Figure 1: The best-fit H(z) curve for the proposed model is compared with the ΛCDM model. parameterized form of the Hubble parameter in equation (24), are constrained using the cosmic chronome￾ter (CC) dataset along with the combined (CC+Pantheon) dataset. The estimation of these parameters is performed by minimizing the χ 2 function, together with the Markov chain Monte Carlo (MCMC) sampling technique, implemented … view at source ↗
Figure 2
Figure 2. Figure 2: Marginalized 1D and 2D posterior contour map with median values of H0, ω0 and n using the Joint dataset. 8 [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Plot of the deceleration parameter (q) with z. 5 The physical and dynamical characteristics of the model 5.1 Analysis of deceleration parameter The deceleration parameter q is a fundamental quantity for characterizing the expansion dynamics of the universe, as it provides insight into the nature of cosmic evolution. Different values of q correspond to distinct expansion regimes: q < 0 signifies an accelera… view at source ↗
Figure 5
Figure 5. Figure 5: Plot of pressure (pDE) with z. 5.2 Observational study of energy density, pressure and equation of state parameter We examine the physical properties of key cosmological quantities, namely the energy density and pressure. For the constrained model parameters, the energy density remains positive throughout the cosmic expan￾sion, while the pressure exhibits negative values, driving the accelerated expansion … view at source ↗
Figure 6
Figure 6. Figure 6: Plot of EoS parameter (ωDE) with z. The graphical evolution of the EoS parameter for the proposed model is illustrated in Fig. (6). The present-day values at z = 0 are found to be ωDE = −0.769 for the CC dataset and ωDE = −0.843 for the joint dataset. These values indicate that the model exhibits a quintessence-like behavior of DE at the current epoch for both datasets. The evolution of ωDE further suggest… view at source ↗
Figure 7
Figure 7. Figure 7: The components of energy conditions with [PITH_FULL_IMAGE:figures/full_fig_p012_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: Plot of s and r plane. • In the Chaplygin gas (CG) model, the parameters typically satisfy (r > 1, s < 0). • The standard ΛCDM model is represented by r = 1 and s = 0. • For Quintessence model, one generally finds (r < 1, s > 0). • Holographic dark energy (HDE) model, (r = 1, s = 2 3 ). • For Standard cold dark matter (SCDM), one may have (r = 1, s = 1). The evolutionary trajectories of the proposed model … view at source ↗
Figure 9
Figure 9. Figure 9: Plot of Om(z) diagnostics with z. powerful diagnostic tool for exploring dark energy dynamics, effectively delineating regions corresponding to accelerated cosmic expansion. This methodology, first proposed by Caldwell and Linder [98] for quintessence scalar fields, offers a systematic approach for categorizing dark energy models according to their evolutionary trajectories. Two characteristic behaviors ar… view at source ↗
Figure 10
Figure 10. Figure 10: Plot of (ωDE −ω ′ DE) plane. ity of this law has also been examined in the framework of f(T) teleparallel gravity in earlier studies [33, 60], highlighting its significance in modified gravitational scenarios. In this work, we employ the Gong-Zhang parametrization of the DE EoS parameter within the framework of f(T) teleparallel gravity. It is therefore of considerable interest to examine whether the prop… view at source ↗
Figure 11
Figure 11. Figure 11: Plot of S˙ tot with z. where the subscript ‘t’ denotes the total quantity and Vh = 4 3 πR 3 h represents the volume enclosed by the ap￾parent horizon. Therefore, the rate of change of entropy associated with the fluid inside the horizon can be written as S˙ in = (ρt + pt)V˙ h +ρ˙tVh Tin . (42) Under the assumption of thermal equilibrium between the cosmic fluid and the horizon, the temperature of the flui… view at source ↗
read the original abstract

We present the cosmic expansion scenario in the framework of $f(T)$ gravity by employing a dark energy equation of state (EoS) parameter. Specifically, we proceed with the power-law form of the function $f(T) = \alpha$$(-T)^{n}$, in conjunction with the Gong-Zhang parametrization of the dark energy EoS. We derive the expansion rate in terms of the redshift for the considered model, providing deeper insights into the underlying cosmic dynamics. The model is further utilized to explore the expansion history of the universe and the evolution of several cosmological parameters. By using the Bayesian methods based on the $\chi^{2}$-minimization technique, the median values of the model parameters are determined for the cosmic chronometer (CC) and joint (CC+Pantheon) datasets. The evolution of the deceleration parameter, energy density, pressure, EoS parameter and the energy conditions for dark energy is analyzed in detail. The model captures the observed acceleration as a transient phenomenon, followed by future deceleration. Additionally, the nature of both geometrical and dynamical diagnostics robustly indicates a quintessence-like behavior at the present epoch. Finally, the thermodynamic viability of the model is confirmed through the generalized second law of thermodynamics and the estimated age of the universe further supports the model's compatibility with astronomical observations.

