REVIEW 3 major objections 4 minor 1 cited by
For sharply peaked initial states, the Krylov complexity of the quantum universe grows as (σ/2)²(φ−φ0)² for states and double that for operators—so it diverges at the WDW singularity but stays finite through the loop-quantum bounce.
Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →
T0 review · deepseek-v4-flash
2026-08-03 20:55 UTC pith:MKFG7JNC
load-bearing objection Genuine first: Krylov complexity for a constrained quantum cosmological system with a relational clock, cleanly derived at leading order; the uncontrolled sharp-peaking approximation is the main soft spot but not disqualifying. the 3 major comments →
Quantum Cosmology in Krylov Space: Complexity and Entropy
The pith
A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.
Core claim
The central claim is that, for sharply peaked states (k0 >> σ), the Krylov state complexity of the universe in both WDW quantum cosmology and sLQC is C_K^(ψ) = (σ²/4)(φ−φ0)² and the Krylov operator complexity, computed for the pure-state density operator, is C_K^(O) = (σ²/2)(φ−φ0)², so C_K^(O) = 2 C_K^(ψ). The Lanczos coefficients are b_n = (√n/2)σ for states and b_n = √(n/2)σ for operators, giving Poisson probability distributions with means σ²(φ−φ0)²/4 and σ²(φ−φ0)²/2 respectively. Because the same Hamiltonian and inner product appear in both frameworks, the formulas are identical; the two theories differ only in which values of φ correspond to physical events. Consequently, Krylov complex
What carries the argument
The Lanczos algorithm applied to the physical Hamiltonian H = −√Θ, which in momentum space multiplies by −k. The key approximations are replacing the physical half-line inner product 2∫_0^∞ dk k χ̃₁*χ̃₂ by the full-line version 2∫_{-∞}^∞ dk k χ̃₁*χ̃₂ and extending the initial Gaussian to all k; this yields the exact Hermite-polynomial Krylov basis |K_n⟩ = (1/√(2^n n!)) H_n(−√2(k−k0)/σ) χ̃(k), with Lanczos coefficients a_n ≈ −k0 and b_n = (√n/2)σ for states. For operators, the Liouvillian L = [−√Θ, ·] gives b_n = √(n/2)σ. These b_n are the machine that produces the Poisson distributions and hence the quadratic growth and the factor-2 operator-to-state ratio.
Load-bearing premise
Everything hinges on the sharp-peaking approximation that replaces the physical half-line momentum inner product with a full-line inner product and extends the Gaussian initial state to all momenta; if it fails, the exact Hermite-polynomial basis, the Poisson distribution, the quadratic growth, and the factor-2 relation all become approximate or invalid.
What would settle it
Compute the exact Lanczos coefficients for the unapproximated physical inner product (χ1,χ2)_phys = 2∫_0^∞ dk k χ̃₁*χ̃₂ for finite k0/σ, either analytically or numerically. If b_n deviates from √n σ/2 by more than O(σ³/k0²), or if the resulting Krylov complexity is not C_K^(ψ) = σ²(φ−φ0)²/4 up to that error, the central claim is falsified.
If this is right
- In both WDW quantum cosmology and sLQC, the Krylov state and operator complexity grow as the square of the scalar-field clock, consistent with integrable (non-chaotic) dynamics.
- The exact relation C_K^(O) = 2 C_K^(ψ) holds for these infinite-dimensional systems, not just for qubits.
- Krylov entropy is minimized at the initial time φ0 and increases monotonically in each branch; in sLQC the bounce provides a canonical φ0, while in WDW the initial time is ad hoc.
- Complexity and entropy diverge at the WDW big-bang/big-crunch singularities but remain finite throughout sLQC, including at the bounce.
- The construction demonstrates a template for defining Krylov complexity in constrained systems by using a relational clock instead of external time.
Where Pith is reading between the lines
- Because the factor-2 and quadratic-growth results rest on the sharp-peaking approximation, an exact (or numerical) treatment of finite σ/k0 is likely to show the relation holds only approximately; the paper itself flags corrections of order σ³/k0².
