Pith. sign in

REVIEW 3 major objections 6 minor 1 cited by

Unitary quantum matter-bounce in a universe with a positive cosmological constant

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

Pith's one-line read A hydrogen-atom map turns the Big Bang into a quantum bounce

desk verdict A clean exactly solvable minisuperspace model with a hydrogen-atom analogy, but the bounce is an input (Dirichlet boundary condition) rather than a robust output of unitary dynamics. read the letter →

arxiv 2505.16863 v2 pith:FGDZOZGR submitted 2025-05-22 gr-qc astro-ph.COhep-th

classification gr-qcastro-ph.COhep-th MSC 83C4583F0581Q05 PACS 04.60.-m98.80.Qc
keywords quantumcosmologyWheeler-DeWittequationunimodularclockBrown-Kuchařdustbouncehydrogenatomanalogysingularityresolutioncosmologicalconstant
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 analyzes a spatially flat universe containing pressureless dust and a positive cosmological constant, quantized through the Wheeler-DeWitt equation with unimodular time as the clock. It establishes that the quantum dynamics are exactly solvable because the Wheeler-DeWitt equation becomes the radial Schrödinger equation for scattering states of a hydrogen atom, with volume playing the role of radius, the dust density playing the role of Coulomb strength, and the cosmological constant playing the role of energy. Using normalized scattering states, the authors build wave packets that evolve unitarily in unimodular time and show that the expectation value of the volume bounces at a positive minimum instead of reaching zero. If correct, the classical Big Bang singularity is replaced by a quantum bounce, and the model supplies a concrete, unitary quantum origin for the contracting phase needed in matter-bounce cosmology.

What carries the argument

The load-bearing object is the exact mapping between the Wheeler-DeWitt equation and the $l=0$ radial Schrödinger equation of the hydrogen atom: the volume variable $v\leftrightarrow r$, the cosmological constant $\Lambda\leftrightarrow E$, the dust term $\rho_0/v\leftrightarrow$ the Coulomb potential, and the wave function $\psi(v)\leftrightarrow u(r)$. This correspondence turns the positive-$\Lambda$ sector into hydrogen scattering states, gives an explicit delta-normalized basis, permits the self-adjointness analysis of the unimodular Hamiltonian using known results for half-line Coulomb-type operators, and supplies the normalization coefficients used to build the wave packets whose evolution exhibits the bounce.

What would settle it

Compute the reduced density matrix evolution for a wave packet with a broad, non-peaked distribution $B(\rho_0)$ instead of the sharply peaked one; if the $\langle v\rangle$ trajectory develops a vanishing minimum or the norm fails to stay constant in unimodular time, the bounce is an artifact of the $\rho_0$-reduction. A second check is to quantize with the dust clock $T$ and test whether normalized orthonormal stationary states exist; if they do not and the dust-clock theory is non-unitary, the bounce is clock-dependent.

Watch

Extended reading notes

Core claim

The central claim is that for a flat FLRW universe with dust and $\Lambda>0$, the Wheeler-DeWitt quantization with the unimodular clock yields a unitary quantum theory whose stationary states are Coulomb scattering states. The unimodular Hamiltonian is self-adjoint on $L^2(\mathbb{R}_+, dv)$ after choosing the boundary condition that selects Kummer functions of the first kind, so the spectrum includes a continuous part for $\Lambda>0$. $\Delta$-normalized scattering states are used to construct normalized wave packets, and their numerical evolution shows the probability density vanishing at $v=0$ at all times, $\langle v\rangle$ tracing a bounce with positive minimum, and an effective Hubble parameter that vanishes at the bounce and matches the classical value far away. The paper therefore claims the Big Bang singularity is resolved within the model rather than merely avoided by a boundary condition.

Load-bearing premise

The dust energy density $\rho_0$ is treated as a fixed c-number after the dust variable is traced out; the bounce and unitarity are proven only for this reduced model, whose validity rests on the state being sharply peaked in $\rho_0$, an assumption asserted rather than demonstrated for the constructed wave packets.

Editorial extensions

If this is right

  • The classical $v=0$ singularity is replaced by a bounce: $\langle v\rangle$ reaches a positive minimum and the probability density vanishes at $v=0$ for all clock times.
  • Away from the bounce the wave packet becomes a single-peaked semiclassical state tracking the classical trajectory, so the model connects quantum and classical cosmology.
  • The effective Hubble parameter for the quantum-corrected metric vanishes at the bounce and asymptotes to $\sqrt{\Lambda/3}$, supporting a contracting-then-expanding history.
  • Because the background bounces during a dust-dominated contracting phase, the model provides a unitary quantum origin for the matter-bounce scenario's prerequisite stage for generating a scale-invariant primordial spectrum.
  • Relative volume fluctuations do not decay to zero in the late universe, so quantum effects could persist into the de Sitter phase rather than vanishing.