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 / 2 minor

Summary. The manuscript presents a cosmological model in f(T) teleparallel gravity employing the power-law ansatz f(T) = α(-T)^n together with the Gong-Zhang parametrization of the dark-energy equation of state. The authors derive an analytic expression for the Hubble rate H(z), determine the free parameters (α, n, w0, w1) by χ² minimization against cosmic-chronometer and Pantheon supernova data, and then examine the redshift evolution of the deceleration parameter q(z), energy density, pressure, EoS parameter, energy conditions, and thermodynamic quantities. They conclude that the present-day acceleration is transient and will be followed by deceleration at future times, while the present epoch exhibits quintessence-like behavior; thermodynamic viability is asserted via the generalized second law.

Significance. If the transient-acceleration result survives robustness checks, the work supplies a concrete, observationally calibrated example of how a simple f(T) modification can produce a temporary accelerated phase without a cosmological constant. The combination of analytic derivation, numerical fitting to two independent datasets, and multiple geometric/dynamical diagnostics is a positive feature. The significance is nevertheless reduced by the absence of quantified uncertainties on the future q(z) sign change and by the lack of tests against alternative parametrizations that fit the same data.

major comments (2)
  1. [Results / deceleration-parameter evolution] Results section on the deceleration parameter: the central claim that acceleration is transient (q0 < 0 followed by q(z) > 0 for some z < 0) is obtained by extrapolating the fitted Gong-Zhang wDE(z) and power-law f(T) beyond the redshift range of the data (z ≲ 2). No error bands, MCMC posterior samples, or prior-variation tests are shown for the future sign change in q(z), so it is impossible to assess whether the claimed transition is robust or an artifact of the chosen functional forms.
  2. [Model construction and fitting procedure] Parameter-fitting and model-construction paragraphs: the Gong-Zhang parameters w0, w1 and the exponents n, α are determined by minimizing χ² against the identical CC + Pantheon datasets that are later used to assert the transient behavior. Because the future evolution is a direct consequence of the fitted ansatz rather than an independent prediction, the manuscript must demonstrate that the sign change in q(z) persists under equally plausible alternative parametrizations that also fit the data.
minor comments (2)
  1. [Abstract and thermodynamic analysis] The abstract states that the model is “thermodynamically viable” but does not specify which form of the generalized second law is employed or whether the entropy production rate remains positive for all future times; a brief clarification would improve readability.
  2. [Notation throughout] Notation for the Gong-Zhang parameters (w0, w1) and the f(T) exponents (n, α) should be introduced once in the model section and used consistently thereafter; occasional redefinition of symbols in later figures is distracting.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for the thorough review and insightful comments on our manuscript. We address each major comment below and outline the revisions we will make to improve the presentation and robustness of our results.

read point-by-point responses
  1. Referee: Results section on the deceleration parameter: the central claim that acceleration is transient (q0 < 0 followed by q(z) > 0 for some z < 0) is obtained by extrapolating the fitted Gong-Zhang wDE(z) and power-law f(T) beyond the redshift range of the data (z ≲ 2). No error bands, MCMC posterior samples, or prior-variation tests are shown for the future sign change in q(z), so it is impossible to assess whether the claimed transition is robust or an artifact of the chosen functional forms.

    Authors: We agree with the referee that displaying uncertainties is crucial for assessing the robustness of the future deceleration. In the revised manuscript, we will include 1σ and 2σ confidence bands on the deceleration parameter q(z) derived from the covariance matrix of the best-fit parameters obtained via χ² minimization. This will allow readers to evaluate the statistical significance of the sign change in q(z) at negative redshifts. We will also mention the limitations of extrapolation beyond the data range. revision: yes

  2. Referee: Parameter-fitting and model-construction paragraphs: the Gong-Zhang parameters w0, w1 and the exponents n, α are determined by minimizing χ² against the identical CC + Pantheon datasets that are later used to assert the transient behavior. Because the future evolution is a direct consequence of the fitted ansatz rather than an independent prediction, the manuscript must demonstrate that the sign change in q(z) persists under equally plausible alternative parametrizations that also fit the data.

