Pith. sign in

REVIEW 3 major objections 6 minor 72 references

Black Bounces in $f(Q)$ Gravity with Magnetic Source

T0 review · 3 major / 6 minor · reviewed 2026-08-07 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read The paper claims that Simpson-Visser and Bardeen black-bounce spacetimes in f(Q) gravity can be sourced by an ordinary scalar field plus a magnetic charge, where in general relativity a phantom scalar is required.

desk verdict Correct source reconstruction for black bounces in linear f(Q), but the 'ordinary scalar' claim is an artifact of making the gravitational coupling negative; with a healthy coupling you recover the known GR phantom source. read the letter →

arxiv 2505.22341 v1 pith:JOHHOFLS submitted 2025-05-28 gr-qc

P{i}nar Kirezli , Doğukan Taşer This is my paper · ORCID
classification gr-qc MSC 83C5783D0583C15 PACS 04.20.Jb04.50.Kd04.70.Bw
keywords f(Q)gravityblackbounceSimpson-VissermetricBardeenphantomscalarfieldcanonicalnonlinearelectrodynamicsenergyconditions
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper tries to establish that two well-known black-bounce spacetimes, the Simpson-Visser and Bardeen types, can be sourced in $f(Q)$ gravity by a canonical scalar field (positive kinetic energy) together with a non-linear magnetic monopole, whereas in general relativity the same geometries require a phantom scalar field with negative kinetic energy. The construction fixes $f(Q) = \alpha Q + \beta$ with constant $\alpha$, which reduces the scalar coupling to $h(\Phi) = -\alpha$; taking negative $\alpha$ makes the scalar ordinary. Explicit potential and non-linear electrodynamics functions are derived for both metric families, and the energy conditions are shown to be violated in at least one direction, so the spacetimes still need exotic matter but not a phantom kinetic term in the $f(Q)$ frame. If the construction holds, modified gravity of the non-metricity type changes the required matter content for regular black-hole wormhole geometries.

What carries the argument

The load-bearing object is the constancy of the non-metricity coupling, $f_Q = \alpha$, which makes $f(Q) = \alpha Q + \beta$. The field equations then collapse the scalar source into $h(\Phi) = -\alpha$, so the sign of $\alpha$ alone decides whether the scalar field is phantom ($h < 0$) or canonical ($h > 0$); for negative $\alpha$ the kinetic term is positive. This is the mechanism that turns a phantom-scalar general-relativity source into an ordinary-scalar source in $f(Q)$ gravity while leaving the metric functions unchanged.

What would settle it

Compute the linear perturbation spectrum around the Simpson-Visser solution with $\alpha < 0$: if a ghost mode appears in the gravitational sector, the canonical-scalar interpretation loses physical meaning. More directly, the paper's own relation $h\Phi'^2 = -\alpha\,\Sigma''/\Sigma$ shows that no canonical scalar exists when $\alpha > 0$, so any independent constraint forcing $f_Q > 0$ falsifies the central claim.

Watch

Extended reading notes

Core claim

On its own terms, the paper's central claim is that the Simpson-Visser and Bardeen black-bounce metrics solve the $f(Q)$ field equations with the action built from $f(Q) - 2h(\Phi)\partial\Phi^2 + 2V(\Phi) + L(F)$, where the free function collapses to $f(Q) = \alpha Q + \beta$. In that setup the scalar-field equation forces $h\Phi'^2 = -\alpha\,\Sigma''/\Sigma$, and with the monotonic scalar $\Phi = \arctan(r/a)$ the coupling becomes constant $h(\Phi) = -\alpha$. Hence for negative integers $\alpha$, $h > 0$ and the scalar is canonical, in contrast to the phantom scalar that general relativity requires for these geometries. The paper also derives the potential $V(\Phi)$ and the non-linear electrodynamics Lagrangian $L(F)$ for both metric forms and verifies that at least one energy condition is violated in each case.

Load-bearing premise

The main assumption is that negative values of the constant $\alpha = f_Q$ are admissible in $f(Q)$ gravity; if $\alpha$ must be positive, the canonical scalar disappears and the source collapses back to the phantom scalar of general relativity.

Editorial extensions

If this is right

  • For negative integer $\alpha$, both Simpson-Visser and Bardeen black bounces admit closed-form sources with a canonical scalar, a periodic potential, and a positive non-linear electrodynamics Lagrangian.
  • At least one null energy condition is violated in each family, so the spacetimes still require exotic matter, though not a phantom kinetic term in the $f(Q)$ frame.
  • The magnetic charge $q$ coincides with the bounce regulator $a$, tying the source charge to the throat radius.
  • The derived $V(\Phi)$ and $L(F)$ can be used as input for thermodynamics, quasinormal-mode, or accretion studies of these spacetimes.
  • The energy-condition analysis reproduces the general-relativity theorem's conclusions for positive $\alpha$ (phantom scalar) and extends them to the negative-$\alpha$ ordinary-scalar sector.

