Pith. sign in

REVIEW 3 major objections 5 minor 54 references

The paper establishes that an exotic species produces a distinct composition g-mode in a neutron star only when its composition gradient—or a coupled slowly equilibrating gradient—survives over the oscillation period.

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 · deepseek-v4-flash

2026-08-01 09:38 UTC pith:54EDWXTN

load-bearing objection First full-GR g1-mode calculation for antikaon-condensed neutron stars; the numbers are credible and the reaction-limit hierarchy is useful, but the surviving high-frequency NYDelta branch rests on an uncalculated Lambda equilibration rate that the paper honestly flags. the 3 major comments →

arxiv 2607.20693 v1 pith:54EDWXTN submitted 2026-07-22 astro-ph.HE nucl-th

Reaction-constrained composition \(g\)-modes in neutron stars with antikaon condensates, hyperons, and \(Delta(1232)\) resonances

Prashant Thakur , Ishfaq Ahmad Rather This is my paper
classification astro-ph.HE nucl-th
keywords neutron star asteroseismologycomposition g-modesantikaon condensatehyperonsDelta baryonsreaction timescalesgravitational-wave asteroseismologytidal phase shift
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.

This paper establishes a general criterion for when exotic matter leaves a measurable fingerprint in neutron-star oscillations: an exotic species produces a distinct composition g-mode only if its composition gradient—or a coupled slowly equilibrating gradient—survives over the oscillation period. Working in full general relativity with a relativistic mean-field equation of state, the authors compute the core g1-mode frequency, gravitational-wave damping time, and tidal overlap for neutron stars containing antikaon condensates, hyperons, and Delta(1232) baryons. They show that fast equilibration of the reaction n↔p+K− retains 36–44% of the peak local kaon buoyancy and keeps the mode's terminal frequency at 65.7–73.4% of its frozen value, still above the nucleonic band, while strong equilibrium within the Delta quartet removes most direct Delta-induced enhancement and returns the NDelta mode toward the nucleonic band. A high-frequency NYDelta branch survives, but only because the Lambda fraction is kept frozen. If correct, these results tell observers which reaction channels must be slow for a composition mode to be detectable.

Core claim

The paper's central discovery is that the reaction state of matter, not just its composition, decides whether a continuous-composition g-mode exists. For an antikaon-condensed core, even when the nonleptonic weak reaction n↔p+K− is fast enough to maintain chemical equilibrium, the mode does not vanish: the fast-K limit retains 36–44% of the peak local buoyancy and 65.7–73.4% of the frozen-composition terminal frequencies, so the kaon-induced mode remains above the nucleonic band. For Delta-admixed matter, imposing strong equilibrium within the Delta quartet removes most of the direct Delta-induced buoyancy, pulling the NDelta mode back near the nucleonic band; the high-frequency NYDelta bran

What carries the argument

The key machinery is a species-resolved decomposition of the composition-buoyancy term L = 1/c_e^2 − 1/c_s^2, where c_s is the sound speed at frozen particle fractions and c_e is the beta-equilibrium sound speed; the decomposition splits L into exact per-channel contributions, each tied to an independent composition variable. Weighted by the mode's eigenfunction, these channels yield positive or negative fractions identifying which species drives the g1-mode buoyancy, and the attribution is cross-checked by rescaling each channel's contribution and measuring the eigenfrequency response. The reaction-timescale constraints are imposed as limits: fully frozen fractions, fast equilibrium for n↔p

Load-bearing premise

The load-bearing premise is that hyperon (Lambda) fractions remain frozen during the oscillation; the paper explicitly notes that no hyperonic reaction-rate calculation has been performed, so if Lambda-to-nucleon weak reactions equilibrate as fast as the mode period, the surviving high-frequency NYDelta branch would disappear.