    Authors: The Gong-Zhang parametrization was selected for its ability to model the dark energy EoS with a simple form that accommodates both past and future evolution. We acknowledge that the transient acceleration is specific to this choice. In the revision, we will add a paragraph in the discussion section comparing briefly with the Chevallier-Polarski-Linder (CPL) parametrization using the same f(T) form, noting any differences in the predicted future behavior. However, an exhaustive test of all possible parametrizations is beyond the scope of this work, as our focus is on providing an analytic model with the Gong-Zhang form calibrated to observations. revision: partial

Circularity Check

0 steps flagged

No significant circularity; transient behavior follows from assumed forms and data fit without reduction to inputs by construction

full rationale

The paper adopts the power-law ansatz f(T) = α(-T)^n and Gong-Zhang parametrization for w_DE(z) by explicit assumption, derives H(z) from the f(T) Friedmann equation, fits the free parameters via χ² minimization to CC and Pantheon data, and then evaluates the resulting q(z) evolution. The statement that acceleration is transient (present q0 < 0 followed by future deceleration) is a direct consequence of extrapolating the fitted functional forms to z < 0, but this does not constitute a self-definitional loop, a fitted quantity renamed as prediction, or any other enumerated circular pattern. No load-bearing self-citations, uniqueness theorems, or ansatz smuggling are present. The derivation chain is self-contained given the stated assumptions and does not reduce any claimed result to equivalence with its inputs by construction.

Axiom & Free-Parameter Ledger

3 free parameters · 2 axioms · 0 invented entities

The model rests on the standard FLRW metric, the teleparallel equivalent of general relativity, and the assumption that the Gong-Zhang parametrization plus power-law f(T) together constitute a complete effective description from z=0 to the future. No new particles or forces are postulated.

free parameters (3)
  • α
    Amplitude of the power-law f(T) term, fitted to data.
  • n
    Exponent of the power-law f(T) term, fitted to data.
  • w0, w1 (Gong-Zhang parameters)
    Two parameters in the dark-energy equation-of-state parametrization, fitted to data.
axioms (2)
  • standard math The universe is described by a flat FLRW metric with torsion scalar T = -6H².
    Invoked when writing the modified Friedmann equations in f(T) gravity.
  • domain assumption The Gong-Zhang parametrization w(z) = w0 + w1 z/(1+z) remains valid at all redshifts.
    Used to close the system and extrapolate to future deceleration.

pith-pipeline@v0.9.0 · 5539 in / 1600 out tokens · 37444 ms · 2026-05-10T06:29:11.098973+00:00 · methodology

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

107 extracted references · 107 canonical work pages · 1 internal anchor

  1. [1]

    A. G. Riess, A. V . Filippenko, P . Challis, A. Clocchiatti , A. Diercks et al., Observational Evidence from Supernovae for an Accelerating Universe and a Cosmological Constant, Astronomical Journal, 116, 1009- 1038 (1998) https://doi.org/10.1086/300499

  2. [2]

    and Aldering, G

    S. Perlmutter, G. Aldering, G. Goldhaber, R. A. Knop, P . N ugent et al., Measurements of Ω and Λ from 42 High-Redshift Supernovae, Astrophysical Journal, 517, 565–586 (1999) https://doi.org/10.1086/307221

  3. [3]

    A&A , volume =

    N. Aghanim, Y . Akrami, M. Ashdown, J. Aumont, C. Baccigal upi, et al., Planck 2018 results. VI. Cosmological parameters, Astronomy and Astro physics, 641, A6 (2020) https://doi.org/10.1051/0004-6361/201833910

  4. [4]

    Weinberg, The Cosmological Constant Problem, Rev

    S. Weinberg, The cosmological constant problem, Review s of Modern Physics, 61, 1 (1989) https://doi.org/10.1103/RevModPhys.61.1

  5. [5]

    Classical and Quantum Gravity , keywords =

    E. Di V alentino, O. Mena, S. Pan, L. Visinelli, W. Y ang, et al., In the realm of the Hubble tension—a review of solutions, Classical and Quantu m Gravity, 38, 153001 (2021) https://doi.org/10.1088/1361-6382/ac086d

  6. [6]

    S. M. Carroll, The cosmological constant, Living Review s in Relativity, 4, 1-56 (2001) https://doi.org/10.12942/lrr-2001-1

  7. [7]

    Padmanabhan, Cosmological constant—the weight of th e vacuum, Physics reports, 380, 235–320 (2003) https://doi.org/10.1016/S0370-1573(03)00120-0

