Pith. sign in

REVIEW 3 major objections 4 minor 42 references

Collisional decoherence overdamps neutron–mirror-neutron conversion in neutron stars, so the mirror admixture stays tiny at all times.

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 →

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

T0 review · grok-4.5

2026-07-14 22:30 UTC pith:JPPYL43R

load-bearing objection Clean Lindblad application shows n–n′ is overdamped in NS matter; the tiny-admixture claim is solid under the stated premises but rests on idealizations that matter for mixed-star conclusions. the 3 major comments →

arxiv 2603.11930 v2 pith:JPPYL43R submitted 2026-03-12 hep-ph astro-ph.HE

Overdamping of Neutron-Mirror-Neutron Transitions in Neutron Stars

B.O. Kerbikov This is my paper
classification hep-ph astro-ph.HE
keywords neutron-mirror-neutron oscillationsneutron starscollisional decoherenceLindblad equationoverdampingopen quantum systemsmirror matter
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

The paper argues that neutron-to-mirror-neutron conversion inside a neutron star does not proceed by coherent oscillations. High-rate collisions with surrounding neutrons destroy the off-diagonal coherences of the two-state density matrix on timescales many orders of magnitude shorter than the vacuum oscillation period. The correct description is therefore an open quantum system governed by Lindblad/Bloch equations with a friction term proportional to the collision rate. In the resulting overdamped regime the ordinary-neutron population decays only exponentially at the suppressed rate 4ε²/M, while the mirror-neutron population is further suppressed by a factor 4ε²/M² and remains negligible. Consequently the conversion rate itself is tiny (∼10⁻²⁰ yr⁻¹ for laboratory-scale ε), and the star never becomes appreciably mixed by this mechanism alone.

Core claim

Inside neutron-star matter the n–n′ system is overdamped (M ≫ ε). After a transient of duration ∼1/M the populations evolve as ρ₁₁(t) ≃ exp(−4ε² t / M) and ρ₂₂(t) ≃ (4ε²/M²) exp(−4ε² t / M), so the transition rate is Γ(n–n′) = 4ε²/M and the mirror admixture is suppressed by ∼(ε/M)² ≪ 1 at every later time.

What carries the argument

The Lindblad/Bloch equation for the reduced n–n′ density matrix, with a jump operator that acts only on the ordinary-neutron component and generates the friction parameter M = ½ n σ v. This term replaces unitary oscillations by overdamped relaxation when M ≫ ε.

Load-bearing premise

The jump operator is assumed to act only on ordinary neutrons (exact Z₂ symmetry, no mirror-matter scattering, negligible mirror density), so any appreciable mirror component would change the dissipator and the overdamping conclusion.

What would settle it

A first-principles calculation of the n–n′ collision rate M in dense nuclear matter that yields M ≲ 2ε, or an observation that a neutron star has already evolved into a substantially mixed ordinary-plus-mirror object on a timescale shorter than M/4ε².

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper argues that n–n′ conversion inside a neutron star is overdamped by collisional decoherence rather than oscillatory. Using the reduced density matrix and Lindblad/Bloch equations with a jump operator that acts only on the ordinary-neutron component, it reduces the dynamics (after dropping Vz) to a damped oscillator. With M ≫ ε the long-time populations are ρ11(t) ≃ exp(−4ε² t/M) and ρ22(t) ≃ (4ε²/M²) exp(−4ε² t/M), so the transition rate is Γ = 4ε²/M and the mirror admixture remains ≪ 1 at all times. An asymptotic branching ratio under the same assumptions is used to contrast with mixed-star scenarios.