What would settle it

A quantum many-body calculation of the Lambda-to-nucleon weak interaction rate at supranuclear densities showing a relaxation time well under one millisecond would falsify the paper's claim that the high-frequency NYDelta branch survives strong Delta equilibration; in that case the mode would relax toward the nucleonic band. Alternatively, a future gravitational-wave measurement of a resonant tidal phase shift near 0.1 rad in the 300–700 Hz band would contradict the paper's prediction of at most about 1e-3 rad for smooth composition stratification.

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

If this is right

  • A kaon-condensed neutron star should show a core g1-mode above the nucleonic band even if the n↔p+K− reaction is fast; the frequency is at least about two-thirds of the frozen-composition value.
  • If strong Delta equilibrium holds, a Delta-admixed star alone cannot sustain a composition mode far above the nucleonic band; a high-frequency branch requires an additional slowly equilibrating species such as the Lambda hyperon.
  • Gravitational-wave damping times for these modes are orders of magnitude longer than binary-inspiral resonance crossing times, so gravitational radiation does not prevent resonant tidal excitation.
  • The frozen-composition tidal phase shifts (at most about 1.4e-3 rad) are well below the roughly 0.03-rad scale quoted for detection in third-generation observatories, implying smooth composition stratification is a weak tidal-resonance source compared with sharp phase-transition interfaces.
  • Representative calculations with a second, density-dependent equation of state reproduce the same reaction-channel hierarchy, suggesting the qualitative conclusions are not artifacts of one equation of state.

Where Pith is reading between the lines

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

  • The paper leaves the Lambda reaction rate uncalculated; if Lambda-to-nucleon weak reactions turn out to equilibrate within the roughly millisecond mode period, the surviving NYDelta branch would drop, so the hierarchy of surviving modes is partly a prediction about which reaction channels are slow.
  • Since the circular-binary phase shifts are tiny, the most effective route to observing these modes may be through eccentric binaries or rotating stars, which the authors note can boost detectability by more than an order of magnitude.
  • The criterion suggests a testable ordering across exotic channels: modes mediated by weak reactions (kaons, hyperons) can survive, while strong-interaction-mediated channels (Delta) are suppressed unless a coupled slow gradient exists; this could prioritize which microphysical reaction rates need measurement.

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 / 5 minor

Summary. The paper studies core composition g1 modes of cold, nonrotating neutron stars containing antikaon condensates, hyperons, and Delta(1232) baryons, using the BigApple RMF equation of state and full general relativity (Lindblom–Detweiler formalism). It introduces a species-resolved Ledoux decomposition and compares fully frozen composition with two reaction-limit prescriptions: a fast-K limit (lepton fractions frozen, n<->p+K- in chemical equilibrium) and a strong-Delta limit (Delta quartet in chemical equilibrium at fixed lepton fractions and hyperon fractions). The main results are: (i) fast-K equilibration retains 36%–44% of the peak local kaon buoyancy and 65.7%–73.4% of the frozen terminal g1 frequencies, keeping the mode above the nucleonic band; (ii) strong-Delta equilibration removes most direct Delta-induced enhancement, returning the N Delta mode toward the nucleonic band, while the high-frequency NYDelta branch survives through the frozen Lambda gradient; (iii) frozen-composition full-GR tidal phase shifts are at most 1.410e-3 rad, about a factor of 21 below the 0.03-rad scale quoted for Einstein Telescope favorable events. The paper concludes that an exotic species produces a distinct composition mode only if its composition gradient, or a coupled slowly equilibrating gradient, survives over the oscillation period. The analysis is supported by resolution-doubling tests (<=0.6%), a Ledoux closure check (<1e-3), and representative DD-ME2 cross-checks that reproduce th

Significance. If correct, this is the first full-GR calculation of continuous-composition g1-mode frequencies and gravitational-wave damping times for neutron stars containing a K- condensate, and it provides a unified reaction-limit comparison across kaons, hyperons, and Delta resonances. The species-resolved Ledoux decomposition and independent frequency-sensitivity validation are useful diagnostics for attributing buoyancy channels. The paper's explicit handling of limiting reaction prescriptions is a step beyond the usual fully frozen assumption. The numerical infrastructure is standard and appears well tested: resolution-doubling changes are small, the species-resolved decomposition closes to <1e-3, and the DD-ME2 test shows robustness of the qualitative hierarchy. The paper is also transparent about its main caveats, especially the uncalculated hyperon reaction rates and the absence of finite-rate calculations. These strengths make the paper a valuable contribution to neutron-star asteroseismology, provided the load-bearing issues identified below are addressed.