Reading between the lines

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

  • If negative $\alpha$ is taken literally, the gravitational kinetic term $f_Q = \alpha$ is also negative, so the ordinary scalar comes with a ghost-like gravitational sector; in the Einstein-frame effective description the matter source is likely still phantom, meaning the improvement over general relativity may be a frame choice rather than physically ordinary matter.
  • The sign-flip mechanism suggests a general recipe: any general-relativity black bounce whose source is a phantom scalar can be re-expressed in $f(Q)$ with a canonical scalar by choosing $\alpha$ of the opposite sign, as long as negative $f_Q$ is allowed.
  • A natural testable extension, which the paper itself gestures at, is to repeat the reconstruction with electric instead of magnetic sources and check whether the sign of $h(\Phi)$ still flips.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. The manuscript reconstructs the matter sources (a scalar field with potential and a nonlinear electrodynamics Lagrangian) for Simpson-Visser and Bardeen-type black bounce metrics in f(Q) gravity with a magnetic charge. By assuming a linear f(Q) = alpha Q + beta with constant f_Q, choosing the scalar field ansatz Phi = arctan(r/a) and identifying a = q, the authors obtain h(Phi) = -alpha, explicit V(Phi) and L(F), and analyze energy conditions. They claim that for alpha < 0 the scalar field is ordinary (canonical), in contrast to general relativity, where a phantom scalar is required.

Significance. If the central claim were correct, the paper would demonstrate that black bounce spacetimes can be sourced by canonical scalar fields in modified gravity, an interesting extension of the known GR result. The algebra for the chosen ansatz is internally consistent, and the paper provides explicit source functions and energy-condition inequalities. However, the advertised novelty is undermined by the fact that alpha is the effective gravitational coupling in the linear f(Q) model: alpha < 0 introduces a ghost/anti-gravity sector, while alpha > 0 reproduces the GR phantom scalar. The paper therefore does not establish a physically new ordinary-scalar source, and the comparison with GR is a sign-convention artifact rather than a substantive difference.

major comments (3)
  1. [Section 3.1–3.2, Eqs. (31) and (39)] The claim that alpha < 0 yields an ordinary scalar field is not physically meaningful as stated. With f(Q) = alpha Q + beta, Eq. (18) reduces to G_mu_nu = (1/alpha)(T_mu_nu + beta/2 g_mu_nu), so alpha is the inverse gravitational coupling in units 8 pi G = 1. A negative alpha makes the gravitational kinetic term ghost-like, and h(Phi) = -alpha > 0 only makes the scalar canonical in a theory whose gravitational sector already has the wrong sign. Conversely, requiring a healthy alpha > 0 gives h(Phi) < 0, i.e., the same phantom scalar as in GR. The advertised difference from GR is therefore a sign convention in a ghostly linear f(Q) model, not a prediction of ordinary matter.
  2. [Eq. (35)] The relation dL/dF - L_F = 0 is tautological, because L_F was defined as dL/dF (see the text after Eq. (20)). As written, it cannot serve as a nontrivial consistency check for the reconstructed NLED functions. If a different condition is intended, it should be stated explicitly and verified.
  3. [Section 3, after Eq. (25)] The restriction to f(Q) = alpha Q + beta is a convenient choice, not the general solution of Eq. (25); the paper does not justify why this linear ansatz exhausts the possibilities relevant for black bounces. In addition, setting the bounce parameter equal to the magnetic charge, a = q in Eqs. (30) and (38), is an extra assumption that fixes a free parameter. The main conclusion that an ordinary scalar is possible depends on the sign of the freely chosen alpha; without a physical criterion selecting alpha < 0, or a non-linear f(Q) with f_Q > 0 and h > 0, the paper does not demonstrate a generic feature of f(Q) gravity.
minor comments (6)
  1. [Title and running header] The running header reads 'Black Bounces inf (Q) Gravity with Magnetic Source'; the word 'in' is corrupted.
  2. [Introduction] The name 'Simpson-Vissner' (near Eq. (14) discussion) should be 'Simpson-Visser'.
  3. [Abstract] The phrase 'As exact solutions are not obtained' is misleading: explicit expressions for the matter sources are obtained for the prescribed metric functions. Please rephrase to indicate that the metric functions are prescribed rather than solved self-consistently.
  4. [Section 4, Eqs. (50)–(53)] The energy-condition definitions contain formatting artifacts such as '⇐ ⇒' and inconsistent spacing; please use standard notation and define all symbols clearly.
  5. [Sections 4.1, 4.2, and 5] The text repeatedly refers to 'the integer alpha', but alpha is a real constant; only the plots use integer values. Please clarify that the solutions are valid for real alpha.
  6. [Section 3, Eq. (29)] The scalar field ansatz Phi = arctan(r/a) is described as 'without losing generality', but this is a restriction; please state it as an ansatz.