Significance. If the overdamping result and the small-admixture conclusion hold under realistic NS conditions, they would substantially revise the literature on neutron-star conversion into mixed ordinary/mirror stars and the associated observational signatures. The vacuum limit is recovered correctly, the reduction to the damped Bloch oscillator is standard and algebraically clean, and the rate formula follows from the Lindblad algebra rather than a fit. The work therefore supplies a concrete, falsifiable alternative to Hamiltonian-only treatments of n–n′ conversion in dense matter.

major comments (3)
  1. [Sec. 4, Eqs. (27)–(30)] Sec. 4, Eqs. (27)–(30): the analytic overdamped solution and the long-time populations (35)–(38) are obtained only after setting Vz = d + K to zero. The paper itself states that the full set (22)–(25) or (27) “can hardly be solved analytically.” Because the central claim that the mirror admixture remains very small at all times rests on those populations, either a controlled expansion in Vz/M, a numerical solution of the full Bloch system for representative d and K, or an explicit bound showing that retained Vz does not reopen a coherent channel is needed.
  2. [Sec. 4, Eqs. (20)–(21); Sec. 6, Eq. (39)] Sec. 4, assumptions 2–3 and Eqs. (20)–(21); Sec. 6, Eq. (39): the jump operator is taken as L̂ = √(nv) F̂ with F̂ = diag(f(θ), 0), which freezes ordinary density n and forbids n′–OM scattering and n′–n′ regeneration. The asymptotic branching ratio used to contrast with mixed-star scenarios is derived under exactly these restrictions. If a non-negligible mirror component builds up, the dissipator changes form and the factor 4ε²/M that suppresses ρ22 can be lifted. The manuscript should either justify that the mirror density remains negligible throughout the evolution or estimate how the rate and admixture change once a mirror component is allowed.
  3. [Sec. 4, Eq. (32)] Sec. 4, estimate of M (around Eq. (32)): M ≃ 0.4 × 10⁸ eV is obtained from n = 2n₀, σ ≃ 30 mb (taken from Fig. 7 of Ref. [39] with the authors’ own caveat that the in-medium cross section is not well defined), and v ≃ 0.4. Because the hierarchy M/ε ∼ 10²⁵–10²⁶ and the numerical rate Γ are load-bearing for the overdamping claim, a short sensitivity discussion (range of n, Pauli-blocked σ, and velocity) is required to show that M ≫ ε survives reasonable variations.
minor comments (4)
  1. [Sec. 5] In Sec. 5 the text writes “δ = 1.5 · 10⁻¹³ eV” while the rest of the paper uses ε = 1.5 · 10⁻¹⁸ eV; this appears to be a typographical inconsistency that should be corrected.
  2. [Sec. 5] The coefficient relating M to the mean free time t_nn is left model-dependent (Sec. 5). A short explicit statement that Γ ∼ ε² t_nn with an O(1) coefficient of uncertain magnitude would clarify the comparison with earlier Schrödinger-based estimates.
  3. [Sec. 6] β-decay is omitted from the dynamical equations and restored only for the asymptotic branching ratio (39). A sentence on whether the free-neutron lifetime remains a good proxy inside the NS would help the reader.
  4. Typographical items: “Acknowlegments”, “propostionality”, and the repeated author name in Ref. [37] should be cleaned up.

Circularity Check

1 steps flagged

No significant circularity: overdamping rate follows from Lindblad algebra with external ε and estimated M; self-citations are contextual, not load-bearing.

specific steps
  1. self citation load bearing [Sec. VI, Eq. (39) and surrounding text; also Ref. [17]]
    "Following [28, 29, 17] we integrate the system of equations (22)-(25) with the initial conditions ρ₁₁(t=0)=1, ρ₂₂=ρ₁₂=ρ₂₁=0, and obtain the following result for the n′ branching ratio Br(n′)≃(M/γ)(2ε^{2}/(M^{2}+K^{2}))"

    The asymptotic branching-ratio formula is presented as following [28, 29, 17], where [17] is the author’s own prior PRD paper. This is a minor self-citation that supplies a calculational template rather than a uniqueness theorem or a fitted parameter that forces the main overdamping claim. The primary rate Γ=4ε^{2}/M is derived independently from the Lindblad/Bloch algebra in Sec. IV and does not rest on [17]. Hence the step is noted but does not raise the score above 1.