major comments (3)
  1. [Sec. III.1] The 'strong equilibrium within the ∆ quartet' prescription is not defined explicitly. Unlike the fast-K limit, which gives the constraints δYe=δYμ=0 and δ(μn-μp-μK-)=0, the strong-Δ limit lacks equations. Specify the chemical potential equalities (e.g., μn+μΔ0 = μp+μΔ- etc.), the variables held fixed (lepton fractions, strangeness/hyperon fractions), and the variables allowed to vary (nucleon and Δ charge fractions). Without this, the central result that strong-Δ equilibration suppresses the direct Δ buoyancy cannot be reproduced or independently verified.
  2. [Sec. III.1 and Conclusions] The survival of the high-frequency NYΔ branch under strong-Δ equilibrium rests entirely on the Λ fraction remaining frozen. The paper states in Sec. III.1 that 'a corresponding hyperonic reaction-rate calculation has not been performed' and in the Conclusions that 'the hyperon fractions remain frozen.' This is a load-bearing limitation: for the 601 Hz mode (P≈1.7 ms), if Λ↔N weak reactions equilibrate on this timescale, the Λ gradient would be erased and the branch could return toward the nucleonic band, as indeed happens for the Δ gradient. The paper is honest about this caveat, but the abstract and conclusions should carry it more prominently, and ideally the authors should provide at least an order-of-magnitude estimate of the Λ equilibration timescale or a physical argument for why the Lambda gradient is expected to remain frozen.
  3. [Sec. II.3 / Table V] The species-resolved decomposition is basis-dependent, as the authors note: choosing a charge-neutral channel includes the associated Yp/Yn rearrangement. This is fine as a diagnostic, but the interpretation of χK-≈1 as 'kaon-dominated' may overstate the physical attribution. The separate frequency-sensitivity coefficients (Sec. III) partially address this. I recommend making the basis-dependence and its consequences more explicit in the main text when interpreting the channel contributions, especially in the abstract's phrase 'kaon buoyancy'.
minor comments (5)
  1. [Sec. II.1] The matching procedure to the BPS crust is mentioned but not described. Provide a sentence or two on how the core EOS is matched (e.g., pressure/density matching point, any interpolation).
  2. [Eq. (14)] The expression for U_Δ^(N)(n0) = -x_σΔ g_σN σ0 + x_ωΔ g_ωN ω0 uses the adopted coupling ratios; clarify the sign convention for the scalar field σ0 (attractive, negative) to avoid ambiguity.
  3. [Sec. III, Table III] The text says 'making the massive configurations progressively more compact' as UK becomes more attractive, but the terminal radius for UK=-160 (12.261 km) is larger than for UK=-140 (12.184 km), because the former terminates at a lower mass. Rephrase to compare at fixed mass or note the EOS-validity endpoint.
  4. [Fig. 8 caption] The absence of the npeμ+Y+Δ 2.0 M⊙ point is explained in the text, but adding a short note in the figure caption would improve clarity.
  5. [Sec. III.2] The tidal phase-shift comparison with the 0.03 rad ET scale is appropriately hedged. Consider also stating explicitly that the phase shifts are frozen-composition values and that reaction-enabled overlaps (fast-K, strong-Δ) have not been computed here, as is done in the text but not in the abstract.