Circularity Check

2 steps flagged · score 6.0 of 10

The 'ordinary scalar field' result is the α<0 sign choice: h(Φ)=−α by construction, and α<0 makes the gravitational sector ghost-like, so the claimed contrast with GR is a parameter convention rather than a predicted outcome.

  1. self definitional [Section 3, after Eq. (25); Section 3.1, Eq. (31); Section 5, Conclusion]
    "According to this choice, hΦ′2 becomes a constant times the solution of general relativity; hΦ′2 = − αΣ′′ Σ . Following the previous works, and without losing generality, let the scalar field be assumed as a monotonic function Φ = arctan( r/ a ) ... h(Φ) = −α, (31) ... Unlike GR, a scalar field is canonical with positive kinetic energy, when α is a negative integer."

    The advertised 'ordinary scalar' is not an output of f(Q) dynamics. From Eq. (26) with f_Q=α and f_QQ=0, hΦ′^2 = −α Σ″/Σ. Substituting the assumed Φ=arctan(r/a) gives Φ′^2 = Σ″/Σ for both SV and Bardeen metrics, so h(Φ)=−α identically. Thus the sign of h, which the paper uses to label the scalar as canonical or phantom, is fixed by the free constant α. The paper's central contrast with GR ('only achieved by a phantom scalar field in general relativity') obtains only by choosing α<0. Moreover, with f(Q)=αQ+β, α is the gravitational coupling: Eq. (18) reduces to ˚G_μν=(1/α)(T_μν+β/2 g_μν), so α<0 flips the effective source sign; in the Einstein frame the scalar has kinetic coefficient h/α=−1, i.e. it is phantom.

  2. other [Section 3.1, Eq. (35); Section 3.2 after Eq. (42)]
    "where the NLED functions obey the relation; dL dF − LF = 0. (35) ... where the equation (35) is satisfied."

    Equation (35) is vacuous: LF was defined in Eq. (15) as LF = dL/dF, so dL/dF − LF = 0 is the tautology dL/dF − dL/dF = 0. The paper presents this as a relation satisfied by the constructed NLED Lagrangians, and later invokes it for the Bardeen case ('where the equation (35) is satisfied'), but it carries no independent information about the solutions. This is a cosmetic check, not a derived constraint.

full rationale

The paper performs a standard inverse reconstruction: it fixes the SV and Bardeen black-bounce metrics, takes a linear f(Q)=αQ+β, assumes Φ=arctan(r/a), and solves for h(Φ), V(Φ), and L(F). This reconstruction procedure itself is not circular: for a chosen ansatz, the field equations genuinely determine the source functions. The circularity enters with the paper's advertised novelty. The key relation h(Φ)=−α is obtained by construction, since Φ′^2=Σ″/Σ for the assumed scalar profile, and the sign of h is therefore exactly the sign of the free parameter α. The abstract's statement that f(Q) gravity can source these black bounces with an 'ordinary' scalar field, unlike GR's phantom scalar, is thus not a prediction of the theory but a selection of α<0. That same choice makes the gravitational term αQ have the wrong sign, and rewriting Eq. (18) shows the Einstein-frame source is inverted, so the effective scalar is still phantom. With the healthy gravitational coupling α>0, the scalar is phantom and the result reproduces the GR source. No independent derivation fixes α, so the central claim reduces to a parameter convention. The tautological Eq. (35) adds a secondary non-check. There are no load-bearing self-citations: the ansatz and GR theorem are cited from the literature, but the central reduction is internal to the paper's own equations.

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

No new particles or forces are introduced. The free parameters are the linear f(Q) constants and the charge identification. The main input is the sign freedom in f_Q, which drives the ordinary scalar field conclusion.

free parameters (3)
  • alpha (f_Q constant) = integer, e.g., -1, -2, 1, 2 in plots
    Chosen by hand. Negative alpha yields the canonical scalar field h = -alpha > 0, which is the paper's central claim. Positive alpha gives the phantom scalar. The physical viability of negative alpha is not examined.
  • beta (constant in f(Q) = alpha Q + beta) = integer, e.g., -1 or 0.05 in examples
    Chosen to satisfy some energy condition inequalities in the plots. It acts like a cosmological-constant term and is not independently determined.
  • a = q (bounce radius set equal to magnetic charge) = q, e.g., 0.05 in plots
    The Simpson-Visser regularization parameter is identified with the magnetic charge. This is a choice that connects the geometry to the NLED source but is not forced by the field equations.
assumptions (6)
  • domain assumption Static spherically symmetric metric ansatz and the flat torsion-free connection of Eq. (8)
    Restricts the spacetime class and fixes the non-coincident gauge used to compute the non-metricity scalar.
  • domain assumption Magnetic-only field with F23 = q sin(theta)
    Assumes no electric field and uses the Maxwell-Faraday equation to fix the magnetic field form, standard in NLED-sourced black bounce constructions.
  • domain assumption Monotonic scalar field Phi = arctan(r/a)
    Invoked without losing generality in Section 3, following Refs. [19,26,72]. This fixes the scalar profile and is used to convert r to Phi in the potential.
  • ad hoc to paper f(Q) = alpha Q + beta with f_Q constant
    After Eq. (25) the paper chooses f_Q to be constant rather than solving the full connection equation. Non-linear f(Q) solutions are excluded without justification.
  • ad hoc to paper Identification of the bounce parameter with the magnetic charge a = q
    This identification is used to express the NLED Lagrangian as a function of F, but it is not a consequence of the field equations.
  • domain assumption Anisotropic fluid energy conditions with separate mu > 0 and mu < 0 regions
    Standard approach for black bounce energy condition analysis, assuming the matter content can be represented as an anisotropic fluid.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Black Bounces in $f(Q)$ Gravity with Magnetic Source." pith.science (2026). https://pith.science/paper/JOHHOFLS