    T. Padmanabhan, Cosmological constant—the weight of th e vacuum, Physics reports, 380, 235–320 (2003) https://doi.org/10.1016/S0370-1573(03)00120-0

  8. [8]

    E. J. Copeland, M. Sami, S. Tsujikawa, Dynamics of dark en ergy, International Journal of Modern Physics D, 15, 1753–1935 (2006) https://doi.org/10.1142/S021827180600942X 18

  9. [9]

    H. A. Buchdahl, Non-linear Lagrangians and cosmologica l theory, Monthly Notices of the Royal Astro- nomical Society, 150, 1-8 (1970) https://doi.org/10.1093/mnras/150.1.1

  10. [10]

    Harko, F

    T. Harko, F. S. N. Lobo, S. Nojiri, S. D. Odintsov, f (R,T ) gravity, Physical Review D,84, 024020 (2011) https://doi.org/10.1103/PhysRevD.84.024020

  11. [11]

    Unified cosmic history in modified gravity: from F(R) theory to Lorentz non-invariant models,

    S. Nojiri, S. D. Odintsov, Unified cosmic history in modi fied gravity: from f (R) theory to Lorentz non-invariant models, Physics Reports, 505, 59-144 (2011) https://doi.org/10.1016/j.physrep.2011.04.001

  12. [12]

    J. B. Jim´ enez, L. Heisenberg, T. Koivisto, Coincident general relativity, Physical Review D, 98, 044048 (2018) https://doi.org/10.1103/PhysRevD.98.044048

  13. [13]

    Modified Gravity Theories on a Nutshell: Inflation, Bounce and Late-time Evolution,

    S. Nojiri, S. D. Odintsov, V . K. Oikonomou, Modified grav ity theories on a nut- shell: Inflation, bounce and late-time evolution, Physics R eports, 692, 1-104 (2017) https://doi.org/10.1016/j.physrep.2017.06.001

  14. [14]

    Bamba, S

    K. Bamba, S. D. Odintsov, L. Sebastiani, S. Zerbini, Fin ite-time future singularities in modified Gauss– Bonnet and f(R, G) gravity and singularity avoidance, The Eu ropean Physical Journal C, 67, 295–310 (2010) https://doi.org/10.1140/epjc/s10052-010-1292-8

  15. [15]

    Elizalde,and R

    E. Elizalde,and R. Myrzakulov, V . V . Obukhov, D. S´ aez- G´ omez,Λ CDM epoch reconstruction from F (R, G) and modified Gauss-Bonnet gravities, Classical and Q uantum Gravity, 27, 095007 (2010) https://doi.org/10.1088/0264-9381/27/9/095007

  16. [16]

    Harko, F

    T. Harko, F. S. N. Lobo, f (R,Lm) gravity, The European Physical Journal C, 70, 373–379 (2010) https://doi.org/10.1140/epjc/s10052-010-1467-3

  17. [17]

    Capozziello, R

    S. Capozziello, R. D’Agostino, O. Luongo, Extended gra vity cosmography, International Journal of Modern Physics D, 28, 1930016 (2019) https://doi.org/10.1142/S0218271819300167

  18. [18]

    Capozziello, V

    S. Capozziello, V . De Falco, C. Ferrara, The role of the b oundary term in f (Q,B) symmetric teleparallel gravity,The European Physical Jou rnal C, 83, 915 (2023) https://doi.org/10.1140/epjc/s10052-023-12072-y

  19. [19]

    Kotambkar, G

    S. Kotambkar, G. P . Singh, R. Kelkar, B. K. Bishi, Anisot ropic Bianchi type I cosmological models with generalized Chaplygin gas and dynamical gravitational and cosmological constants, Communications in Theoretical Physics, 67, 222 (2017) https://doi.org/10.1088/0253-6102/67/2/222

  20. [20]

    A. R. Lalke, G. P . Singh, A. Singh, Late-time accelerati on from ekpyrotic bounce in f (Q,T ) gravity, International Journal of Geometric Methods in Mod ern Physics, 20, 2350131 (2023) doi:https://doi.org/10.1142/S0219887823501311

  21. [21]

    Hulke, G

    N. Hulke, G. P . Singh, B. K. Bishi, A. Singh, V ariable Cha plygin gas cosmolo- gies in f (R,T ) gravity with particle creation, New Astronomy, 77, 101357 (2020) https://doi.org/10.1016/j.newast.2020.101357

  22. [22]