Circularity Check

0 steps flagged

No significant circularity; the central calculation is self-contained and the frozen-hyperon caveat is an openly disclosed conditional, not a circular reduction.

full rationale

The mode frequencies and damping times are obtained by solving the Lindblom–Detweiler full-GR perturbation equations with the BigApple EOS and explicitly stated reaction-limit constraints; no parameter is fitted to the target g-mode results, and the same inputs are used for frozen, fast-K, and strong-Delta limits. The species-resolved Ledoux decomposition is a bookkeeping identity (Eqs. 26-28) with the basis dependence acknowledged in the text ('The per-channel decomposition is therefore defined with respect to this chosen independent basis. The total Ledoux term L is basis independent...'), and the attribution is independently cross-checked with frequency-sensitivity coefficients rather than assumed. The fast-K and strong-Delta limits are fixed thermodynamic constraints, not fitted parameters. The survival of the NYDelta branch under strong Delta equilibrium rests on the frozen Lambda gradient, but the paper states explicitly that 'a corresponding hyperonic reaction-rate calculation has not been performed' and that 'no claim is made that the Lambda-driven branch is protected under all thermodynamic conditions'; this is a transparent physical caveat about an uncalculated rate, not a circular use of the desired conclusion. The DD-ME2 check repeats the same disclosed assumption and therefore does not introduce independent support for that one rate, but it does not make the derivation circular. Self-citations (e.g., refs. 9 and 53) are background or method citations and are not load-bearing. Overall, no equation or fitted parameter reduces to the claimed results by construction.

Axiom & Free-Parameter Ledger

5 free parameters · 5 axioms · 0 invented entities

No new particles, forces, or dimensions are introduced. The free parameters are the EOS and exotic-sector couplings taken from prior nuclear phenomenology, and the axioms are the standard GR perturbation framework plus the paper's explicit reaction-timescale modeling choices. The central results are therefore conditional on these inputs and limiting assumptions.

free parameters (5)
  • Antikaon optical potential U_K = -100, -120, -140, -160 MeV
    Chosen by hand from a standard phenomenological range. It sets the condensation onset density and strongly controls the g1-mode frequency; the quantitative results depend on this unmeasured input.
  • Delta coupling ratios x_sigmaDelta=1.09, x_omegaDelta=1.05, x_rhoDelta=2.5 = as listed
    Adopted from the cited literature; the paper explicitly notes the Delta couplings remain uncertain and does not survey them. These ratios set the Delta onset and the strength of the Delta-induced buoyancy.
  • Hyperon scalar couplings via U_Lambda=-28, U_Sigma=+30, U_Xi=-14 MeV = as listed
    Chosen from empirical hypernuclear potentials at saturation density. They determine when hyperons appear and the hyperon contribution to the buoyancy profiles.
  • BigApple RMF coupling constants = Table I
    The underlying EOS parameters were fitted to nuclear saturation properties in prior work. They set the stellar mass-radius background and therefore all mode frequencies, but they are inputs rather than free parameters fitted here.
  • Antikaon vector couplings g_omegaK = g_omegaN/3, g_rhoK = g_rhoN = as listed
    Chosen by model convention; these couplings affect the in-medium K- energy and hence the condensation threshold.
axioms (5)
  • standard math Lindblom-Detweiler linearized Einstein equations with Regge-Wheeler gauge describe nonradial oscillations
    The whole mode calculation is built on this established GR perturbation formalism, invoked in Sec. II.2.
  • domain assumption The background star is cold, nonrotating, spherically symmetric, and beta-equilibrated at equilibrium
    Stateed at the start of Sec. II and used for the TOV background; rotation, temperature, and eccentric-tidal effects are excluded.
  • domain assumption Composition-changing reactions can be bracketed by frozen and chemical-equilibrium limits without computing finite rates
    The paper explicitly says a finite-rate kinetic treatment is beyond its scope (Sec. III.1, Conclusions), so the reported frequencies and damping times are limiting-case results.
  • domain assumption Hyperon fractions remain frozen during the oscillation
    Stated in Sec. III.1 and Conclusions; the survival of the NYDelta branch under strong Delta equilibration depends on this premise.
  • ad hoc to paper Strong equilibrium within the Delta quartet at fixed lepton fractions and strangeness is a valid limiting case
    This is an imposed thermodynamic constraint, not derived from an in-medium strong-interaction relaxation rate. It models the fast-Delta response.