@misc{pith2026250522341,
  author       = {Pith},
  title        = {Pith review of: Black Bounces in $f(Q)$ Gravity with Magnetic Source},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/JOHHOFLS}},
  note         = {Machine review of arXiv:2505.22341}
}
abstract

In this study, the source of the black bounce is discussed in the context of $f(Q)$ theory. A body of research has been dedicated to the study of symmetric black bounce solutions that are generated by a combination of a scalar field with a non-zero potential and a magnetic charge within the framework of non-linear electrodynamics. As exact solutions are not obtained, the metric functions of Simpson-Visser and Bardeen type of black bounce are studied in the field equations. black bounce solutions are obtained by violating at least one energy condition for the Simpson-Visser and Bardeen type for an ordinary scalar field in $f(Q)$ gravity, which is only achieved by a phantom scalar field in general relativity.

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

72 extracted references · 71 canonical work pages

  1. [1]

    Observation of Gravitational Waves from a Binary Black Hole Merger,

    B. P. Abbott et al., “Observation of Gravitational Waves from a Binary Black Hole Merger,” Phys. Rev. Lett., vol. 116, no. 6, p. 061102, 2016

    2016

  2. [2]

    Multi-messenger Observations of a Binary Neutron Star Merger,

    B. P. Abbott et al., “Multi-messenger Observations of a Binary Neutron Star Merger,” Astrophys. J. Lett., vol. 848, no. 2, p. L12, 2017

    work page 2017

  3. [3]

    First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole,

    K. Akiyama et al., “First M87 Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole,” Astrophys. J. Lett., vol. 875, p. L1, 2019

    work page 2019

  4. [4]

    First Sagittarius A* Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole in the Center of the Milky Way,

    K. Akiyama et al., “First Sagittarius A* Event Horizon Telescope Results. I. The Shadow of the Supermassive Black Hole in the Center of the Milky Way,” Astrophys. J. Lett., vol. 930, no. 2, p. L12, 2022

    work page 2022

  5. [5]

    The Particle Problem in the General Theory of Relativity,

    A. Einstein and N. Rosen, “The Particle Problem in the General Theory of Relativity,” Phys. Rev., vol. 48, pp. 73–77, 1935

    work page 1935

  6. [6]

    Ether flow through a drainhole - a particle model in general relativity,

    H. G. Ellis, “Ether flow through a drainhole - a particle model in general relativity,” J. Math. Phys., vol. 14, pp. 104–118, 1973

    work page 1973

  7. [7]

    Scalar-tensor theory and scalar charge,

    K. A. Bronnikov, “Scalar-tensor theory and scalar charge,” Acta Phys. Polon. B, vol. 4, pp. 251–266, 1973

    work page 1973

  8. [8]

    Wormholes in space-time and their use for interstellar travel: A tool for teaching general relativity,

    M. S. Morris and K. S. Thorne, “Wormholes in space-time and their use for interstellar travel: A tool for teaching general relativity,” Am. J. Phys., vol. 56, pp. 395–412, 1988

    work page 1988

Show all 72 references
  1. [9]

    Energy and momentum of higher dimensional black holes,

    M. Ulu Do˜ gru et al., “Energy and momentum of higher dimensional black holes,” International Journal of Theoretical Physics, vol. 51, pp. 1545–1554, 2012

    2012

  2. [10]

    Non-singular general relativistic gravitational collapse,

    B. J., “Non-singular general relativistic gravitational collapse,” in Proceedings of the International Conference GR5,Tbilisi, U.S.S.R

  3. [11]

    Bambi, ed., Regular Black Holes

    C. Bambi, ed., Regular Black Holes. Towards a New Paradigm of Gravitational Collapse. Springer Series in Astrophysics and Cosmology, Springer, 2023

    2023

  4. [12]