- The use of the density operator as the probe makes the two frameworks mathematically identical; choosing a Dirac observable with different spectra, like the volume operator, would likely expose theory-specific complexity behavior.
- The monotone growth of Krylov entropy away from the bounce is suggestive of an information-theoretic arrow of time, but the paper correctly notes that no rigorous link to thermodynamic entropy has been established.
- Extending this analysis to anisotropic models is a natural test: if quantum chaos survives, Krylov complexity should switch from quadratic to exponential growth, providing a sharp signature of chaos near singularities.
Editorial analysis
A structured set of objections, weighed in public.
Referee Report
Summary. The paper studies Krylov (state and operator) complexity and Krylov entropy for a flat FLRW universe with a massless scalar field in two canonical quantum cosmology frameworks: Wheeler-DeWitt (WDW) and solvable loop quantum cosmology (sLQC). Using the physical Hilbert space and Hamiltonian of Ref. [11], the authors construct the Krylov basis analytically, starting from a Gaussian state sharply peaked in the scalar-field momentum (k0 >> sigma). They replace the physical half-line inner product with a full-line approximation and obtain Lanczos coefficients b_n ~ sqrt(n) sigma/2 for states and b_n ~ sqrt(n/2) sigma for operators. This leads to Poisson probability distributions, Krylov state complexity C_K^(psi) = sigma^2 (phi-phi0)^2 / 4, Krylov operator complexity C_K^(O) = sigma^2 (phi-phi0)^2 / 2, and hence C_K^(O) = 2 C_K^(psi). The paper interprets these results globally: in WDW the complexity and entropy diverge at the big bang/big crunch (phi -> +- infinity), whereas in sLQC they remain finite at the finite-time bounce.
Significance. If the central results hold, this is the first construction of Krylov complexity for a totally constrained quantum cosmological system with an internal clock, and the first direct bridge between Krylov complexity and canonical quantum gravity/LQC. The paper is explicit and analytic, uses the independently established physical Hilbert space of Ref. [11], introduces no fitted parameters, and gives falsifiable predictions (quadratic growth, factor-2 relation, finite-at-bounce behavior). These are genuine strengths. However, the entire quantitative structure rests on the sharp-peaking approximation introduced in Sec. IV.A, and the manuscript does not provide a controlled error analysis for the Lanczos coefficients or the resulting probabilities. Since the main physical conclusions (divergence vs. finiteness) are global in the internal time phi, the absence of such control is load-bearing.
major comments (3)
- [Sec. IV.A, Eqs. (4.3)-(4.17)] The Hermite basis (4.13) is not orthonormal with respect to the approximate inner product (4.3), because the factor k in the measure breaks the Gaussian-Hermite orthogonality. For the normalized Gaussian (4.4), a direct evaluation gives <K0|K1> = O(sigma^2/k0), not zero. The Lanczos algorithm with the exact a0 = -k0(1 + sigma^2/(4 k0^2)) would shift A1 in Eq. (4.7) by an O(sigma^2/k0) term. Thus the claims b_n = sqrt(n) sigma/2, the Poisson distribution (4.16), and the complexity (4.17) are leading-order statements; they are not exact consequences of the stated inner product. Moreover, retaining the k variation in the integral (4.14) gives corrections to the Krylov coefficients that are not uniformly small in phi - phi0; for late times the correction can become O(1). The citation to Ref. [64] concerns semiclassical expectation values, not orthonormality of a Krylov basis. The authors sho
- [Sec. IV.A and IV.B, Eq. (4.28) and the induction for b_n] The paper asserts, after constructing K0, K1, K2, K3, that 'continuing this iteration' yields a_n ~ -k0 and b_n ~ sqrt(n) sigma/2. No induction proof is given for either the state or the operator Lanczos coefficients. The quoted error term O(sigma^3 k0^-2) in Eq. (4.28) is not derived from a recurrence and is stated only for fixed n. The subsequent Poisson statistics and the exact factor-2 relation depend on all n, and the divergence at phi -> +- infinity probes arbitrarily large n. A general argument (or an explicit recurrence bound) is needed to justify that the approximation remains valid for the entire support of the probability distribution and for all relevant phi.