Reading between the lines

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

  • Beyond the paper: if the unitary bounce survives in the full two-clock theory, the same hydrogen-atom toolkit could be used to compute cosmological perturbations on the bouncing background, turning the qualitative matter-bounce prerequisite into a quantitative prediction.
  • Beyond the paper: the $\Lambda<0$ sector's discrete spectrum, if interpreted as a quantization of the cosmological constant, suggests a testable selection rule for $\Lambda$ determined by dust content; the paper only announces this and leaves it to the companion paper.
  • Beyond the paper: a direct numerical check of the dust-clock quantization without the $\rho_0$ c-number reduction would determine whether the bounce is clock-dependent, extending the paper's remark that dust-clock orthonormality is hard to establish.
  • Beyond the paper: the persistent late-time fluctuations could be mapped to observables in the quantum-corrected metric, offering a way to look for imprints of quantum gravity in late-time cosmological measurements.
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. This paper studies the Wheeler-DeWitt quantization of a spatially flat FLRW universe with pressureless dust (Brown-Kuchař formalism) and a positive cosmological constant introduced via unimodular gravity. The authors show that the quantum dynamics reduces to a radial Schrödinger equation with a Coulomb-like potential and exploit the analogy with the hydrogen atom to write stationary solutions in terms of confluent hypergeometric functions. For Λ > 0 they construct normalized scattering-type states, superpose them with a Poisson-like weight over k, and numerically evolve the resulting wave packets. They report a quantum bounce: the probability density vanishes at the classical singularity v = 0, the expectation value ⟨v⟩ has a nonzero minimum, and the wave packet tracks the classical trajectory away from the bounce. They also compute relative volume fluctuations and derive an effective Hubble parameter, concluding that quantum effects persist at late times. The central claims are that the unimodular Hamiltonian is self-adjoint, that the evolution is unitary, and that the Big Bang singularity is replaced by a robust quantum bounce.

Significance. The hydrogen-atom analogy is a valuable and pedagogically appealing addition to the quantum-cosmology toolkit, and the analytic form of the stationary states enables a controlled numerical investigation of wave-packet dynamics. The paper includes explicit numerical norm-conservation checks and constructs normalizable wave packets, which are concrete strengths. If the central claims were fully established, the model would provide an exactly solvable example of singularity resolution in quantum cosmology and a useful testbed for relational-time frameworks. However, the claimed robustness of the bounce is not established: the result depends crucially on the choice of a particular self-adjoint extension, and the text does not deliver the promised proof of self-adjointness. The paper is therefore best viewed as an instructive toy model rather than a definitive resolution of the Big Bang singularity.

major comments (3)
  1. [III C, Eq. (48) and boundary condition after Eq. (60)] The abstract and introduction state that the paper ensures self-adjointness of the unimodular Hamiltonian, but Section III C only says that the authors proceed 'based on generalizations of analyses like that in Ref. [58]'; no proof is provided. More importantly, the choice of the self-adjoint extension parameter ε = π/2 is justified only by convenience and by the fact that it discards the Tricomi U solutions, which do not vanish at v = 0. Because the vanishing of the wave function at v = 0 is a direct consequence of setting a2 = 0, the singularity resolution and the bounce are an input of the boundary condition rather than a generic output of the Wheeler-DeWitt dynamics. To support the central claim of a robust quantum bounce, the authors must either derive this boundary condition from the physical model or show that the DeWitt criterion and the bounce persist for other members of the U(1) family of self-adjoint extensions.
  2. [Appendix A, Eqs. (A11), (A14)-(A16), and Eq. (61)] The derivation of the continuous-spectrum normalization contains a sign error. Eq. (A9) gives (−i)^{-1−i2ρ0/(3k)} = e^{−πρ0/(3k)+iπ/2}, but Eqs. (A11) and (A14) write e^{+πρ0/(3k)}. As a result, the step from Eq. (A14) to Eq. (A16) is inconsistent: with the sign as printed, the required coefficient would contain e^{−πρ0/(3k)}, whereas Eq. (A16) has e^{+πρ0/(3k)}. Once the sign in Eqs. (A11) and (A14) is corrected, the final coefficient in Eq. (A17) is consistent with the standard hydrogen-atom scattering-state normalization; but as written the derivation is not self-consistent. The authors should fix the sign error and re-verify the wave-packet normalization condition in Eq. (67) with the corrected derivation.
  3. [III B, Eqs. (53)-(55)] The reduction of the dust momentum to a c-number ρ0 is justified by the statement that the system is 'sharply peaked in ρ0'. However, the paper never constructs or tests such a peaked state; all subsequent wave packets in Section IV use a fixed ρ0 and contain only a superposition over Λ. The reduced density operator in Eq. (55) is asserted to be approximately pure for a sharply peaked B(ρ0), but no consistency check with a finite-width distribution is provided. The unitary bounce is therefore established only for the reduced, effectively single-particle model. The paper should state this limitation explicitly in the conclusions or provide a numerical check with a nonzero-width B(ρ0) to show that the bounce is not an artifact of the reduction.
minor comments (6)
  1. [Abstract and Introduction] The abstract and the introduction claim that the paper 'proves' self-adjointness and 'rigorously constructs' the physical Hilbert space, but the text in Section III C explicitly relies on 'generalizations of analyses' from the literature. The language should be aligned with what is actually demonstrated.
  2. [Figure 2] In the heatmaps of Figure 2, the classical trajectory (dotted black line) and the expectation value ⟨v⟩ (solid black line) are nearly indistinguishable in gray scale; please use distinct colors or line styles and label them clearly.
  3. [Eq. (61)] There is a typo in Eq. (61): the argument of the Kummer function is written as '2ikvv', which should be '2ikv'.
  4. [Figure captions, Figures 2-5] The captions for Figures 2-5 do not list the fixed parameters (ρ0, λ, κ values, Λmean) used in each panel; please include the parameter values in the captions or in a table.
  5. [Eq. (69) and surrounding text] The weight A(k) in Eq. (69) is called a 'Λ-distribution', but it is a function of k; clarify that the distribution is over k and that Λ = 3k²/4, or call it a k-distribution.
  6. [Reference [46]] The companion paper [46] is cited without an arXiv identifier, journal reference, or publication status; please provide an arXiv number or other accessible citation so that readers can verify the claimed extensions.