full rationale

The central claim (overdamped relaxation with Γ=4ε^{2}/M and ρ₂₂ ≪ 1) is obtained by writing the Lindblad equation with a jump operator that acts only on the ordinary-neutron component, reducing the Bloch dynamics (after dropping Vz) to the friction oscillator (30), and solving it under M ≫ ε. ε is taken from an external free-neutron experiment [30]; M is estimated from nuclear-matter density and a published nn cross-section figure [39]. Neither parameter is fitted to the target populations or to mixed-star phenomenology. The asymptotic branching ratio (39) is an optional extension that again uses the same external inputs plus the free-neutron lifetime. Self-citations ([17] and the author’s earlier related work) supply context and comparison but are not invoked as uniqueness theorems or as the sole justification of the dissipator. The idealizations (dropping Vz, freezing n, forbidding n′–OM scattering) are modeling assumptions that affect correctness risk, not circular reductions of the form “prediction = input by construction.” Score 1 reflects only the minor presence of author self-citation that is not load-bearing for the derivation.

Axiom & Free-Parameter Ledger

2 free parameters · 5 axioms · 0 invented entities

The central claim rests on standard open-quantum-system mathematics plus a short list of domain assumptions about mirror symmetry and the absence of mirror-matter interactions inside the star. No new particles or forces are invented; the free parameters are external experimental or nuclear-physics inputs, not fitted to the target rate.

free parameters (2)
  • ε (n–n′ mixing amplitude) = 1.5e-18 eV (baseline); literature range up to ~1e-11 eV
    Taken from free-neutron oscillation searches (quoted value 1.5×10⁻¹⁸ eV) or from larger values discussed in the literature (up to 10⁻¹¹ eV). Not fitted inside the paper; the overdamping conclusion holds for any ε ≪ M.
  • M (collisional friction / decoherence rate) = ~0.4e8 eV (~1e23 s⁻¹)
    Estimated as (1/2)nσv with n=2n₀, σ≃30 mb (from a medium-dependent plot), v≃0.4. Order-of-magnitude only; the precise numerical value is not critical provided M/ε ≫ 1.
axioms (5)
  • domain assumption Exact Z₂ mirror symmetry: m_n = m_n′ and equal free lifetimes.
    Stated as assumption 1 in Sec. 4; used to set the diagonal entries of H equal (apart from medium shifts) and to assign γ_n′ = γ_n in the branching-ratio estimate.
  • domain assumption Mirror neutrons do not scatter on ordinary matter and there is no n′–n regeneration.
    Assumption 2 of Sec. 4; directly determines the form of the Lindblad operator L̂ = √(nv) diag(f,0).
  • domain assumption Admixture of mirror matter inside the NS is negligible, so n′–n′ scattering can be ignored.
    Assumption 3 of Sec. 4; keeps the dissipator one-sided and prevents a back-reaction term that would alter the long-time balance.
  • standard math The reduced dynamics of the n–n′ subsystem is completely positive and Markovian, i.e., of Lindblad form.
    Invoked throughout Secs. 3–4; standard for open quantum systems under the usual weak-coupling / short-memory approximations.
  • domain assumption β-decay can be omitted for the short-time overdamping analysis (re-introduced only for the asymptotic branching ratio).
    Assumption 4 of Sec. 4; simplifies the Bloch equations to the pure damping form used for Eqs. 29–36.

pith-pipeline@v1.1.0-grok45 · 13639 in / 3644 out tokens · 27793 ms · 2026-07-14T22:30:40.232864+00:00 · methodology

0 comments
read the original abstract

The neutron to mirror neutron transitions in neutron stars would possibly result in significant effects. In this work we show that collisional decoherence entails exponential relaxation in lieu of oscillations. Decoherence is a great many orders of magnitude faster than the expected oscillations. The admixture of mirror neutrons at all times remains very small with respect to ordinary neutrons component.

discussion (0)

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

Reference graph

Works this paper leans on

42 extracted references · 26 linked inside Pith

  1. [1]

    T. D. Lee and C. N. Yang,Phys. Rev.104, 254 (1956)

    1956

  2. [2]

    Kobzarev, L

    I. Kobzarev, L. Okun, and I. Pomeranchuk,Sov. J. Nucl. Phys.3, 837 (1966)

    1966

  3. [3]

    L. B. Okun,Phys. Usp.50, 380 (2007),arXiv:hep-ph/0606202

    Pith/arXiv arXiv 2007

  4. [4]