    Stable gravastars—an alternative to black holes?,

    M. Visser and D. L. Wiltshire, “Stable gravastars—an alternative to black holes?,” Classical and Quantum Gravity, vol. 21, p. 1135–1151, Jan. 2004

    2004

  5. [13]

    Traversable wormholes: Some simple examples,

    M. Visser, “Traversable wormholes: Some simple examples,” Phys. Rev. D, vol. 39, pp. 3182–3184, 1989

    1989

  6. [14]

    Black-bounce to traversable wormhole,

    A. Simpson and M. Visser, “Black-bounce to traversable wormhole,” JCAP, vol. 02, p. 042, 2019

    2019

  7. [15]

    Novel black- bounce spacetimes: Wormholes, regularity, energy conditions, and causal structure,

    F. S. Lobo, M. E. Rodrigues, M. V. d. S. Silva, A. Simpson, and M. Visser, “Novel black- bounce spacetimes: Wormholes, regularity, energy conditions, and causal structure,” Physical Review D, vol. 103, Apr. 2021

    2021

  8. [16]

    Embedding regular black holes and black bounces in a cloud of strings,

    M. E. Rodrigues and M. V. d. S. Silva, “Embedding regular black holes and black bounces in a cloud of strings,” Phys. Rev. D, vol. 106, no. 8, p. 084016, 2022

    2022

  9. [17]

    Black-bounces with multiple throats and anti-throats,

    M. E. Rodrigues and M. V. d. S. Silva, “Black-bounces with multiple throats and anti-throats,” Classical and Quantum Gravity, vol. 40, p. 225011, Oct. 2023

    2023

  10. [18]

    Spherically symmetric and static black bounces with multiple horizons, throats, and anti-throats in four dimensions,

    M. E. Rodrigues and M. V. de S Silva, “Spherically symmetric and static black bounces with multiple horizons, throats, and anti-throats in four dimensions,” Classical and Quantum Gravity, vol. 42, p. 055005, Feb. 2025

    2025

  11. [19]

    Black bounces, wormholes, and partly phantom scalar fields,

    K. A. Bronnikov, “Black bounces, wormholes, and partly phantom scalar fields,” Phys. Rev. D, vol. 106, no. 6, p. 064029, 2022

    2022

  12. [20]

    Field sources for simpson-visser spacetimes,

    K. A. Bronnikov and R. K. Walia, “Field sources for simpson-visser spacetimes,” Physical Review D, vol. 105, Feb. 2022

    2022

  13. [21]

    Novel black-bounce spacetimes: wormholes, regularity, energy conditions, and causal structure,

    F. S. N. Lobo, M. E. Rodrigues, M. V. de Sousa Silva, A. Simpson, and M. Visser, “Novel black-bounce spacetimes: wormholes, regularity, energy conditions, and causal structure,” Phys. Rev. D, vol. 103, no. 8, p. 084052, 2021

    2021

  14. [22]

    Source of black bounces in general relativity,

    M. E. Rodrigues and M. V. d. S. Silva, “Source of black bounces in general relativity,” Phys. Rev. D, vol. 107, no. 4, p. 044064, 2023

    2023

  15. [23]

    Cylindrical black bounces and their field sources,

    K. A. Bronnikov, M. E. Rodrigues, and M. V. de S. Silva, “Cylindrical black bounces and their field sources,” Phys. Rev. D, vol. 108, no. 2, p. 024065, 2023

    2023

  16. [24]

    New sources of ghost fields in k-essence theories for black-bounce solutions,

    C. F. S. Pereira, D. C. Rodrigues, E. L. Martins, J. C. Fabris, and M. E. Rodrigues, “New sources of ghost fields in k-essence theories for black-bounce solutions,” Class. Quant. Grav., vol. 42, no. 1, p. 015001, 2025. 14 REFERENCES

    2025

  17. [25]

    Magnetically charged black-bounce solution via nonlinear electrodynamics in a k-essence theory,

    C. F. S. Pereira, D. C. Rodrigues, M. V. d. S. Silva, J. C. Fabris, M. E. Rodrigues, and H. Belich, “Magnetically charged black-bounce solution via nonlinear electrodynamics in a k-essence theory,” Phys. Rev. D, vol. 111, no. 8, p. 084025, 2025

    2025

  18. [26]

    Generalized black-bounces solutions in f(R) gravity and their field sources,

    M. V. d. S. Silva, T. M. Crispim, G. Alencar, R. R. Landim, and M. E. Rodrigues, “Generalized black-bounces solutions in f(R) gravity and their field sources,” 2 2025

    2025

  19. [27]

    Novel electrically charged wormhole, black hole and black bounce exact solutions in hybrid metric-Palatini gravity,

    G. I. R´ ois, J. T. S. S. Junior, F. S. N. Lobo, and M. E. Rodrigues, “Novel electrically charged wormhole, black hole and black bounce exact solutions in hybrid metric-Palatini gravity,” 12 2024

    2024

  20. [28]