- [Sec. IV.A, Eqs. (4.2)-(4.4)] The replacement of the physical inner product 2 int_0^infinity dk k ... by 2 int_-infinity^infinity dk k ... is not a positive-definite inner product on L^2(R). For states with support at negative k the measure is negative. While this is harmless for the very-low-n overlap of a Gaussian peaked at k0 >> sigma, the Hermite polynomials in (4.13) grow at negative k as n grows; for n of order (k0/sigma)^2 the negative-k tail may no longer be negligible. Since the claimed divergence of Krylov complexity and entropy in WDW occurs at late internal times, where the relevant Krylov index grows without bound, the global interpretation is not established by the leading-order calculation. A numerical or analytic computation of the actual Lanczos coefficients for the half-line measure would settle whether the qualitative conclusions survive.
minor comments (4)
- [Sec. IV.A, Eq. (4.4)] The notation '.=' is used for an approximate equality but is never defined. Please define this notation explicitly (e.g., 'equality up to the sharp-peaking approximation').
- [Sec. IV.B, Eq. (4.31)] The solution is written with 'for some constant m' and then m is set to phi0 by the initial condition. This is fine mathematically, but the symbol m is unnecessary and can be eliminated for clarity.
- [Sec. IV.B, Eq. (4.24)] There appear to be typographical issues with subscripts/superscripts in the trace expression (e.g., 'brho2_0' and 'brho_2_0'). Please proofread the equation and define all terms.
- [Sec. IV.A, reference [64]] The statement that extending the Gaussian to all k introduces only 'negligible error' is cited to Ref. [64]. That reference studies coherent states and expectation values of Dirac observables; it does not address the orthonormality of the Krylov basis or the Lanczos coefficients. This justification should be supplemented with a direct estimate in the context of the present calculation.
Circularity Check
No significant circularity: the Krylov complexity results are derived from the independently established WDW/sLQC framework and the stated sharp-peaking approximation, not assumed as inputs.
full rationale
The derivation chain is not circular. The physical Hamiltonian, inner product, and singularity/bounce structure are imported from Ref. [11], which shares a co-author but is an independently established and widely used framework; the paper's new content is the Lanczos construction and the resulting Krylov coefficients, probabilities, and complexities. The initial Gaussian and parameters k0 and sigma are chosen initial-state data, not fitted to produce the claimed quadratic growth. The replacement of the half-line inner product (4.2) by the full-line approximation (4.3) is an explicit approximation: it makes the Hermite-basis results leading-order in sigma/k0, and the paper consistently states that all results hold only for k0 >> sigma, with Eq. (4.28) carrying O(sigma^3 k0^-2) corrections. This is an accuracy/justification limitation, not a circular reduction, because the complexity is computed honestly within the approximate model rather than imposed by construction. The relation C_K^(O) = 2 C_K^(psi) follows algebraically from the Lanczos coefficients b_n^(state) = sqrt(n) sigma/2 and b_n^(op) = sqrt(n/2) sigma, and the divergence/finiteness at singularities versus the bounce is read off from the known dependence of the physical volume on the internal clock. No fitted parameter is renamed as a prediction, and no load-bearing step reduces to a self-citation. The work is self-contained against the Krylov-complexity formalism and the standard WDW/sLQC quantization.
Axiom & Free-Parameter Ledger
free parameters (3)
- sigma (Gaussian width)
- k0 (mean momentum)
- phi0 (initial internal time)
axioms (5)
- domain assumption The physical Hilbert space, physical inner product, and physical Hamiltonian for the flat FLRW massless-scalar universe in WDW and sLQC are those constructed in Ref. [11]; in the k-representation both reduce to a free-particle Hamiltonian H_phys = -√Θ ≈ -|k| on positive-frequency solutions.