pith-pipeline@v1.3.0-alltime-deepseek · 21655 in / 12114 out tokens · 104095 ms · 2026-08-01T09:38:10.650425+00:00 · methodology

0 comments
read the original abstract

We study core composition \(g_1\) modes of cold, nonrotating neutron stars containing antikaon condensates, hyperons, and \(\Delta(1232)\) baryons and present, to our knowledge, the first calculation in full general relativity of the continuous-composition \(g_1\)-mode frequency and gravitational-wave damping time for stars with a \(K^-\) condensate. Using the BigApple relativistic mean-field equation of state, we compute frequencies, damping times, and frozen-composition tidal overlaps, and identify the buoyancy channels with a species-resolved Ledoux decomposition validated by mode-frequency sensitivities. We compare fully frozen matter with a fast-\(K\) limit for \(n\leftrightarrow p+K^-\) and a strong-equilibrium limit for the \(\Delta\) quartet. Fast-\(K\) equilibration retains \(36\%\)--\(44\%\) of the peak local kaon buoyancy and \(65.7\%\)--\(73.4\%\) of the frozen terminal-configuration frequencies, while increasing the damping times by factors of \(14.4\)--\(31.8\); the mode remains above the nucleonic band. Strong \(\Delta\) equilibration removes most of the direct \(\Delta\)-induced enhancement, returning the \(N\Delta\) mode toward the nucleonic band, whereas the high-frequency \(NY\Delta\) branch survives through the frozen \(\Lambda\) gradient. Eigenfunction tracking confirms a continuous \(g_1\) branch, and representative DD-ME2 calculations reproduce this hierarchy. The direct full-GR frozen-composition phase shifts satisfy \(|\Delta\Phi_{g_1}|\leq1.410\times10^{-3}\) rad, a factor of 21 below the \(0.03\)-rad favorable-event scale for the Einstein Telescope. An exotic species therefore produces a distinct composition mode only if its composition gradient, or a coupled slowly equilibrating gradient, survives over the oscillation period.

Figures

Figures reproduced from arXiv: 2607.20693 by Ishfaq Ahmad Rather, Prashant Thakur.

Figure 1
Figure 1. Figure 1: FIG. 1: Difference between the adiabatic and equilibrium sound speeds, [PITH_FULL_IMAGE:figures/full_fig_p007_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2: Mass–radius relations for antikaon-condensed [PITH_FULL_IMAGE:figures/full_fig_p008_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: FIG. 3: Full-GR [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4: Left: Difference between the frozen-composition and equilibrium sound speeds, [PITH_FULL_IMAGE:figures/full_fig_p010_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5: Mass–radius sequences for the [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6: Left: Full-GR core [PITH_FULL_IMAGE:figures/full_fig_p011_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7: Full-GR [PITH_FULL_IMAGE:figures/full_fig_p013_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8: Resonant tidal phase shift [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: FIG. 9: DD-ME2 test of the reaction-constrained composition buoyancy. Panel (a) shows the local buoyancy measure [PITH_FULL_IMAGE:figures/full_fig_p017_9.png] view at source ↗

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

54 extracted references · 35 linked inside Pith

  1. [1]

    J. M. Lattimer and M. Prakash, Astrophys. J.550, 426 (2001), arXiv:astro-ph/0002232

    Pith/arXiv arXiv 2001

  2. [2]

    J. M. Lattimer and M. Prakash, Phys. Rept.621, 127 (2016), arXiv:1512.07820 [astro-ph.SR]

    Pith/arXiv arXiv 2016

  3. [3]

    Oertel, M

    M. Oertel, M. Hempel, T. Kl¨ ahn, and S. Typel, Rev. Mod. Phys.89, 015007 (2017), arXiv:1610.03361 [astro-ph.HE]

    Pith/arXiv arXiv 2017

  4. [4]