    R. Garg, G. P . Singh, A. R. Lalke, S. Ray, Cosmological mo del with linear equa- tion of state parameter in f (R,Lm) gravity, Physics Letters A, 525, 129937 (2024) https://doi.org/10.1016/j.physleta.2024.129937

  23. [23]

    Singh, S

    A. Singh, S. Mandal, R. Chaubey, R. Raushan, Observatio nal constraints on the expansion scalar and shear relation in the Locally rotationally symmetric Bianc hi I model, Physics of the Dark Universe, 47, 101798 (2025) https://doi.org/10.1016/j.dark.2024.101798 19

  24. [24]

    K. N. Singh, G. R. P . Teruel, S. K. Maurya, T. Chowdhury, F . Rahaman, Conservative worm- holes in generalized K(R,T ) function, Journal of High Energy Astrophysics, 44, 132–145 (2024) https://doi.org/10.1016/j.jheap.2024.09.009

  25. [25]

    Chaudhary, S

    H. Chaudhary, S. K. J. Pacif, G. Mustafa, F. Atamurotov, F. Javed, Extracting H0 and rd in q(t) parametrization models, Journal of High Energy Astrophysi cs, 45, 340–349 (2025) https://doi.org/10.1016/j.jheap.2025.01.001

  26. [26]

    G. K. Goswami, R. Rani, J. K. Singh, A. Pradhan, FLRW cosm ology in Weyl type f (Q) gravity and observational constraints, Journal of High Ene rgy Astrophysics, 43, 105–113 (2024) https://doi.org/10.1016/j.jheap.2024.06.011

  27. [27]

    B. K. Shukla, S. Sahlu, D. Sofuo˘ glu, P . Mishra, A. H. Alf edeel, Multi-components fluid in f (R,T ) gravity with observational constraints, The European Phys ical Journal Plus, 140, 1–14 (2025) https://doi.org/10.1140/epjp/s13360-025-06200-8

  28. [28]

    L. A. Escamilla, D. Fiorucci, G. Montani, E. Di V alentin o, Exploring the Hubble tension with a late time Modified Gravity scenario, Physics of the Dar k Universe, 46, 101652 (2024) https://doi.org/10.1016/j.dark.2024.101652

  29. [29]

    K. R. Patle, G. P . Singh, R. Garg, Dynamical constraints on variable vac- uum energy in Brans-Dicke theory, arXiv preprint arXiv:260 1.00419, (2026) https://doi.org/10.48550/arXiv.2601.00419

  30. [30]

    G. R. Bengochea, R. Ferraro, Dark torsion as the cosmic s peed-up, Physical Review D, 79, 124019 (2009) https://doi.org/10.1103/PhysRevD.79.124019

  31. [31]

    Capozziello, M

    Yi-Fu Cai, S. Capozziello, M. De Laurentis, E. N. Sarida kis, f (T) teleparal- lel gravity and cosmology, Reports on Progress in Physics, 79, 106901 (2016) https://doi.org/10.1088/0034-4885/79/10/106901

  32. [32]

    Paliathanasis, J

    A. Paliathanasis, J. D. Barrow, P . G. L. Leach, Cosmolog ical solutions of f (T) gravity, Physical Review D, 94, 023525 (2016) https://doi.org/10.1103/PhysRevD.94.023525

  33. [33]

    I. G. Salako, M. E. Rodrigues, A. V . Kpadonou, M. J. S. Hou ndjo, J. Tossa, Λ CDM model in f (T ) gravity: reconstruction, thermodynamics and stability, J ournal of Cosmology and Astroparticle Physics, 2013, 060–060 (2013) https://doi.org/10.1088/1475-7516/2013/11/060

  34. [34]

    Capozziello, V

    S. Capozziello, V . F. Cardone, H. Farajollahi, A. Ravan pak, Cosmography in f (T ) gravity, Physical Review D, 84, 043527 (2011) https://doi.org/10.1103/PhysRevD.84.043527

  35. [35]

    Di Liu, M. J. Reboucas, Energy conditions bounds on f (T ) gravity, Physical Review D, 86, 083515 (2012) https://doi.org/10.1103/PhysRevD.86.083515

  36. [36]

    Yi-Fu Cai, Shih-Hung Chen, J. B. Dent, S. Dutta, E. N. Sar idakis, Matter bounce cosmology with the f (T ) gravity, Classical and Quantum Gravity, 28, 215011 (2011) https://doi.org/10.1088/0264-9381/28/21/215011

  37. [37]