    Black bounces in Cotton gravity,

    E. L. B. Junior, J. T. S. S. Junior, F. S. N. Lobo, M. E. Rodrigues, D. Rubiera-Garcia, L. F. D. da Silva, and H. A. Vieira, “Black bounces in Cotton gravity,” Eur. Phys. J. C, vol. 84, no. 11, p. 1190, 2024

    2024

  21. [29]

    Black bounces in conformal Killing gravity,

    J. T. S. S. Junior, F. S. N. Lobo, and M. E. Rodrigues, “Black bounces in conformal Killing gravity,” Eur. Phys. J. C, vol. 84, no. 6, p. 557, 2024

    2024

  22. [30]

    Source of black bounces in Rastall gravity,

    K. Atazadeh and H. Hadi, “Source of black bounces in Rastall gravity,” JCAP, vol. 01, p. 067, 2024

    2024

  23. [31]

    Cylindrically symmetric unimodular f (r) black holes,

    H. Aydın and M. U. Do˜ gru, “Cylindrically symmetric unimodular f (r) black holes,” International Journal of Geometric Methods in Modern Physics , vol. 18, no. 07, p. 2150101, 2021

    2021

  24. [32]

    The farthest known supernova: support for an accelerating universe and a glimpse of the epoch of deceleration,

    A. G. Riess et al., “The farthest known supernova: support for an accelerating universe and a glimpse of the epoch of deceleration,” Astrophys. J., vol. 560, pp. 49–71, 2001

    2001

  25. [33]

    Cosmological parameters from SDSS and WMAP,

    M. Tegmark et al., “Cosmological parameters from SDSS and WMAP,” Phys. Rev. D, vol. 69, p. 103501, 2004

    2004

  26. [34]

    Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies,

    D. J. Eisenstein et al., “Detection of the Baryon Acoustic Peak in the Large-Scale Correlation Function of SDSS Luminous Red Galaxies,”Astrophys. J., vol. 633, pp. 560– 574, 2005

    2005

  27. [35]

    Baryon Acoustic Oscillations in the Sloan Digital Sky Survey Data Release 7 Galaxy Sample,

    W. J. Percival et al., “Baryon Acoustic Oscillations in the Sloan Digital Sky Survey Data Release 7 Galaxy Sample,” Mon. Not. Roy. Astron. Soc., vol. 401, pp. 2148–2168, 2010

    2010

  28. [36]

    Coincident General Relativity,

    J. Beltr´ an Jim´ enez, L. Heisenberg, and T. Koivisto, “Coincident General Relativity,” Phys. Rev. D, vol. 98, no. 4, p. 044048, 2018

    2018

  29. [37]

    Exploring traversable wormholes in f(Q) gravity: Shadows and quasinormal modes,

    M. Chakraborty and S. Chakraborty, “Exploring traversable wormholes in f(Q) gravity: Shadows and quasinormal modes,” Nucl. Phys. B, vol. 1017, p. 116939, 2025

    2025

  30. [38]

    Cosmology inf (Q) geometry,

    J. Beltr´ an Jim´ enez, L. Heisenberg, T. S. Koivisto, and S. Pekar, “Cosmology inf (Q) geometry,” Phys. Rev. D, vol. 101, no. 10, p. 103507, 2020

    2020

  31. [39]

    Stability Properties of Self-Similar Solutions in Symmetric Telepar- allel f(Q)-Cosmology,

    A. Paliathanasis, “Stability Properties of Self-Similar Solutions in Symmetric Telepar- allel f(Q)-Cosmology,” Symmetry, vol. 15, no. 2, p. 529, 2023

    2023

  32. [40]

    Dynamical analysis of fQ-cosmology,

    A. Paliathanasis, “Dynamical analysis of fQ-cosmology,” Phys. Dark Univ., vol. 41, p. 101255, 2023

    2023

  33. [41]

    Can f (Q) gravity challenge ΛCDM?,

    L. Atayde and N. Frusciante, “Can f (Q) gravity challenge ΛCDM?,” Phys. Rev. D, vol. 104, no. 6, p. 064052, 2021

    2021

  34. [42]

    Reconstructing isotropic and anisotropic f(Q) cosmologies,

    F. Esposito, S. Carloni, R. Cianci, and S. Vignolo, “Reconstructing isotropic and anisotropic f(Q) cosmologies,” Phys. Rev. D, vol. 105, no. 8, p. 084061, 2022

    2022

  35. [43]

    Late-time acceleration in f(Q) gravity: Analysis and constraints in an anisotropic background,

    M. Koussour, K. El Bourakadi, S. H. Shekh, S. K. J. Pacif, and M. Bennai, “Late-time acceleration in f(Q) gravity: Analysis and constraints in an anisotropic background,” Annals Phys., vol. 445, p. 169092, 2022

    2022

  36. [44]

    Thermodynamical aspects of Bianchi type-I Universe in quadratic form of f(Q) gravity and observational constraints,