    Blinnikov and M

    S. Blinnikov and M. Khlopov,Sov. J. Nucl. Phys.36, 472 (1982)

    1982

  5. [5]

    H. M. Hodges,Phys. Rev.D 47, 456 (1993)

    1993

  6. [6]

    Z. G. Berezhiani, A. D. Dolgov, and R. N. Mohapatra,Phys. Lett.B 375, 26 (1996),arXiv:hep-ph/9511221

    Pith/arXiv arXiv 1996

  7. [7]

    R. N. Mohapatra, S. Nussinov, and V. L. Teplitz,Phys. Rev.D 66, 063002 (2002),arXiv:hep-ph/0111381

    Pith/arXiv arXiv 2002

  8. [8]

    Foot,Int

    R. Foot,Int. J. Mod. Phys.A 29, 1430013 (2014),arXiv:1401.3965 [astro-ph.CO]

    Pith/arXiv arXiv 2014

  9. [9]

    A quest for weak objects and for invisible stars

    S. I. Blinnikov, “A quest for weak objects and for invisible stars”,arXiv: astro-ph/9801015

    Pith/arXiv arXiv

  10. [10]

    Foot,Phys

    R. Foot,Phys. Lett.B 452, 83 (1999),arXiv:astro-ph/9902065

    Pith/arXiv arXiv 1999

  11. [11]

    R. N. Mohapatra and V. L. Teplitz,Phys. Lett.B 462, 302 (1999), arXiv:astro-ph/9902085. 10

    Pith/arXiv arXiv 1999

  12. [12]

    J. M. Lattimer,Ann. Rev. Nucl. Part. Sci.71, 433 (2021)

    2021

  13. [13]

    Unusual effects inn−n ′ conversion

    Z. Berezhiani, “Unusual effects inn−n ′ conversion”, Talk at the Workshop INT-17-69W, Seattle, 23–27 Oct. 2017

    2017

  14. [14]

    Goldman, R

    I. Goldman, R. N. Mohapatra, and S. Nussinov,Phys. Rev.D 100, 123021 (2019),arXiv:1901.07077 [hep-ph]

    Pith/arXiv arXiv 2019

  15. [15]

    Berezhiani, R

    Z. Berezhiani, R. Biondi, M. Mannarelli, and F. Tonelli,Eur. Phys. J.C 81, 1036 (2021),arXiv:2012.15233 [astro-ph.HE]

    Pith/arXiv arXiv 2021

  16. [16]

    McKeen, M

    D. McKeen, M. Pospelov, and N. Raj,Phys. Rev. Lett.127, 061805 (2021), arXiv:2105.09951 [hep-ph]

    Pith/arXiv arXiv 2021

  17. [17]

    B. O. Kerbikov,Phys. Rev.D 106, 015015 (2022),arXiv:2112.14157 [hep-ph]

    Pith/arXiv arXiv 2022

  18. [18]

    Goldman, R

    I. Goldman, R. N. Mohapatra, S. Nussinov, and Y. Zhang,Phys. Rev. Lett. 129, 061103 (2022),arXiv:2208.03771 [hep-ph]

    Pith/arXiv arXiv 2022

  19. [19]

    Goldman, R

    I. Goldman, R. N. Mohapatra, S. Nussinov, and Y. Zhang,Eur. Phys. J.C 82, 945 (2022),arXiv:2203.08473 [hep-ph]

    Pith/arXiv arXiv 2022

  20. [20]

    L. D. Landau and E. M. Lifshitz,Quantum Mechanics: Course of Theoretical Physics, Vol. 3 (Pergamon Press, Oxford, 1978)

    1978

  21. [21]

    R. P. Feynman,Statistical Mechanics: A Set of Lectures(W. A. Benjamin Inc., Mass., 1972)

    1972

  22. [22]

    Breuer and F

    H.-P. Breuer and F. Petruccione,The Theory of Open Quantum Systems(OUP, New York, 2002)

    2002

  23. [23]