Circularity Check

1 steps flagged · score 6.0 of 10

Singularity resolution is encoded in the chosen ε=π/2 self-adjoint extension, not derived from the Wheeler-DeWitt dynamics; the wave-packet results themselves are genuine numerical output.

  1. self definitional [Section III C (Self-adjoint extension); applied in Section III D and Section IV]
    "Following Ref. [58], the self-adjoint extension corresponding to ϵ = π/2 is particularly convenient. This choice implies a2 = 0, meaning that the solutions involving the hypergeometric function of the second kind (U) do not contribute to the eigenfunctions of this specific self-adjoint Hamiltonian. This selection is crucial for deriving standard orthonormality relations based on the hypergeometric functions of the first kind (F), which are essential for constructing unitarily evolving wave packets. Other choices of ϵ ̸= π/2 would include contributions from U functions [51, 58]."

    Under a1 cos ε = a2 sin ε, the choice ε=π/2 forces a2=0, so only the Kummer-F solution survives. That solution has ψ^1_k(v)=const·v+O(v²) (Eq. (61)); the discarded Tricomi-U solution would be non-vanishing at v=0. Section III D then identifies 'Ψ(v)→0' with DeWitt's singularity-avoidance criterion, and Section IV reports that 'the probability distribution associated with the wave packet vanishes at v = 0 for all times' as the demonstration of the quantum bounce. The claimed singularity resolution is therefore exactly the Dirichlet boundary condition chosen for convenience in defining the self-adjoint Hamiltonian: it is an input to the quantization, not a dynamical output.

full rationale

Most of the derivation is self-contained: the hydrogen-atom mapping, the spectral construction, and the numerical wave-packet evolution are genuine calculations, and the Poisson weight (Eq. (69)) is chosen for tractability rather than fitted to the bounce. The self-citations [22,23] are used only for qualitative comparison of fluctuation trends and are not load-bearing. The dust-c-number reduction (Sec. III B) is an asserted assumption (sharply peaked ρ0) rather than a proved reduction, but it is not circular. Appendix A's asymptotic normalization of the Kummer states is an evidentiary gap—the paper relies on the asymptotic method of [59], notes that orthonormality of these functions is 'scarcely studied,' and verifies norm conservation only numerically—but that is a proof gap, not circularity. The central circular step is the self-adjoint extension: Sec. III C selects ε=π/2 within a U(1) family of extensions, discarding the Tricomi-U solution. The retained F solution vanishes linearly at v=0 by construction, and Sec. III D presents this linear vanishing as the DeWitt singularity-avoidance criterion; Sec. IV presents the same vanishing as the demonstration of the quantum bounce. The paper is transparent that the choice is 'particularly convenient,' and the wave-packet ringing, expectation values, and late-time fluctuations are independent outputs within that chosen extension. Nevertheless, the singularity-resolution claim reduces by construction to the chosen boundary condition, so the analysis is partially circular. Score 6 reflects that partial reduction rather than total circularity.

Assumptions & free parameters 3 free parameters · 8 assumptions · 0 invented entities

The model rests on two standard gauge-fixing formalisms (Brown-Kuchar dust, unimodular gravity), a chosen operator ordering, a c-number reduction of the dust sector, and ad hoc choices of self-adjoint extension and wave packet weight. The bounce follows from these inputs; none of them is fitted to the bounce.

free parameters (3)
  • Poisson weight scale λ = λ = 1 in the figures
    Set to 1; controls the mean Λ via Λ̄ = 3(1+κ)/(4λ).
  • Poisson weight shape κ = κ = 0.8 to 80 in the figures
    Shapes the Λ-distribution and controls the quantum fluctuations; not derived.
  • Self-adjoint extension angle ε = ε = π/2
    Boundary condition a2=0 excluding Tricomi U solutions; adopted to make the F-function basis orthonormal.
assumptions (8)
  • domain assumption Brown-Kuchar dust fields provide a physical clock via T and dust momentum ρ₀.
    Used in Sec. II to build the action Eq. (8).
  • domain assumption The cosmological constant is dynamical via unimodular gravity, with conjugate variable T.
    Introduced in Sec. II, Eqs. (7)-(9).
  • domain assumption The Hamiltonian constraint is quantized with trivial operator ordering, giving Eq. (39).
    Sec. III, first paragraph.
  • ad hoc to paper The dust momentum is reduced to a c-number ρ₀ by assuming a sharply peaked state in ρ₀.
    Sec. III B: “we bypass these issues by working in an effective description”.
  • standard math The operator -d²/dv² + ρ₀/v on L²(R⁺,dv) has deficiency indices (1,1) and admits U(1) self-adjoint extensions.
    Sec. III C, based on Ref. [58].
  • ad hoc to paper The self-adjoint extension ε=π/2 is the physically relevant one.
    Sec. III C: “particularly convenient”.
  • ad hoc to paper The initial state of the universe is a Poisson-like superposition A(k) of stationary states.
    Sec. IV, Eq. (69).
  • domain assumption Vanishing of the wave function at v=0 (DeWitt's criterion) implies singularity resolution.
    Sec. III D.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Unitary quantum matter-bounce in a universe with a positive cosmological constant." pith.science (2026). https://pith.science/paper/FGDZOZGR