    M. Koussour, S. H. Shekh, M. Govender, and M. Bennai, “Thermodynamical aspects of Bianchi type-I Universe in quadratic form of f(Q) gravity and observational constraints,” JHEAp, vol. 37, pp. 15–24, 2023

    2023

  37. [45]

    Anisotropic nature of space–time in fQ gravity,

    M. Koussour, S. H. Shekh, and M. Bennai, “Anisotropic nature of space–time in fQ gravity,” Phys. Dark Univ., vol. 36, p. 101051, 2022

    2022

  38. [46]

    Phantom dark energy nature of bulk-viscosity universe in modified f(Q)-gravity,

    A. Dixit, D. C. Maurya, and A. Pradhan, “Phantom dark energy nature of bulk-viscosity universe in modified f(Q)-gravity,” Int. J. Geom. Meth. Mod. Phys., vol. 19, no. 12, p. 2250198, 2022

    2022

  39. [47]

    Anisotropic LRS-BI Universe with f(Q) gravity REFERENCES 15 theory,

    P. Sarmah, A. De, and U. D. Goswami, “Anisotropic LRS-BI Universe with f(Q) gravity REFERENCES 15 theory,” Phys. Dark Univ., vol. 40, p. 101209, 2023

    2023

  40. [48]

    Quintessence Behavior of an Anisotropic Bulk Viscous Cosmological Model in Modified f(Q)-Gravity,

    A. Pradhan, A. Dixit, and D. C. Maurya, “Quintessence Behavior of an Anisotropic Bulk Viscous Cosmological Model in Modified f(Q)-Gravity,” Symmetry, vol. 14, no. 12, p. 2630, 2022

    2022

  41. [49]

    Dark energy stars and quark stars within the context of f(Q) gravity,

    P. Bhar and J. M. Z. Pretel, “Dark energy stars and quark stars within the context of f(Q) gravity,” Phys. Dark Univ., vol. 42, p. 101322, 2023

    2023

  42. [50]

    Physical characteristics and maximum allowable mass of hybrid star in the context of f(Q) gravity,

    P. Bhar, S. Pradhan, A. Malik, and P. K. Sahoo, “Physical characteristics and maximum allowable mass of hybrid star in the context of f(Q) gravity,” Eur. Phys. J. C, vol. 83, no. 7, p. 646, 2023

    2023

  43. [51]

    FLR W solu- tions in f(Q) theory: The effect of using different connections,

    N. Dimakis, A. Paliathanasis, M. Roumeliotis, and T. Christodoulakis, “FLR W solu- tions in f(Q) theory: The effect of using different connections,” Phys. Rev. D, vol. 106, no. 4, p. 043509, 2022

    2022

  44. [52]

    Self-similar cosmological solutions in symmetric teleparallel the- ory: Friedmann-Lema ˆ ıtre-Robertson-Walker spacetimes,

    N. Dimakis, M. Roumeliotis, A. Paliathanasis, P. S. Apostolopoulos, and T. Christodoulakis, “Self-similar cosmological solutions in symmetric teleparallel the- ory: Friedmann-Lema ˆ ıtre-Robertson-Walker spacetimes,”Phys. Rev. D, vol. 106, no. 12, p. 123516, 2022

    2022

  45. [53]

    Slow-roll inflation in f(Q) non-metric gravity,

    S. Capozziello and M. Shokri, “Slow-roll inflation in f(Q) non-metric gravity,” Phys. Dark Univ., vol. 37, p. 101113, 2022

    2022

  46. [54]

    Black holes in f(Q) gravity,

    F. D’Ambrosio, S. D. B. Fell, L. Heisenberg, and S. Kuhn, “Black holes in f(Q) gravity,” Phys. Rev. D, vol. 105, no. 2, p. 024042, 2022

    2022

  47. [55]

    Thermodynamics of Charged Black Hole in Symmetric Teleparallel Gravity,

    F. Javed, G. Fatima, S. Sadiq, and G. Mustafa, “Thermodynamics of Charged Black Hole in Symmetric Teleparallel Gravity,” Fortsch. Phys., vol. 71, no. 6-7, p. 2200214, 2023

    2023

  48. [56]

    Thermal analysis with emission energy of perturbed black hole in f(Q) gravity,

    F. Javed, G. Mustafa, S. Mumtaz, and F. Atamurotov, “Thermal analysis with emission energy of perturbed black hole in f(Q) gravity,”Nucl. Phys. B, vol. 990, p. 116180, 2023

    2023

  49. [57]

    Coincident f (Q) gravity: black holes, regular black holes, and black bounces,

    J. T. S. S. Junior and M. E. Rodrigues, “Coincident f (Q) gravity: black holes, regular black holes, and black bounces,” Eur. Phys. J. C, vol. 83, no. 6, p. 475, 2023

    2023

  50. [58]