- domain assumption The massless scalar field φ is a global monotonic internal clock for the entire non-singular history in sLQC and for each branch (expanding/contracting) in WDW.
- ad hoc to paper The physical inner product can be approximated by the full-line inner product (Eq. 4.3) and the initial state can be taken as a Gaussian on all of k (Eq. 4.4) with k0 >> σ.
- standard math The Lanczos algorithm for the Gaussian state yields b_n = √n σ/2 for states and b_n = √(n/2) σ for operators for all n (Eqs. 4.13, 4.28).
- standard math The Hilbert-Schmidt inner product is well-defined and normalizable for the pure-state density matrix and all Liouvillian iterates used in the operator Lanczos algorithm.
read the original abstract
We study the quantum dynamics in Krylov space of a spatially flat, homogeneous, and isotropic universe sourced with a massless scalar field within Wheeler-DeWitt (WDW) quantum cosmology and loop quantum cosmology (LQC) frameworks. The availability of a physical Hilbert space and physical Hamiltonian and the presence of an internal clock enable us to construct the Krylov basis analytically by applying the Lanczos algorithm. We then evaluate both the Krylov state and operator complexity for WDW quantum cosmology and LQC on this basis. In regimes where the wave function of the universe is sharply peaked, our results indicate that the Krylov complexity grows quadratically with the scalar field clock for the state and operator complexities in both the WDW quantum cosmology and LQC. We further show that the operator complexity is exactly twice the state complexity in these regimes. We discuss the interpretation of the global behavior of these systems by calculating the Krylov entropy for both quantum cosmological frameworks. We observe that in LQC, the Krylov complexity and entropy remain finite at the bounce, whereas in the WDW quantum cosmology, they diverge at the big bang/crunch singularity. Our work provides the first example of computing Krylov complexity for a system with a totally constrained Hamiltonian and no external time, a framework to calculate a purely quantum-mechanical entropy in quantum cosmology, and, to our knowledge, the first direct bridge between Krylov complexity and canonical quantum cosmology, as a first step toward understanding how polymerized quantum geometry modifies complexity and entropy.
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Forward citations
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Reference graph
Works this paper leans on
-
[1]
R. P. Geroch, What is a singularity in general relativity?, Annals Phys.48, 526 (1968)
1968
-
[2]
As before, this is achieved by using the definitionb 2 =||A 2|| and the Hilbert-Schmidt operator norm
Then, we find the second normalized Krylov operator basis element, which reads |ρ1) = √ 2 σ bρ0 q bΘ − q bΘ bρ0 .(4.22) Next, forn= 2, i.e., the third unnormalized Krylov operator basis element, we have |A2) =L|ρ 1)−b 1|ρ0) = √ 2 σ " bρ0 q bΘ 2 −2 q bΘ bρ0 q bΘ + q bΘ 2 bρ0 # − σ√ 2 bρ0.(4.23) To normalize, we need to computeb 2. As before, this is achiev...