@misc{pith2026250516863,
  author       = {Pith},
  title        = {Pith review of: Unitary quantum matter-bounce in a universe with a positive cosmological constant},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/FGDZOZGR}},
  note         = {Machine review of arXiv:2505.16863}
}
abstract

We analyze the Wheeler-DeWitt quantization of a spatially flat Friedmann-Lema\^itre-Robertson-Walker universe containing pressureless dust and a positive cosmological constant ($\Lambda > 0$). Following relational time framework, we establish a direct mathematical correspondence between the cosmological Hamiltonian and the radial Schr\"odinger equation for the scattering states of the non-relativistic hydrogen atom. This exact solvability allows us to rigorously construct the physical Hilbert space and ensure the self-adjointness of the Hamiltonian. As a concrete result, we show that the wave packets unitarily evolve depicting a non-singular quantum bounce, systematically replacing the classical Big Bang singularity. Finally, we discuss the physical relevance of this exact solution within the matter-bounce scenario. We demonstrate that this framework provides a robust quantum origin for a bounce during a dust-dominated contracting phase -- a necessary prerequisite for generating a scale-invariant spectrum of primordial perturbations -- derived from the unitary dynamics of the quantized background.

Figures

Figures reproduced from arXiv: 2505.16863 by the authors.

Figure 1
Figure 1. FIG. 1. Classical trajectories and Hubble parameters for two [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. Heatmaps for the probability density functions on ( [PITH_FULL_IMAGE:figures/full_fig_p011_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. Relative deviation of expectation values of [PITH_FULL_IMAGE:figures/full_fig_p012_3.png] view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: FIG. 4. Quantum fluctuations in [PITH_FULL_IMAGE:figures/full_fig_p013_4.png]
Figure 5
Figure 5. Figure 5: FIG. 5. Hubble parameters for different [PITH_FULL_IMAGE:figures/full_fig_p014_5.png]

Discussion (0). Sign in to comment.

Forward citations

Cited by 1 Pith paper

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Unimodular quantum cosmology in the connection representation: A minimal model

    gr-qc 2026-02 conditional novelty 5.0 of 10

    In a flat, empty unimodular quantum cosmology in connection variables, positive-cosmological-constant wave functions vanish at zero volume, while a negative cosmological constant is excluded by operator regularity and...

Reference graph

Works this paper leans on

83 extracted references · 66 canonical work pages · cited by 1 Pith paper

  1. [58]

    A Unimodular Theory of Canonical Quantum Gravity,

    W. G. Unruh, “A Unimodular Theory of Canonical Quantum Gravity,” Phys. Rev. D40 (1989) 1048

  2. [1]

    In this gauge, the dust degree of freedom ( T) is the natural choice for reference clock

    Comoving “dust” gauge As the name suggests, the observer is comoving with the Brown-Kuchaˇ r dust. In this gauge, the dust degree of freedom ( T) is the natural choice for reference clock. From Eq. (17) for the dust sector, we get: T′ = 1 = ⇒ T = τ + constant. (23) Thus, the Hubble parameter is: H ≡ a′ a = v′ 3v , (24) and the energy density as a function...

  3. [2]

    effective charge

    Unimodular gauge In this gauge, the momentum conjugate to the cosmo- logical constant, T, provides the reference clock. Impos- ing the choice of the lapse function N = v−1 in Eq. (15) FIG. 1. Classical trajectories and Hubble parameters for two lapse choices with ρ0 = 100 and Λ = 3. leads to: ˙T = 1 = ⇒ T = t + constant. (31) The solution for the dust con...

  4. [3]

    Positive Cosmological Constant (Λ > 0): This sector is analogous to the continuous spectrum (scattering states) of the hydrogen atom whereE >

  5. [4]

    The solutions ψ1 Λ,ρ0 (v) and ψ2 Λ,ρ0 (v) Eq

    The parameter k = 2 p Λ/3 is real and acts like a wave number. The solutions ψ1 Λ,ρ0 (v) and ψ2 Λ,ρ0 (v) Eq. (42), involving confluent hypergeometric func- tions F and U with complex arguments1, are anal- ogous to Coulomb wave functions. These represent oscillatory (non-normalizable) states

  6. [5]

    For physically well-behaved solutions (analogous to normalizable bound states), the cosmological con- stant Λ becomes quantized

    Negative Cosmological Constant (Λ < 0): This sector shows a direct equivalence with the bound states of the hydrogen atom ( E < 0). For physically well-behaved solutions (analogous to normalizable bound states), the cosmological con- stant Λ becomes quantized. The quantization con- dition is derived by requiring the solutions to be fi- nite for large v (a...

  7. [6]

    (40): First, when the cosmological constant is taken to zero (Λ = 0), the system describes a quantized dust-dominated universe [22]

    Single-fluid quantum cosmology: Let us con- sider two specific limiting scenarios of the Wheeler- DeWitt equation Eq. (40): First, when the cosmological constant is taken to zero (Λ = 0), the system describes a quantized dust-dominated universe [22]. The governing equa- tion in this instance, ψ′′ 0,ρ0 (v) + 4ρ0 3v ψ0,ρ0 (v) = 0, is analogous to the radial...