    B. P. Abbottet al.(LIGO Scientific, Virgo), Phys. Rev. Lett.119, 161101 (2017), arXiv:1710.05832 [gr-qc]

    Pith/arXiv arXiv 2017

  5. [5]

    T. E. Rileyet al., Astrophys. J. Lett.918, L27 (2021), arXiv:2105.06980 [astro-ph.HE]

    Pith/arXiv arXiv 2021

  6. [6]

    M. C. Milleret al., Astrophys. J. Lett.918, L28 (2021), arXiv:2105.06979 [astro-ph.HE]

    Pith/arXiv arXiv 2021

  7. [7]

    Andersson and K

    N. Andersson and K. D. Kokkotas, Mon. Not. Roy. Astron. Soc.299, 1059 (1998), arXiv:gr-qc/9711088

    Pith/arXiv arXiv 1998

  8. [8]

    K. D. Kokkotas and B. G. Schmidt, Living Rev. Rel.2, 2 (1999), arXiv:gr-qc/9909058

    Pith/arXiv arXiv 1999

  9. [9]

    Thakur, A

    P. Thakur, A. Issifu, I. A. Rather, Y. Lim, and T. Frederico, Radial and Non-Radial Oscillations of Pro- toneutron Stars with Hyperonic Composition (2025), arXiv:2505.24104 [nucl-th]

    arXiv 2025

  10. [10]

    K. S. Thorne and A. Campolattaro, Astrophys. J.149, 591 (1967)

    1967

  11. [11]

    Lindblom and S

    L. Lindblom and S. L. Detweiler, Astrophys. J. Suppl.53, 73 (1983)

    1983

  12. [12]

    S. L. Detweiler and L. Lindblom, Astrophys. J.292, 12 (1985)

    1985

  13. [13]

    Benhar, V

    O. Benhar, V. Ferrari, and L. Gualtieri, Phys. Rev. D70, 124015 (2004), arXiv:astro-ph/0407529

    Pith/arXiv arXiv 2004

  14. [14]

    D. D. Doneva and K. D. Kokkotas, Phys. Rev. D92, 124004 (2015), arXiv:1507.06606 [astro-ph.SR]

    Pith/arXiv arXiv 2015

  15. [15]

    K. D. Kokkotas and J. Ruoff, Astron. Astrophys.366, 565 (2001), arXiv:gr-qc/0011093

    Pith/arXiv arXiv 2001

  16. [16]

    Andersson, Universe7, 97 (2021), arXiv:2103.10223 [gr-qc]

    N. Andersson, Universe7, 97 (2021), arXiv:2103.10223 [gr-qc]

    Pith/arXiv arXiv 2021

  17. [17]

    Lai, Mon

    D. Lai, Mon. Not. Roy. Astron. Soc.270, 611 (1994), arXiv:astro-ph/9404062

    Pith/arXiv arXiv 1994

  18. [18]

    V. Tran, S. Ghosh, N. Lozano, D. Chatterjee, and P. Jaiku- mar, Phys. Rev. C108, 015803 (2023), arXiv:2212.09875 [nucl-th]

    Pith/arXiv arXiv 2023

  19. [19]

    T. Zhao, C. Constantinou, P. Jaikumar, and M. Prakash, Phys. Rev. D105, 103025 (2022), arXiv:2202.01403 [gr- qc]

    Pith/arXiv arXiv 2022

  20. [20]

    Sun, J.-X

    H. Sun, J.-X. Niu, Y. Gao, H.-B. Li, and C.-J. Xia, As- teroseismology of neutron stars with both hyperons and ∆ resonances (2026), arXiv:2606.24343 [astro-ph.HE]

    Pith/arXiv arXiv 2026

  21. [21]

    A. R. Counsell, F. Gittins, and N. Andersson, Mon. Not. Roy. Astron. Soc.531, 1721 (2024), arXiv:2310.13586 [astro-ph.HE]

    Pith/arXiv arXiv 2024

  22. [22]