-
[3]
S. W. Hawking and R. Penrose, The Singularities of gravitational collapse and cosmology, Proc. Roy. Soc. Lond. A314, 529 (1970)
1970
-
[4]
C. W. Misner, Mixmaster universe, Phys. Rev. Lett.22, 1071 (1969)
1969
-
[5]
V. A. Belinsky, I. M. Khalatnikov, and E. M. Lifshitz, Oscillatory approach to a singular point in the relativistic cosmology, Adv. Phys.19, 525 (1970)
1970
-
[6]
D. E. Parker, X. Cao, A. Avdoshkin, T. Scaffidi, and E. Altman, A Universal Operator Growth Hypothesis, Phys. Rev. X9, 041017 (2019), arXiv:1812.08657
Pith/arXiv arXiv 2019
-
[7]
V. Balasubramanian, P. Caputa, J. M. Magan, and Q. Wu, Quantum chaos and the complexity of spread of states, Phys. Rev. D106, 046007 (2022), arXiv:2202.06957
Pith/arXiv arXiv 2022
-
[8]
A. Ashtekar and P. Singh, Loop Quantum Cosmology: A Status Report, Class. Quant. Grav.28, 213001 (2011), arXiv:1108.0893
Pith/arXiv arXiv 2011
-
[9]
A. Ashtekar, T. Pawlowski, and P. Singh, Quantum nature of the big bang, Phys. Rev. Lett.96, 141301 (2006), arXiv:gr-qc/0602086
Pith/arXiv arXiv 2006
-
[10]
A. Ashtekar, T. Pawlowski, and P. Singh, Quantum Nature of the Big Bang: An Analytical and Numerical Investigation. I., Phys. Rev. D73, 124038 (2006), arXiv:gr-qc/0604013
Pith/arXiv arXiv 2006
-
[11]
A. Ashtekar, T. Pawlowski, and P. Singh, Quantum Nature of the Big Bang: Improved dynamics, Phys. Rev. D74, 084003 (2006), arXiv:gr-qc/0607039
Pith/arXiv arXiv 2006
-
[12]
A. Ashtekar, A. Corichi, and P. Singh, Robustness of key features of loop quantum cosmology, Phys. Rev. D77, 024046 (2008), arXiv:0710.3565
Pith/arXiv arXiv 2008
-
[13]
A. Ashtekar, T. Pawlowski, P. Singh, and K. Vandersloot, Loop quantum cosmology of k=1 FR W models, Phys. Rev. D75, 024035 (2007), arXiv:gr-qc/0612104
Pith/arXiv arXiv 2007
-
[14]
Vandersloot, Loop quantum cosmology and the k = - 1 R W model, Phys
K. Vandersloot, Loop quantum cosmology and the k = - 1 R W model, Phys. Rev. D75, 023523 (2007), arXiv:gr-qc/0612070
Pith/arXiv arXiv 2007
-
[15]
D. A. Craig, Dynamical eigenfunctions and critical density in loop quantum cosmology, Class. Quant. Grav.30, 035010 (2013), arXiv:1207.5601
Pith/arXiv arXiv 2013
-
[16]
P. Diener, B. Gupt, and P. Singh, Chimera: A hybrid approach to numerical loop quantum cosmology, Class. Quant. Grav.31, 025013 (2014), arXiv:1310.4795
Pith/arXiv arXiv 2014
-
[17]
P. Diener, B. Gupt, and P. Singh, Numerical simulations of a loop quantum cosmos: robustness of the quantum bounce and the validity of effective dynamics, Class. Quant. Grav.31, 105015 (2014), arXiv:1402.6613
Pith/arXiv arXiv 2014
-
[18]
P. Diener, B. Gupt, M. Megevand, and P. Singh, Numerical evolution of squeezed and non-Gaussian states in loop quantum cosmology, Class. Quant. Grav.31, 165006 (2014), arXiv:1406.1486
Pith/arXiv arXiv 2014
-
[19]
P. Diener, A. Joe, M. Megevand, and P. Singh, Numerical simulations of loop quantum Bianchi-I spacetimes, Class. Quant. Grav.34, 094004 (2017), arXiv:1701.05824
Pith/arXiv arXiv 2017
-
[20]
Singh, Glimpses of Space-Time Beyond the Singularities Using Supercomputers, Comput
P. Singh, Glimpses of Space-Time Beyond the Singularities Using Supercomputers, Comput. Sci. Eng. 20, 26 (2018), arXiv:1809.01747