    Zhadyranova, M

    A. Zhadyranova, M. Koussour, S. Bekkhozhayev, V . Zhuma bekova, J. Rayimbaev, Exploring late-time cosmic acceleration: A study of a linear f (T ) cosmological model using observational data, Physics of the Dark Universe, 45, 101514 (2024) https://doi.org/10.1016/j.dark.2024.101514

  38. [38]

    K. Bamba, Chao-Qiang Geng, Chung-Chi Lee, Ling-Wei Luo , Equation of state for dark en- ergy in f (T ) gravity, Journal of Cosmology and Astroparticle Physics, 2011, 021–021 (2011) https://doi.org/10.1088/1475-7516/2011/01/021 20

  39. [39]

    Paliathanasis, S

    A. Paliathanasis, S. Basilakos, E. N. Saridakis, S. Cap ozziello, K. Atazadeh, F. Darabi, M. Tsamparlis, New Schwarzschild-like solutions in f (T ) gravity through Noether symmetries, Physical Review D, 89, 104042 (2014) https://doi.org/10.1103/PhysRevD.89.104042

  40. [40]

    Capozziello, R

    S. Capozziello, R. D’Agostino, O. Luongo, Model-indep endent reconstruction of f (T ) teleparallel cosmology, General Relativity and Gravitati on, 49, 141 (2017) https://doi.org/10.1007/s10714-017-2304-x

  41. [41]

    S. H. Shekh, A. Pradhan, A. Dixit, S. N. Bayaskar, S. C. Da runde, Cosmographical analysis for H(z) parametrization towards viscous f (T ) gravity, Modern Physics Letters A, 40, 2450187 (2025) https://doi.org/10.1142/S0217732324501876

  42. [42]

    L. K. Duchaniya, K. Gandhi, B. Mishra, Attractor behavi or of f (T ) modified grav- ity and the cosmic acceleration, Physics of the Dark Univers e, 44, 101461 (2024) https://doi.org/10.1016/j.dark.2024.101461

  43. [43]

    S. K. Maurya, A. Errehymy, M. Govender, G. Mustafa, N. Al -Harbi et al., Anisotropic compact stars in complexity formalism and isotropic stars made of anisotr opic fluid under minimal geometric de- formation (MGD) context in f (T ) gravity-theory, The European Physical Journal C, 83, 348 (2023) https://doi.org/10.1140/epjc/s10052-023-11507-w

  44. [44]

    D. C. Maurya, Accelerating scenarios of viscous fluid un iverse in modified f (T ) grav- ity, International Journal of Geometric Methods in Modern P hysics, 19, 2250144 (2022) https://doi.org/10.1142/S0219887822501444

  45. [45]

    Bamba, G

    K. Bamba, G. G. L. Nashed, W. El Hanafy, Sh. K. Ibraheem, B ounce inflation in f (T ) Cosmology: A unified inflaton-quintessence field, Physical R eview D, 94, 083513 (2016) https://doi.org/10.1103/PhysRevD.94.083513

  46. [46]

    P . Bhar, F. Rahaman, S. Das, S. Aktar, A. Errehymy, Aniso tropic quintessence compact star in f (T ) gravity with Tolman–Kuchowicz metric potentials, Communi cations in Theoretical Physics, 76, 015401 (2024) https://doi.org/10.1088/1572-9494/ad08ad

  47. [47]

    R. C. Nunes, S. Pan, E. N. Saridakis, New observational c onstraints on f (T ) gravity from cosmic chronometers, Journal of Cosmology and Astropartic le Physics, 2016, 011–011 (2016) https://doi.org/10.1088/1475-7516/2016/08/011

  48. [48]

    Chaudhary, U

    H. Chaudhary, U. Debnath, T. Roy, S. Maity, G. Mustafa et al., Constraints on the pa- rameters of modified Chaplygin–Jacobi and modified Chaplygi n–Abel gases in f (T ) grav- ity, International Journal of Geometric Methods in Modern P hysics, 21, 2450248 (2024) https://doi.org/10.1142/S0219887824502487

  49. [49]

    L. K. Duchaniya, S. V . Lohakare, B. Mishra, S. K. Tripath y, Dynamical stability analy- sis of accelerating f (T ) gravity models, The European Physical Journal C, 82, 448 (2022) https://doi.org/10.1140/epjc/s10052-022-10406-w

  50. [50]

    Chakraborty, S

    M. Chakraborty, S. Chakraborty, The classical and quan tum implications of the Ray- chaudhuri equation in f (T )-gravity, Classical and Quantum Gravity, 40, 155010 (2023) https://doi.org/10.1088/1361-6382/ace231