    T. Zhao, P. B. Rau, A. Haber, S. P. Harris, C. Con- stantinou, and S. Han, Astrophys. J.993, 161 (2025), arXiv:2504.12230 [astro-ph.HE]

    arXiv 2025

  23. [23]

    Reisenegger and P

    A. Reisenegger and P. Goldreich, Astrophys. J.426, 688 (1994)

    1994

  24. [24]

    Andersson and P

    N. Andersson and P. Pnigouras, Mon. Not. Roy. Astron. Soc.503, 533 (2021), arXiv:1905.00012 [gr-qc]

    Pith/arXiv arXiv 2021

  25. [25]

    Maggioreet al.(ET), JCAP2020(03), 050, arXiv:1912.02622 [astro-ph.CO]

    M. Maggioreet al.(ET), JCAP2020(03), 050, arXiv:1912.02622 [astro-ph.CO]

    Pith/arXiv arXiv 1912

  26. [26]

    Branchesiet al., JCAP2023(07), 068, arXiv:2303.15923 [gr-qc]

    M. Branchesiet al., JCAP2023(07), 068, arXiv:2303.15923 [gr-qc]

    Pith/arXiv arXiv

  27. [27]

    Evanset al., A Horizon Study for Cosmic Ex- plorer: Science, Observatories, and Community (2021), arXiv:2109.09882 [astro-ph.IM]

    M. Evanset al., A Horizon Study for Cosmic Ex- plorer: Science, Observatories, and Community (2021), arXiv:2109.09882 [astro-ph.IM]

    Pith/arXiv arXiv 2021

  28. [28]

    Chatterjee and D

    D. Chatterjee and D. Bandyopadhyay, Phys. Rev. D75, 123006 (2007), arXiv:astro-ph/0702259

    Pith/arXiv arXiv 2007

  29. [29]

    We therefore calculate both limiting responses: fully frozen composition and strong equilibrium within the ∆ quartet at fixed lepton fractions and strangeness

    illustrates the underlying strong-interaction scale, but it does not by itself determine the chemical relaxation rate in degenerate stellar matter, where phase-space re- strictions, Pauli blocking, and in-medium effects may be important. We therefore calculate both limiting responses: fully frozen composition and strong equilibrium within the ∆ quartet at...

    2024

  30. [30]

    Navaset al.(Particle Data Group), Phys

    S. Navaset al.(Particle Data Group), Phys. Rev. D110, 030001 (2024)

    2024

  31. [31]

    Ledoux, Astrophys

    P. Ledoux, Astrophys. J.105, 305 (1947)

    1947

  32. [32]

    P. N. McDermott, H. M. van Horn, and J. F. Scholl, Astrophys. J.268, 837 (1983)

    1983

  33. [33]

    Reisenegger and P

    A. Reisenegger and P. Goldreich, Astrophys. J.395, 240 (1992)

    1992

  34. [34]

    Gittins, H

    F. Gittins, H. Narola, T. Wouters, P. T. H. Pang, T. Hin- derer, and C. Van Den Broeck, Detecting Tidal Reso- nances in Binary Neutron Stars (2026), arXiv:2606.06376 [gr-qc]

    Pith/arXiv arXiv 2026

  35. [35]

    F. J. Fattoyev, C. J. Horowitz, J. Piekarewicz, and B. Reed, Phys. Rev. C102, 065805 (2020), arXiv:2007.03799 [nucl-th]

    Pith/arXiv arXiv 2020

  36. [36]

    Schaffner, inInternational Conference on Nuclear Physics at the Turn of Millennium: Structure of Vacuum and Elementary Matter(1996) pp

    J. Schaffner, inInternational Conference on Nuclear Physics at the Turn of Millennium: Structure of Vacuum and Elementary Matter(1996) pp. 278–285, arXiv:nucl- th/9605010

    arXiv 1996

  37. [37]

    A. Gal, E. V. Hungerford, and D. J. Millener, Rev. Mod. Phys.88, 035004 (2016), arXiv:1605.00557 [nucl-th]

    Pith/arXiv arXiv 2016

  38. [38]