Pith/arXiv arXiv 2018
-
[21]
Singh, Are loop quantum cosmos never singular?, Class
P. Singh, Are loop quantum cosmos never singular?, Class. Quant. Grav.26, 125005 (2009), arXiv:0901.2750
Pith/arXiv arXiv 2009
-
[22]
P. Singh and F. Vidotto, Exotic singularities and spatially curved Loop Quantum Cosmology, Phys. Rev. D83, 064027 (2011), arXiv:1012.1307
Pith/arXiv arXiv 2011
-
[23]
Singh, Loop quantum cosmology and the fate of cosmological singularities, Bull
P. Singh, Loop quantum cosmology and the fate of cosmological singularities, Bull. Astron. Soc. India 42, 121 (2014), arXiv:1509.09182
Pith/arXiv arXiv 2014
-
[24]
P. Singh, Curvature invariants, geodesics and the strength of singularities in Bianchi-I loop quantum cosmology, Phys. Rev. D85, 104011 (2012), arXiv:1112.6391. 25
Pith/arXiv arXiv 2012
-
[25]
S. Saini and P. Singh, Resolution of strong singularities and geodesic completeness in loop quantum Bianchi-II spacetimes, Class. Quant. Grav.34, 235006 (2017), arXiv:1707.08556
Pith/arXiv arXiv 2017
-
[26]
S. Saini and P. Singh, Generic absence of strong singularities in loop quantum Bianchi-IX spacetimes, Class. Quant. Grav.35, 065014 (2018), arXiv:1712.09474
Pith/arXiv arXiv 2018
-
[27]
M. A. Nielsen, A geometric approach to quantum circuit lower bounds, Quant. Inf. Comput.6, 213 (2006), arXiv:quant-ph/0502070
Pith/arXiv arXiv 2006
-
[28]
M. A. Nielsen, M. R. Dowling, M. Gu, and A. C. Doherty, Quantum Computation as Geometry, Science311, 1133 (2006), arXiv:quant-ph/0603161
Pith/arXiv arXiv 2006
-
[29]
M. R. Dowling and M. A. Nielsen, The geometry of quantum computation, Quant. Inf. Comput.8, 0861 (2008), arXiv:quant-ph/0701004
Pith/arXiv arXiv 2008
-
[30]
P. Caputa, J. M. Magan, and D. Patramanis, Geometry of Krylov complexity, Phys. Rev. Res.4, 013041 (2022), arXiv:2109.03824
Pith/arXiv arXiv 2022
-
[31]
P. Nandy, A. S. Matsoukas-Roubeas, P. Mart ´ ınez-Azcona, A. Dymarsky, and A. del Campo, Quan- tum dynamics in Krylov space: Methods and applications, Phys. Rept.1125-1128, 1 (2025), arXiv:2405.09628
Pith/arXiv arXiv 2025
-
[32]
E. Rabinovici, A. S´ anchez-Garrido, R. Shir, and J. Sonner, Krylov Complexity, (2025), arXiv:2507.06286, arXiv: 2507.06286 [hep-th]
Pith/arXiv arXiv 2025
-
[33]
P. Caputa, H.-S. Jeong, S. Liu, J. F. Pedraza, and L.-C. Qu, Krylov complexity of density matrix operators, JHEP05, 337 (2024), arXiv:2402.09522
Pith/arXiv arXiv 2024
-
[34]
F. B. Trigueros and C.-J. Lin, Krylov complexity of many-body localization: Operator localization in Krylov basis, SciPost Phys.13, 037 (2022), arXiv:2112.04722
Pith/arXiv arXiv 2022
-
[35]
E. Rabinovici, A. S´ anchez-Garrido, R. Shir, and J. Sonner, Operator complexity: a journey to the edge of Krylov space, JHEP06, 062 (2021), arXiv:2009.01862
Pith/arXiv arXiv 2021
-
[36]
A. Avdoshkin, A. Dymarsky, and M. Smolkin, Krylov complexity in quantum field theory, and beyond, JHEP06, 066 (2024), arXiv:2212.14429
Pith/arXiv arXiv 2024
-
[37]
A. Dymarsky and M. Smolkin, Krylov complexity in conformal field theory, Phys. Rev. D104, L081702 (2021), arXiv:2104.09514
Pith/arXiv arXiv 2021
-
[38]