  8. [7]

    This complexity raises questions about the practical con- struction of a unitary quantum theory with this clock choice, though it does not definitively preclude it

    or (51) ⟨Ψρ0 (v)|Ψρ′ 0 (v)⟩ ∼δρ0,ρ′ 0 (52) for the eigenstates Ψ ρ0 (v) across the full spectrum of Λ and ρ0 can be more challenging than for the T-clock case. This complexity raises questions about the practical con- struction of a unitary quantum theory with this clock choice, though it does not definitively preclude it. Moreover, it is not clear whethe...

Show all 83 references
  1. [8]

    The eigenfunc- tions, representing scattering states, are those given in Eq

    Positive Cosmological Constant (Λ > 0): This corresponds to negative eigenvalues for the unimod- ular Hamiltonian ( Eu = −Λ < 0). The eigenfunc- tions, representing scattering states, are those given in Eq. (42), where k ≡ 2 p Λ/3 is real and positive

  2. [9]

    For these to be physically acceptable bound states, Λ must be quantized, leading to discrete positive eigenval- ues Eu

    Negative Cosmological Constant (Λ < 0): This corresponds to positive eigenvalues for the uni- modular Hamiltonian ( Eu = −Λ > 0). For these to be physically acceptable bound states, Λ must be quantized, leading to discrete positive eigenval- ues Eu. The quantization condition,...

  3. [10]

    V anishing Cosmological Constant (Λ = 0): This corresponds to a zero eigenvalue for the uni- modular Hamiltonian (Eu = 0). The eigenfunc- tions simplify to Bessel functions: ψ1 0,ρ0 (v) = √vJ1 4√ 3 √ρ0v ψ2 0,ρ0 (v) = √vY1 4√ 3 √ρ0v , (57) These solutions match the stationary s...

  4. [11]

    This means the quantum theory allows only discrete val- ues for a negative cosmological constant, dependent on 10 the dust energy density parameter ρ0

    This corresponds to cases where the cosmological constant Λ n = −Eu,n < 0 is quantized as Λ n = − ρ2 0 3n2 , leading to Eu,n = ρ2 0 3n2 for n ∈ Z+. This means the quantum theory allows only discrete val- ues for a negative cosmological constant, dependent on 10 the dust energy...

  5. [12]

    (61) ψ1 k(v) = Ckv e−ikvF 1 + i 2ρ0 3k , 2, 2ikv (A1) δ-function normalized: Z ∞ 0 dv ψ1 k(v)ψ1 k′(v) = δ(k − k′)

    Stationary states with positive eigenvalues In this subsection, the aim is to make the positive cos- mological constant stationary state Eq. (61) ψ1 k(v) = Ckv e−ikvF 1 + i 2ρ0 3k , 2, 2ikv (A1) δ-function normalized: Z ∞ 0 dv ψ1 k(v)ψ1 k′(v) = δ(k − k′). (A2) In order to obta...

  6. [13]

    (62) ψ1 n(v) = Cnv e−2ρ0v/3nL1 n−1 4ρ0v 3n (A18) For orthogonality, we need to show Z ∞ 0 dv ψ1∗ m (v)ψ1 n(v) = 0

    Stationary states with negative eigenvalues In this subsection, we find the normalization of sta- tionary states with negative eigenvalues in Eq. (62) ψ1 n(v) = Cnv e−2ρ0v/3nL1 n−1 4ρ0v 3n (A18) For orthogonality, we need to show Z ∞ 0 dv ψ1∗ m (v)ψ1 n(v) = 0. if n ̸= m. (A19)...

  7. [14]

    Gravitational collapse and space-time singularities,

    R. Penrose, “Gravitational collapse and space-time singularities,” Physical Review Letters14 no. 3, (Jan.,

  8. [15]

    Singularity resolution depends on the clock,

    S. Gielen and L. Men´ endez-Pidal, “Singularity resolution depends on the clock,” Class. Quant. Grav. 37 no. 20, (2020) 205018, arXiv:2005.05357 [gr-qc]

  9. [16]

    Black holes in general relativity,

    S. W. Hawking, “Black holes in general relativity,” Commun. Math. Phys.25 (1972) 152–166

  10. [17]

    Quantum conformal fluctuations in a signular space-time,

    T. Padmanabhan and J. V. Narlikar, “Quantum conformal fluctuations in a signular space-time,” Nature 295 (1982) 677–678

  11. [18]

    J. V. Narlikar and T. Padmanabhan, Gravity, Gauge Theories and Quantum Cosmology. Reidel, Dordrecht, 1986

  12. [19]

    Kiefer, Quantum Gravity

    C. Kiefer, Quantum Gravity. International Series of Monographs on Physics. Oxford University Press, London, England, 3 ed., Apr., 2012

  13. [20]

    Classical and quantum Lema ˆ ıtre-Tolman-Bondi model for the nonmarginal case,

    C. Kiefer, J. M¨ uller-Hill, and C. Vaz, “Classical and quantum Lema ˆ ıtre-Tolman-Bondi model for the nonmarginal case,” Physical Review D73 no. 4, (Feb.,

  14. [21]

    Quantization of Midisuperspace Models,

    J. F. Barbero G. and E. J. S. Villasenor, “Quantization of Midisuperspace Models,” Living Rev. Rel.13 (2010) 6, arXiv:1010.1637 [gr-qc]

  15. [22]