  51. [51]

    S. K. Maurya, J. Kumar, S. Kiroriwal, Role of decoupling process on the configurations of compact stars induced by Thomas-Fermi dark matter with null complex ity in f (T ) gravity, Journal of High Energy Astrophysics, 44, 194–209 (2024) https://doi.org/10.1016/j.jheap.2024.09.012

  52. [52]

    Dixit, A

    A. Dixit, A. Pradhan, D. C. Maurya, A probe of cosmologic al models in modified teleparal- 21 lel gravity, International Journal of Geometric Methods in Modern Physics, 18, 2150208 (2021) https://doi.org/10.1142/S021988782150208X

  53. [53]

    Bahamonde, K

    S. Bahamonde, K. F. Dialektopoulos, C. Escamilla-Rive ra, G. Farrugia, V . Gakis et al., Telepar- allel gravity: from theory to cosmology, Reports on Progres s in Physics, 86, 026901 (2023) https://doi.org/10.1088/1361-6633/ac9cef

  54. [54]

    K. R. Patle, G. P . Singh, Revisiting f (T ) Teleparallel Gravity with a Parametrized Hub- ble Parameter and Observational Constraints, arXiv prepri nt arXiv:2603.18971, (2026) https://doi.org/10.48550/arXiv.2603.18971

  55. [55]

    S. Das, A. Beesham, S. Chattopadhyay, Study of neutron s tar in f (T ) and f (G) grav- ity framework with polytropic gas background, Annals of Phy sics, 458, 169460 (2023) https://doi.org/10.1016/j.aop.2023.169460

  56. [56]

    X. Ren, S. F. Y an, Y . Zhao, Y . F. Cai, E. N. Saridakis, Gaus sian processes and effective field theory of f (T ) gravity under the H 0 tension, The Astrophysical Journal, 932, 131 (2023) https://doi.org/10.3847/1538-4357/ac6ba5

  57. [57]

    Aldrovandi and J

    R. Aldrovandi, J. G. Pereira, Teleparallel gravity: an introduction, Springer Science & Business Media, volume 173, (2012) doi:https://doi.org/10.1007/978-94-007-5143-9

  58. [58]

    E. V . Linder, Einstein’s other gravity and the accelera tion of the universe, Physical Review D, 81, 127301 (2010) https://doi.org/10.1103/PhysRevD.81.127301

  59. [59]

    J. W. Maluf, The teleparallel equivalent of general rel ativity, Annalen der Physik, 525, 339–357 (2013) https://doi.org/10.1002/andp.201200272

  60. [60]

    Karami, A

    K. Karami, A. Abdolmaleki, Generalized second law of th ermodynamics in f (T ) gravity, Journal of Cosmology and Astroparticle Physics, 2012, 007–007 (2012) https://doi.org/10.1088/1475-7516/2012/04/007

  61. [61]

    Rezazadeh, A

    K. Rezazadeh, A. Abdolmaleki, K. Karami, Power-law and intermediate inflation- ary models in f (T )-gravity, Journal of High Energy Physics, 2016, 1–27 (2016) https://doi.org/10.1007/JHEP01(2016)131

  62. [62]

    Basilakos, Linear growth in power law f (T ) gravity, Physical Review D, 93, 083007 (2016) https://doi.org/10.1103/PhysRevD.93.083007

    S. Basilakos, Linear growth in power law f (T ) gravity, Physical Review D, 93, 083007 (2016) https://doi.org/10.1103/PhysRevD.93.083007

  63. [63]

    Malekjani, S

    M. Malekjani, S. Basilakos, N. Heidari, Spherical coll apse model and cluster number counts in power-law f (T ) gravity, Monthly Notices of the Royal Astronomical Society , 466, 3488–3496 (2017) https://doi.org/10.1093/mnras/stw3367

  64. [64]

    R. D. Boko, M. J. S. Houndjo, Cosmological viscous fluid m odels describing infi- nite time singularities in f (T ) gravity, The European Physical Journal C, 80, 855 (2020) https://doi.org/10.1140/epjc/s10052-020-8252-8

  65. [65]

    Kumar, R

    S. Kumar, R. C. Nunes, P . Y adav, New cosmological constr aints on f (T ) gravity in light of full Planck-CMB and type Ia supernovae data, Physical Rev iew D, 107, 063529 (2023) https://doi.org/10.1103/PhysRevD.107.063529

  66. [66]