    Quantum Damping and its Paradoxes

    L. Stodolsky, “Quantum Damping and its Paradoxes” inQuantum Coherence, Ed. by J. S. Anandan (World Scientific, Singapore, 1990)

    1990

  24. [24]

    Lindblad,Commun

    G. Lindblad,Commun. Math. Phys.48, 119 (1976)

    1976

  25. [25]

    Kossakowski,Rep

    A. Kossakowski,Rep. Math. Phys.3, 247 (1972); V. Gorini, A. Kossakowski, and E. C. G. Sudarshan,J. Math. Phys.17, 821 (1976)

    1972

  26. [26]

    Bloch,Phys

    F. Bloch,Phys. Rev.70, 460 (1946)

    1946

  27. [27]

    Feynman, F

    R. Feynman, F. Vernon, and R. Hellwarth,Jour. of Appl. Phys.28, 49 (1957)

    1957

  28. [28]

    Feinberg and S

    G. Feinberg and S. Weinberg,Phys. Rev.123, 1439 (1961)

    1961

  29. [29]

    S. V. Demidov, D. S. Gorbunov, and A. A. Tokareva,Phys. Rev.D 85, 015022 (2012),arXiv:1111.1072 [hep-ph]. 11

    Pith/arXiv arXiv 2012

  30. [30]

    A. P. Serebrov, E. B. Aleksandrov, N. A. Dovator, et al.,Phys. Lett.B 663, 181 (2008),arXiv:0706.3600 [nucl-ex]

    Pith/arXiv arXiv 2008

  31. [31]

    Berezhiani,Universe8, 313 (2022)

    Z. Berezhiani,Universe8, 313 (2022)

    2022

  32. [32]

    Pearle,Eur

    P. Pearle,Eur. J. Phys.33, 805 (2012),arXiv:1204.2016 [math-ph]

    Pith/arXiv arXiv 2012

  33. [33]

    Weinberg,Phys

    S. Weinberg,Phys. Rev.A 94, 042117 (2016),arXiv:1610.02537 [quant-ph]

    Pith/arXiv arXiv 2016

  34. [34]

    Braaten, H.-W

    E. Braaten, H.-W. Hammer, and G. P. Lepage,Phys. Rev.A 95, 012708 (2017), arXiv:1607.08084 [cond-mat.quant-gas]

    Pith/arXiv arXiv 2017

  35. [35]

    A. D. Dolgov,Phys. Rept.370, 333 (2002),arXiv:hep-ph/0202122

    Pith/arXiv arXiv 2002

  36. [36]

    Akamatsu,Phys

    Y. Akamatsu,Phys. Rev.D 91, 056002 (2015),arXiv:1403.5783 [hep-ph]

    Pith/arXiv arXiv 2015

  37. [37]

    Brambilla, N

    N. Brambilla, N. Brambilla, M. A. Escobedo,et al.,Phys. Rev.D 108, L011502 (2023),arXiv:2302.11826 [hep-ph]

    Pith/arXiv arXiv 2023

  38. [38]

    Nikolic,JCAP04, 002 (2015),arXiv:1502.04324 [hep-th]

    H. Nikolic,JCAP04, 002 (2015),arXiv:1502.04324 [hep-th]

    Pith/arXiv arXiv 2015

  39. [39]

    P. S. Shternin, M. Baldo, and P. Haensel,Phys. Rev.C 88, 065803 (2013), arXiv:1311.4278 [astro-ph.SR]

    Pith/arXiv arXiv 2013

  40. [40]

    Gal,Phys

    A. Gal,Phys. Rev.C 61, 028201 (2000),arXiv:hep-ph/9907334

    Pith/arXiv arXiv 2000

  41. [41]

    Redondo,JCAP07, 024 (2015),arXiv:1501.07292 [hep-ph]

    J. Redondo,JCAP07, 024 (2015),arXiv:1501.07292 [hep-ph]

    Pith/arXiv arXiv 2015

  42. [42]

    Demidov, S

    S. Demidov, S. Gninenko, and D. Gorbunov,JHEP07, 162 (2019), arXiv:1812.02719 [hep-ph]. 12

    Pith/arXiv arXiv 2019