    Singularity avoidance in quantum-inspired inhomogeneous dust collapse,

    Y. Liu, D. Malafarina, L. Modesto, and C. Bambi, “Singularity avoidance in quantum-inspired inhomogeneous dust collapse,” Physical Review D90 no. 4, (Aug., 2014) 044040

  16. [23]

    Singularity avoidance and time in quantum gravity,

    A. Kreienbuehl, “Singularity avoidance and time in quantum gravity,” Physical Review D79 no. 12, (June,

  17. [24]

    Unitary evolution of the quantum universe with a Brown-Kuchar dust,

    H. Maeda, “Unitary evolution of the quantum universe with a Brown-Kuchar dust,” Classical and Quantum Gravity 32 no. 23, (Dec., 2015) 235023

  18. [25]

    Singularity avoidance in a quantum model of the Mixmaster universe,

    H. Bergeron, E. Czuchry, J.-P. Gazeau, P. Ma lkiewicz, and W. Piechocki, “Singularity avoidance in a quantum model of the Mixmaster universe,” Physical Review D 92 no. 12, (Dec., 2015) 124018

  19. [26]

    Singularity avoidance for collapsing quantum dust in the Lema ˆ ıtre-Tolman-Bondi model,

    C. Kiefer and T. Schmitz, “Singularity avoidance for collapsing quantum dust in the Lema ˆ ıtre-Tolman-Bondi model,” Physical Review D99 no. 12, (June, 2019) 126010. https: //link.aps.org/doi/10.1103/PhysRevD.99.126010

  20. [27]

    Singularity avoidance in Bianchi I quantum cosmology,

    C. Kiefer, N. Kwidzinski, and D. Piontek, “Singularity avoidance in Bianchi I quantum cosmology,” The European Physical Journal C79 no. 8, (Aug., 2019)

  21. [28]

    Quantum Theory of Gravity. I. The Canonical Theory,

    B. S. DeWitt, “Quantum Theory of Gravity. I. The Canonical Theory,” Physical Review160 no. 5, (Aug.,

  22. [29]

    Quantum empty Bianchi I spacetime with internal time,

    P. Ma lkiewicz, P. Peter, and S. D. P. Vitenti, “Quantum empty Bianchi I spacetime with internal time,” Phys. Rev. D101 no. 4, (2020) 046012, arXiv:1911.09892 [gr-qc]

  23. [30]

    Canonical quantum gravity and the problem of time,

    C. J. Isham, “Canonical quantum gravity and the problem of time,” NATO Sci. Ser. C409 (1993) 157–287, arXiv:gr-qc/9210011

  24. [31]

    Unitarity, clock dependence and quantum recollapse in quantum cosmology,

    S. Gielen and L. Men´ endez-Pidal, “Unitarity, clock dependence and quantum recollapse in quantum cosmology,” Class. Quant. Grav.39 no. 7, (2022) 075011, arXiv:2109.02660 [gr-qc]

  25. [32]

    Unitarity and quantum resolution of gravitational singularities,

    S. Gielen and L. Men´ endez-Pidal, “Unitarity and quantum resolution of gravitational singularities,” Int. J. Mod. Phys. D31 no. 14, (2022) 2241005, arXiv:2205.15387 [gr-qc]

  26. [33]

    Quantum analysis of the recent cosmological bounce in the comoving Hubble length,

    S. Gielen and J. Magueijo, “Quantum analysis of the recent cosmological bounce in the comoving Hubble length,” Phys. Rev. D107 no. 2, (2023) 023518, arXiv:2201.03596 [gr-qc]

  27. [34]

    Possible quantum effects at the transition from cosmological deceleration to acceleration,

    B. Alexandre and J. Magueijo, “Possible quantum effects at the transition from cosmological deceleration to acceleration,” Phys. Rev. D106 no. 6, (2022) 063520, arXiv:2207.03854 [gr-qc]

  28. [35]

    Unimodular Hartle-Hawking wave packets and their probability interpretation,

    B. Alexandre and J. Magueijo, “Unimodular Hartle-Hawking wave packets and their probability interpretation,” Phys. Rev. D107 no. 6, (2023) 063501, arXiv:2210.02179

  29. [36]

    Big bang singularity resolution in quantum cosmology,

    K. P. Y. Thebault, “Big bang singularity resolution in quantum cosmology,” Class. Quant. Grav.40 no. 5, (2023) 055007, arXiv:2209.05905 [gr-qc]

  30. [37]

    Analyzing quantum gravity spillover in the semiclassical regime,

    H. S. Sahota and K. Lochan, “Analyzing quantum gravity spillover in the semiclassical regime,” The European Physical Journal C83 no. 12, (Dec, 2023) 1162, arXiv:2211.16426 [gr-qc]. https://doi.org/10.1140/epjc/s10052-023-12311-2

  31. [38]

    Imprints of the operator ordering ambiguity on the dynamics of perfect fluid dominated quantum Universe,

    H. S. Sahota, “Imprints of the operator ordering ambiguity on the dynamics of perfect fluid dominated quantum Universe,” Class. Quant. Grav.41 no. 17, (2024) 175006, arXiv:2310.09905 [gr-qc]

  32. [39]

    Black hole singularity resolution in unimodular gravity from unitarity,

    S. Gielen and L. Men´ endez-Pidal, “Black hole singularity resolution in unimodular gravity from unitarity,” Phys. Rev. Lett.134 (Mar, 2025) 101501. https://link.aps.org/doi/10.1103/PhysRevLett. 134.101501