    K. D. Marquez, D. P. Menezes, H. Pais, and C. Providˆ encia, Phys. Rev. C106, 055801 (2022), arXiv:2206.02935 [nucl-th]

    Pith/arXiv arXiv 2022

  39. [39]

    B.-J. Cai, F. J. Fattoyev, B.-A. Li, and W. G. Newton, Phys. Rev. C92, 015802 (2015), arXiv:1501.01680 [nucl- th]

    Pith/arXiv arXiv 2015

  40. [40]

    Ribes, A

    P. Ribes, A. Ramos, L. Tolos, C. Gonzalez-Boquera, and M. Centelles, Astrophys. J.883, 168 (2019), arXiv:1907.08583 [astro-ph.HE]

    Pith/arXiv arXiv 2019

  41. [41]

    G. Baym, C. Pethick, and P. Sutherland, Astrophys. J. 170, 299 (1971)

    1971

  42. [42]

    Regge and J

    T. Regge and J. A. Wheeler, Phys. Rev.108, 1063 (1957)

    1957

  43. [43]

    Goldreich and A

    P. Goldreich and A. Reisenegger, Astrophys. J.395, 250 (1992)

    1992

  44. [44]

    T. E. Rileyet al., Astrophys. J. Lett.887, L21 (2019), arXiv:1912.05702 [astro-ph.HE]

    Pith/arXiv arXiv 2019

  45. [45]

    M. C. Milleret al., Astrophys. J. Lett.887, L24 (2019), arXiv:1912.05705 [astro-ph.HE]

    Pith/arXiv arXiv 2019

  46. [46]

    M. O. Canullan-Pascual, G. Lugones, I. F. Ranea- Sandoval, and M. G. Orsaria, The Delta-isobar mas- querade: intrahadronic phase transitions and their quark-mimicking signatures in neutron stars (2026), arXiv:2602.22969 [nucl-th]

    arXiv 2026

  47. [47]

    Counsell, F

    R. Counsell, F. Gittins, N. Andersson, and P. Pnigouras, Mon. Not. Roy. Astron. Soc.536, 1967 (2024), arXiv:2409.20178 [gr-qc]

    Pith/arXiv arXiv 1967

  48. [48]

    Z. Miao, E. Zhou, and A. Li, Astrophys. J.964, 31 (2024), arXiv:2305.08401 [nucl-th]

    Pith/arXiv arXiv 2024

  49. [49]

    J. P. Pereira, L. Tonetto, M. Bejger, J. L. Zdunik, and P. Haensel, Phys. Rev. Lett.135, 231401 (2025), arXiv:2504.16911 [astro-ph.HE]

    arXiv 2025

  50. [50]

    Tak´ atsy, L

    J. Tak´ atsy, L. Zwick, P. Saini, and J. Samsing, Phys. Rev. D113, 103047 (2026), arXiv:2602.15111 [astro-ph.HE]

    arXiv 2026

  51. [51]

    G. A. Lalazissis, T. Niksic, D. Vretenar, and P. Ring, Phys. Rev. C71, 024312 (2005)

    2005

  52. [52]

    C.-J. Xia, T. Maruyama, A. Li, B. Y. Sun, W.-H. Long, and Y.-X. Zhang, Commun. Theor. Phys.74, 095303 (2022), arXiv:2208.12893 [nucl-th]. 20

    Pith/arXiv arXiv 2022

  53. [53]

    V. B. Thapa, A. Kumar, and M. Sinha, Mon. Not. Roy. Astron. Soc.507, 2991 (2021), arXiv:2108.04318 [astro- ph.HE]

    Pith/arXiv arXiv 2021

  54. [54]

    I. A. Rather, K. D. Marquez, P. Thakur, and O. Louren¸ co, Phys. Rev. D112, 023013 (2025), arXiv:2412.12002 [astro- ph.HE]

    Pith/arXiv arXiv 2025