    Mandal, S

    S. Mandal, S. Pradhan, P . K. Sahoo, T. Harko, Cosmologic al observational constraints on the power law f (Q) type modified gravity theory, The European Physical Journal C, 83, 1141 (2023) https://doi.org/10.1140/epjc/s10052-023-12339-4

  67. [67]

    Arora, A

    S. Arora, A. Parida, P . K. Sahoo, Constraining effectiv e equation of 22 state in f (Q,T ) gravity, The European Physical Journal C, 81, 555 (2021) https://doi.org/10.1140/epjc/s10052-021-09358-4

  68. [68]

    Koussour, A

    M. Koussour, A. De, Observational constraints on two co smological mod- els of f (Q) theory, The European Physical Journal C, 83, 400 (2023) https://doi.org/10.1140/epjc/s10052-023-11547-2

  69. [69]

    Myrzakulov, M

    N. Myrzakulov, M. Koussour, A. H. A. Alfedeel, A. Abebe, Constrained evolution of effective equa- tion of state parameter in non-linear f (R,Lm) dark energy model: insights from Bayesian analysis of cosmic chronometers and Pantheon samples, The European P hysical Journal C, 138, 852 (2023) https://doi.org/10.1140/epjp/s13360-023-04483-3

  70. [70]

    Y . Gong, Y . Z. Zhang, Probing the curvature and dark ener gy, Physical Review D, 72, 043518 (2005) https://doi.org/10.1103/PhysRevD.72.043518

  71. [71]

    doi:10.1086/670067 , eprint =

    D. Foreman-Mackey, D. W. Hogg, D. Lang, J. Goodman, emce e: the MCMC hammer, Publications of the Astronomical Society of the Pacific, 125, 306 (2013) https://doi.org/10.1086/670067

  72. [72]

    Constraints on the redshift dependence of the dark energy potential

    J. Simon, L. V erde, R. Jimenez, Constraints on the redsh ift dependence of the dark energy potential, Physical Review D, 71, 123001 (2005) https://doi.org/10.1103/PhysRevD.71.123001

  73. [73]

    G. S. Sharov, V . O. V asiliev, How predictions of cosmological models depend on Hubble parameter data sets, arXiv preprint arXiv:1807.07323 (2018) https://doi.org/10.26456/mmg/2018-611

  74. [74]

    Stern, R

    D. Stern, R. Jimenez, L. V erde, M. Kamionkowski, S. A. St anford, Cosmic chronometers: constraining the equation of state of dark energy. I: H(z) measurements, Journal of Cosmology and Astroparticle Physics, 2010, 008 (2010) https://doi.org/10.1088/1475-7516/2010/02/008

  75. [75]

    M. Moresco, Raising the bar: new constraints on the Hubb le parameter with cosmic chronome- ters at z 2, Monthly Notices of the Royal Astronomical Society: Lette rs, 450, L16–L20 (2015) https://doi.org/10.1093/mnrasl/slv037

  76. [76]

    Jimenez and A

    R. Jimenez, A. Loeb, Constraining cosmological parame ters based on relative galaxy ages, The Astro- physical Journal, 573, 37 (2002) https://doi.org/10.1086/340549

  77. [77]

    Mandal, A

    S. Mandal, A. Singh, R. Chaubey, Cosmic evolution of hol ographic dark energy in f (Q,T ) gravity, International Journal of Geometric Methods in Mod ern Physics, 20, 2350084 (2023) https://doi.org/10.1142/S0219887823500846

  78. [78]

    D. M. Scolnic, D. O. Jones, A. Rest, Y . C. Pan, R. Chornock et al., The complete light- curve sample of spectroscopically confirmed SNe Ia from Pan- STARRS1 and cosmological con- straints from the combined Pantheon sample, The Astrophysi cal Journal, 859, 101 (2018) https://doi.org/10.3847/1538-4357/aab9bb

  79. [79]

    A. G. Riess, R. P . Kirshner, B. P . Schmidt, S. Jha, P . Chal lis et al., BVRI light curves for 22 type Ia supernovae, The Astronomical Journal, 117, 707 (1999) https://doi.org/10.1086/300738

  80. [80]

    , keywords =

    M. Hicken, W. M. Wood-V asey, S. Blondin, P . Challis, S. J ha et al., Improved dark energy con- straints from 100 new CfA supernova type Ia light curves, The Astrophysical Journal, 700, 1097 (2009) https://doi.org/10.1088/0004-637X/700/2/1097

Showing first 80 references.