  33. [40]

    The Theory of gravitation in Hamiltonian form,

    P. A. M. Dirac, “The Theory of gravitation in Hamiltonian form,” Proc. Roy. Soc. Lond. A246 (1958) 333–343

  34. [41]

    The coordinate group symmetries of general relativity,

    P. G. Bergmann and A. Komar, “The coordinate group symmetries of general relativity,” Int. J. Theor. Phys.5 (1972) 15–28

  35. [42]

    Superspace and the nature of quantum geometrodynamics.,

    J. A. Wheeler, “Superspace and the nature of quantum geometrodynamics.,” in In Cecile M.DeWitt and John A. Wheeler, editors,Battelle Rencontres, 1967 Lectures in Mathematicsand Physics, pages 242–307. W.A. Benjamin, New York, 1968

  36. [43]

    The Cosmological Constant and General Covariance,

    M. Henneaux and C. Teitelboim, “The Cosmological Constant and General Covariance,” Phys. Lett. B222 (1989) 195–199

  37. [44]

    Does an unspecified cosmological constant solve the problem of time in quantum gravity?,

    K. V. Kuchaˇ r, “Does an unspecified cosmological constant solve the problem of time in quantum gravity?,” Phys. Rev. D43 (1991) 3332–3344

  38. [45]

    Quantum cosmology via parth integrals,

    J. V. Narlikar and T. Padmanabhan, “Quantum cosmology via parth integrals,” Phys. Rept. 100 (1983) 151–200

  39. [46]

    Quantum cosmology meets atomic physics: A hydrogen atom analogy for the wheeler-dewitt equation with dust and Λ,

    D. Mukherjee, H. S. Sahota, and S. Shankaranarayanan, “Quantum cosmology meets atomic physics: A hydrogen atom analogy for the wheeler-dewitt equation with dust and Λ,” 2025

  40. [47]

    Time and interpretations of quantum gravity,

    K. V. Kuchaˇ r, “Time and interpretations of quantum gravity,” International Journal of Modern Physics D20 no. supp01, (2011) 3–86, https://doi.org/10.1142/S0218271811019347

  41. [48]

    Problem of time in quantum gravity,

    E. Anderson, “Problem of time in quantum gravity,” Annalen der Physik524 no. 12, (2012) 757–786

  42. [49]

    Relational Observables in Gravity: a Review,

    J. Tambornino, “Relational Observables in Gravity: a Review,” SIGMA 8 (2012) 017, arXiv:1109.0740 [gr-qc]

  43. [50]

    Trinity of relational quantum dynamics,

    P. A. Hoehn, A. R. H. Smith, and M. P. E. Lock, “Trinity of relational quantum dynamics,” Phys. Rev. D 104 no. 6, (2021) 066001, arXiv:1912.00033 [quant-ph]

  44. [51]

    Chataignier, Timeless Quantum Mechanics and the Early Universe

    L. Chataignier, Timeless Quantum Mechanics and the Early Universe. Springer Theses. Springer, Berlin, Germany, 2022

  45. [52]

    On the generality of refined algebraic quantization,

    D. Giulini and D. Marolf, “On the generality of refined algebraic quantization,” Classical and Quantum Gravity 16 no. 7, (Jan., 1999) 2479–2488. http://dx.doi.org/10.1088/0264-9381/16/7/321

  46. [53]

    Construction of quantum Dirac observables and the emergence of WKB time,

    L. Chataignier, “Construction of quantum Dirac observables and the emergence of WKB time,” Phys. 18 Rev. D101 no. 8, (2020) 086001, arXiv:1910.02998 [gr-qc]

  47. [54]

    Selection rules for the Wheeler-DeWitt equation in quantum cosmology,

    A. O. Barvinsky and A. Y. Kamenshchik, “Selection rules for the Wheeler-DeWitt equation in quantum cosmology,” Phys. Rev. D89 no. 4, (2014) 043526, arXiv:1312.3147

  48. [55]

    How to switch between relational quantum clocks,

    P. A. H¨ ohn and A. Vanrietvelde, “How to switch between relational quantum clocks,” New J. Phys.22 no. 12, (2020) 123048, arXiv:1810.04153 [gr-qc]

  49. [56]

    Quantum cosmological singularities,

    M. J. Gotay and J. Demaret, “Quantum cosmological singularities,” Phys. Rev. D28 (Nov, 1983) 2402–2413. https: //link.aps.org/doi/10.1103/PhysRevD.28.2402

  50. [57]

    Dust as a Standard of Space and Time in Canonical Quantum Gravity,

    J. D. Brown and K. V. Kuchaˇ r, “Dust as a Standard of Space and Time in Canonical Quantum Gravity,” Physical Review D51 no. 10, (May, 1995) 5600–5629. http://arxiv.org/abs/gr-qc/9409001

  51. [59]

    L. D. Landau and E. M. Lifshitz, Quantum mechanics. Butterworth-Heinemann, Oxford, England, 3 ed., Dec., 1981

  52. [60]

    Semiclassical states for constrained systems,

    A. Ashtekar, L. Bombelli, and A. Corichi, “Semiclassical states for constrained systems,” Phys. Rev. D72 (2005) 025008, arXiv:gr-qc/0504052

  53. [61]