S. Baigueraet al., Quantum complexity in gravity, quantum field theory, and quantum information science, (2025), arXiv:2503.10753
arXiv 2025
-
[39]
H. A. Camargo, V. Jahnke, K.-Y. Kim, and M. Nishida, Krylov complexity in free and interacting scalar field theories with bounded power spectrum, JHEP05, 226 (2023), arXiv:2212.14702
Pith/arXiv arXiv 2023
-
[40]
K. Adhikari and S. Choudhury, Cosmological Krylov Complexity, Fortsch. Phys.70, 2200126 (2022), arXiv:2203.14330
Pith/arXiv arXiv 2022
-
[41]
P. H. S. Bento, A. del Campo, and L. C. C´ eleri, Krylov complexity and dynamical phase transition in the quenched Lipkin-Meshkov-Glick model, Phys. Rev. B109, 224304 (2024), arXiv:2312.05321
Pith/arXiv arXiv 2024
-
[42]
P. G. Bergmann, ’Gauge-Invariant’ Variables in General Relativity, Phys. Rev.124, 274 (1961)
1961
-
[43]
P. G. Bergmann, Observables in General Relativity, Rev. Mod. Phys.33, 510 (1961)
1961
-
[44]
Komar, Construction of a Complete Set of Independent Observables in the General Theory of Relativity, Phys
A. Komar, Construction of a Complete Set of Independent Observables in the General Theory of Relativity, Phys. Rev.111, 1182 (1958)
1958
-
[45]
K. V. Kuchar, Time and interpretations of quantum gravity, Int. J. Mod. Phys.D20, 3 (2011)
2011
-
[46]
Isham, Canonical quantum gravity and the problem of time, NATO Sci
C. Isham, Canonical quantum gravity and the problem of time, NATO Sci. Ser. C409, 157 (1993), arXiv:gr-qc/9210011
Pith/arXiv arXiv 1993
-
[47]
Rovelli, What Is Observable in Classical and Quantum Gravity?, Class
C. Rovelli, What Is Observable in Classical and Quantum Gravity?, Class. Quant. Grav.8, 297 (1991)
1991
-
[48]
Rovelli, Partial observables, Phys
C. Rovelli, Partial observables, Phys. Rev.D65, 124013 (2002), arXiv:gr-qc/0110035
Pith/arXiv arXiv 2002
-
[49]
A. S. Vytheeswaran, Gauge unfixing in second class constrained systems, Annals Phys.236, 297 (1994)
1994
-
[50]
Dittrich, Partial and complete observables for Hamiltonian constrained systems, Gen
B. Dittrich, Partial and complete observables for Hamiltonian constrained systems, Gen. Rel. Grav. 39, 1891 (2007), arXiv:gr-qc/0411013
Pith/arXiv arXiv 2007
-
[51]
Dittrich, Partial and complete observables for canonical general relativity, Class
B. Dittrich, Partial and complete observables for canonical general relativity, Class. Quant. Grav.23, 6155 (2006), arXiv:gr-qc/0507106
Pith/arXiv arXiv 2006
-
[52]
Thiemann, Reduced phase space quantization and Dirac observables, Class
T. Thiemann, Reduced phase space quantization and Dirac observables, Class. Quant. Grav.23, 1163 (2006), arXiv:gr-qc/0411031
Pith/arXiv arXiv 2006
-
[53]
K. Giesel, B.-F. Li, and P. Singh, Towards a reduced phase space quantization in loop quantum cosmology with an inflationary potential, Phys. Rev. D102, 126024 (2020), arXiv:2007.06597
Pith/arXiv arXiv 2020
-
[54]
A. Corichi and P. Singh, Quantum bounce and cosmic recall, Phys. Rev. Lett.100, 161302 (2008), 26 arXiv:0710.4543
Pith/arXiv arXiv 2008
-
[55]
W. Kaminski and T. Pawlowski, Cosmic recall and the scattering picture of Loop Quantum Cosmology, Phys. Rev. D81, 084027 (2010), arXiv:1001.2663
Pith/arXiv arXiv 2010
-
[56]