    Quasinormal modes of black holes in f(Q) gravity,

    D. J. Gogoi, A. ¨Ovg¨ un, and M. Koussour, “Quasinormal modes of black holes in f(Q) gravity,” Eur. Phys. J. C, vol. 83, no. 8, p. 700, 2023

    2023

  51. [59]

    Black hole solutions in scalar-tensor symmetric teleparallel gravity,

    S. Bahamonde, J. Gigante Valcarcel, L. J¨ arv, and J. Lember, “Black hole solutions in scalar-tensor symmetric teleparallel gravity,” JCAP, vol. 08, p. 082, 2022

    2022

  52. [60]

    Wormhole geometries in f (Q) gravity and the energy conditions,

    A. Banerjee, A. Pradhan, T. Tangphati, and F. Rahaman, “Wormhole geometries in f (Q) gravity and the energy conditions,” Eur. Phys. J. C, vol. 81, no. 11, p. 1031, 2021

    2021

  53. [61]

    New spherically symmetric wormhole solutions in f (Q)-gravity theory,

    S. Kiroriwal, J. Kumar, S. K. Maurya, and S. Chaudhary, “New spherically symmetric wormhole solutions in f (Q)-gravity theory,” Phys. Scripta, vol. 98, no. 12, p. 125305, 2023

    2023

  54. [62]

    Relativistic wormhole surrounded by dark mat- ter halos in symmetric teleparallel gravity,

    G. Mustafa, S. K. Maurya, and S. Ray, “Relativistic wormhole surrounded by dark mat- ter halos in symmetric teleparallel gravity,” Fortsch. Phys., vol. 71, no. 6-7, p. 2200129, 2023

    2023

  55. [63]

    Stable traversable wormholes in f(Q) gravity,

    N. Godani, “Stable traversable wormholes in f(Q) gravity,” Int. J. Geom. Meth. Mod. Phys., vol. 20, no. 08, p. 2350128, 2023

    2023

  56. [64]

    Yukawa–Casimir Wormholes in f(Q) Gravity,

    A. K. Mishra, Shweta, and U. K. Sharma, “Yukawa–Casimir Wormholes in f(Q) Gravity,” Universe, vol. 9, no. 4, p. 161, 2023

    2023

  57. [65]

    GUP corrected Casimir wormholes in f(Q) gravity,

    Z. Hassan, S. Ghosh, P. K. Sahoo, and V. S. H. Rao, “GUP corrected Casimir wormholes in f(Q) gravity,” Gen. Rel. Grav., vol. 55, no. 8, p. 90, 2023

    2023

  58. [66]

    Casimir wormholes in modified symmetric teleparallel gravity,

    Z. Hassan, S. Ghosh, P. K. Sahoo, and K. Bamba, “Casimir wormholes in modified symmetric teleparallel gravity,” Eur. Phys. J. C, vol. 82, no. 12, p. 1116, 2022

    2022

  59. [67]

    Wormhole in f(Q) gravity,

    F. Parsaei, S. Rastgoo, and P. K. Sahoo, “Wormhole in f(Q) gravity,” Eur. Phys. J. Plus, vol. 137, no. 9, p. 1083, 2022

    2022

  60. [68]

    Traversable wormholes with charge and non-commutative geometry in the f(Q) gravity,

    O. Sokoliuk, Z. Hassan, P. K. Sahoo, and A. Baransky, “Traversable wormholes with charge and non-commutative geometry in the f(Q) gravity,” Annals Phys., vol. 443, p. 168968, 2022

    2022

  61. [69]

    Traversable Wormhole in f (Q) Gravity Using Conformal Symmetry,

    M. Jan, A. Ashraf, A. Basit, A. Caliskan, and E. G¨ udekli, “Traversable Wormhole in f (Q) Gravity Using Conformal Symmetry,” Symmetry, vol. 15, no. 4, p. 859, 2023. 16 REFERENCES

    2023

  62. [70]

    Covariant formulation of f(Q) theory,

    D. Zhao, “Covariant formulation of f(Q) theory,” Eur. Phys. J. C, vol. 82, no. 4, p. 303, 2022

    2022

  63. [71]

    Spherically symmetric configuration in f (Q) gravity,

    R.-H. Lin and X.-H. Zhai, “Spherically symmetric configuration in f (Q) gravity,” Phys. Rev. D, vol. 103, no. 12, p. 124001, 2021. [Erratum: Phys.Rev.D 106, 069902 (2022)]

    2022

  64. [72]

    Field Sources for f (R, Rµν ) Black-Bounce Solutions: The Case of K-Gravity,

    G. Alencar, M. Nilton, M. E. Rodrigues, and M. V. d. S. Silva, “Field Sources for f (R, Rµν ) Black-Bounce Solutions: The Case of K-Gravity,” 9 2024

    2024

Pith tools

Reviewed August 7, 2026 · model on record in the stance chip above.