    The Quantization of unimodular gravity and the cosmological constant problems,

    L. Smolin, “The Quantization of unimodular gravity and the cosmological constant problems,” Phys. Rev. D 80 (2009) 084003, arXiv:0904.4841 [hep-th]

  54. [62]

    Quantum wave packet revivals,

    R. Robinett, “Quantum wave packet revivals,” Physics Reports 392 no. 1, (2004) 1–119

  55. [63]

    The Case for a positive cosmological Lambda term,

    V. Sahni and A. A. Starobinsky, “The Case for a positive cosmological Lambda term,” Int. J. Mod. Phys. D 9 (2000) 373–444, arXiv:astro-ph/9904398

  56. [64]

    G. B. Arfken, H. J. Weber, and F. E. Harris, Mathematical methods for physicists. Academic Press, San Diego, CA, 6 ed., July, 2005

  57. [65]

    Abramowitz and I

    M. Abramowitz and I. A. Stegun, eds., Handbook of mathematical functions. Dover Books on Mathematics. Dover Publications, Mineola, NY, June, 1965

  58. [66]

    Zettili, Quantum Mechanics: Concepts and Applications

    N. Zettili, Quantum Mechanics: Concepts and Applications. Wiley-Blackwell, Hoboken, NJ, 2 ed., Jan., 2009

  59. [67]

    Gitman, I

    D. Gitman, I. Tyutin, and B. Voronov, Self-adjoint extensions in quantum mechanics. Progress in Mathematical Physics. Birkhauser Boston, Secaucus, NJ, 2012 ed., Apr., 2012

  60. [68]

    Unitarity approach to quantum cosmology,

    A. Barvinsky, “Unitarity approach to quantum cosmology,” Physics Reports230 no. 5, (1993) 237–367. https://www.sciencedirect.com/science/article/ pii/0370157393900329

  61. [69]

    BRST technique for the cosmological density matrix,

    A. O. Barvinsky, “BRST technique for the cosmological density matrix,” JHEP 10 (2013) 051, arXiv:1308.3270 [hep-th]

  62. [70]

    Self-adjointness in the Hamiltonians of deparameterized totally constrained theories: a model,

    R. Gambini and J. Pullin, “Self-adjointness in the Hamiltonians of deparameterized totally constrained theories: a model,” Phys. Rev. D86 (2012) 067501, arXiv:1207.5730 [gr-qc]

  63. [71]

    An effective approach to the problem of time,

    M. Bojowald, P. A. H¨ ohn, and A. Tsobanjan, “An effective approach to the problem of time,” Classical and Quantum Gravity28 no. 3, (Jan., 2011) 035006

  64. [72]

    Effective approach to the problem of time: general features and examples,

    M. Bojowald, P. A. Hohn, and A. Tsobanjan, “Effective approach to the problem of time: general features and examples,” Phys. Rev. D83 (2011) 125023, arXiv:1011.3040 [gr-qc]

  65. [73]

    Self-adjoint extensions of operators and the teaching of quantum mechanics,

    G. Bonneau, J. Faraut, and G. Valent, “Self-adjoint extensions of operators and the teaching of quantum mechanics,” American Journal of Physics69 no. 3, (Mar, 2001) 322–331

  66. [74]

    Self-adjoint extensions and spectral analysis in the generalized kratzer problem,

    M. C. Baldiotti, D. M. Gitman, I. V. Tyutin, and B. L. Voronov, “Self-adjoint extensions and spectral analysis in the generalized kratzer problem,” Physica Scripta 83 no. 6, (May, 2011) 065007. http: //dx.doi.org/10.1088/0031-8949/83/06/065007

  67. [77]

    Wave packets bouncing off walls,

    M. Andrews, “Wave packets bouncing off walls,” American Journal of Physics66 no. 3, (03, 1998) 252–254

  68. [79]

    Representations of Space-time Diffeomorphisms. 2. Canonical Geometrodynamics,

    C. J. Isham and K. V. Kuchar, “Representations of Space-time Diffeomorphisms. 2. Canonical Geometrodynamics,” Annals Phys. 164 (1985) 316

  69. [80]

    Gaussian reference fluid and interpretation of quantum geometrodynamics,

    K. V. Kuchaˇ r and C. G. Torre, “Gaussian reference fluid and interpretation of quantum geometrodynamics,” Phys. Rev. D43 (1991) 419–441

  70. [81]

    The Harmonic gauge in canonical gravity,

    K. V. Kuchaˇ r and C. G. Torre, “The Harmonic gauge in canonical gravity,” Phys. Rev. D44 (1991) 3116–3123

  71. [82]

    Extrinsic curvature as a reference fluid in canonical gravity,

    K. V. Kuchaˇ r, “Extrinsic curvature as a reference fluid in canonical gravity,” Phys. Rev. D45 (1992) 4443–4457

  72. [83]

    Gradshteyn and I

    I. Gradshteyn and I. Ryzhik, Table of Integrals, Series, and Products. Academic Press, 1980. https://www.sciencedirect.com/science/article/ pii/B9780122947605500192

  73. [686]

    http://arxiv.org/abs/1903.04391

  74. [1965]

    https://doi.org/10.1103/physrevlett.14.57

    57–59. https://doi.org/10.1103/physrevlett.14.57. 17

  75. [1967]

    https: //link.aps.org/doi/10.1103/PhysRev.160.1113

    1113–1148. https: //link.aps.org/doi/10.1103/PhysRev.160.1113

Pith tools

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