D. A. Craig and P. Singh, Consistent Probabilities in Wheeler-DeWitt Quantum Cosmology, Phys. Rev. D82, 123526 (2010), arXiv:1006.3837
Pith/arXiv arXiv 2010
-
[57]
D. A. Craig and P. Singh, Consistent probabilities in loop quantum cosmology, Class. Quant. Grav. 30, 205008 (2013), arXiv:1306.6142
Pith/arXiv arXiv 2013
-
[58]
Lanczos, An iteration method for the solution of the eigenvalue problem of linear differential and integral operators, J
C. Lanczos, An iteration method for the solution of the eigenvalue problem of linear differential and integral operators, J. Res. Natl. Bur. Stand. B45, 255 (1950)
1950
-
[59]
J. L. F. Barb´ on, E. Rabinovici, R. Shir, and R. Sinha, On The Evolution Of Operator Complexity Beyond Scrambling, JHEP10, 264 (2019), arXiv:1907.05393
Pith/arXiv arXiv 2019
-
[60]
D. Marolf, Refined algebraic quantization: Systems with a single constraint, (1995), arXiv:gr- qc/9508015
arXiv 1995
-
[61]
A. Ashtekar, J. Lewandowski, D. Marolf, J. Mourao, and T. Thiemann, Quantization of diffeomorphism invariant theories of connections with local degrees of freedom, J. Math. Phys.36, 6456 (1995), arXiv:gr- qc/9504018
arXiv 1995
-
[62]
A. Ashtekar, L. Bombelli, and A. Corichi, Semiclassical states for constrained systems, Phys. Rev. D 72, 025008 (2005), arXiv:gr-qc/0504052
Pith/arXiv arXiv 2005
-
[63]
A. Ashtekar, M. Bojowald, and J. Lewandowski, Mathematical structure of loop quantum cosmology, Adv. Theor. Math. Phys.7, 233 (2003), arXiv:gr-qc/0304074
Pith/arXiv arXiv 2003
-
[64]
A. Corichi, T. Vukasinac, and J. A. Zapata, Polymer Quantum Mechanics and its Continuum Limit, Phys. Rev. D76, 044016 (2007), arXiv:0704.0007
Pith/arXiv arXiv 2007
-
[65]
A. Corichi and E. Montoya, Coherent semiclassical states for loop quantum cosmology, Phys. Rev. D 84, 044021 (2011), arXiv:1105.5081
Pith/arXiv arXiv 2011
-
[66]
A. Corichi and O. Gallegos, Entropy in Loop Quantum Cosmology, (2025), arXiv:2505.09055
Pith/arXiv arXiv 2025
-
[67]
A. Corichi and O. Gallegos, An Extended Second Law of Thermodynamics, (2025), arXiv:2510.17560
Pith/arXiv arXiv 2025
-
[68]
M. Weilenmann, L. Kr¨ amer, P. Faist, and R. Renner, Axiomatic relation between thermodynamic and information-theoretic entropies, Phys. Rev. Lett.117, 260601 (2016), arXiv:1501.06920
Pith/arXiv arXiv 2016
-
[69]
A. E. Motter, Relativistic chaos is coordinate invariant, Phys. Rev. Lett.91, 231101 (2003), arXiv:gr- qc/0305020
arXiv 2003
-
[70]
K. Hashimoto, K. Murata, N. Tanahashi, and R. Watanabe, Krylov complexity and chaos in quantum mechanics, JHEP11, 040 (2023), arXiv:2305.16669
Pith/arXiv arXiv 2023
-
[71]
M. Bojowald and G. Date, Quantum suppression of the generic chaotic behavior close to cosmological singularities, Phys. Rev. Lett.92, 071302 (2004), arXiv:gr-qc/0311003
Pith/arXiv arXiv 2004
-
[72]
S. PG, J. B. Kannan, R. Modak, and S. Aravinda, Dependence of Krylov complexity saturation on the initial operator and state, Phys. Rev. E112, L032203 (2025), arXiv:2503.03400
Pith/arXiv arXiv 2025
-
[73]
B. Craps, O. Evnin, and G. Pascuzzi, Multiseed Krylov Complexity, Phys. Rev. Lett.134, 050402 (2025), arXiv:2409.15666
Pith/arXiv arXiv 2025
discussion (0)
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