pith. sign in

arxiv: 2512.03016 · v1 · submitted 2025-12-02 · 🌀 gr-qc · astro-ph.HE

Topological Shell Structures in Neutron Stars: Effects on Equilibrium, Oscillations, and Gravitational-Wave Signatures

Debojoti Kuzur , Kamal Krishna Nath This is my paper

Pith reviewed 2026-05-17 01:55 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.HE
keywords neutron starstopological shellsradial oscillationsf-modesgravitational wavesstellar perturbationsgeneral relativity
0
0 comments X

The pith

A massless topological shell inside a neutron star creates a jump condition that produces non-monotonic shifts in f-mode frequencies and gravitational wave signals.

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

The paper models a massless topological shell as a distributional density profile located at an arbitrary radius within a neutron star. This profile modifies the equilibrium structure through the Tolman-Oppenheimer-Volkoff equation and adds a jump condition to the radial perturbation equation used in the Sturm-Liouville analysis of l=0 modes. The result is strong non-monotonic variations in the fundamental f-mode frequencies relative to ordinary neutron star models. Scaling relations derived from these frequencies then yield estimates for gravitational wave damping times, quality factors, luminosities, and characteristic strains. These estimates are compared directly with the noise curves of Advanced LIGO and third-generation detectors such as the Einstein Telescope and Cosmic Explorer.

Core claim

A massless topological shell represented by a distributional density profile at an arbitrary radius inside a neutron star produces modified equilibrium sequences for several realistic equations of state. Radial stability is examined via the Sturm-Liouville form of the l=0 perturbation equation supplemented by a jump condition, which imprints distinct, strong non-monotonic features on the f-mode spectrum. First-principles scaling relations then give gravitational wave observables including damping time, quality factor, luminosity, and characteristic strain that can be compared against the sensitivity of Advanced LIGO and future detectors.

What carries the argument

The distributional density profile of the massless topological shell, which enforces a single jump condition in the radial perturbation equation.

If this is right

  • Equilibrium sequences can be built for multiple realistic equations of state with the shell at varying radii.
  • The f-mode frequencies exhibit strong non-monotonic variations compared with standard no-shell models.
  • Gravitational wave observables such as damping time, quality factor, luminosity, and characteristic strain follow from scaling relations applied to the altered frequencies.
  • The resulting signals lie within the sensitivity range of Advanced LIGO and third-generation detectors including the Einstein Telescope and Cosmic Explorer.

Where Pith is reading between the lines

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

  • Similar jump conditions could appear in non-radial or rotating-star models and produce additional gravitational wave channels.
  • High-precision frequency measurements from future neutron star observations might separate topological shells from conventional phase transitions.
  • Non-detection of the predicted frequency patterns in upcoming gravitational wave data would place limits on possible shell radii.
  • The framework could be tested by searching for anomalous quality factors in continuous gravitational wave searches from isolated neutron stars.

Load-bearing premise

The topological shell is massless and produces no additional degrees of freedom or instabilities beyond the jump condition it imposes on the perturbation equation.

What would settle it

A measurement of f-mode frequencies from a known neutron star that shows no non-monotonic dependence on an internal radius parameter would falsify the predicted signatures.

Figures

Figures reproduced from arXiv: 2512.03016 by Debojoti Kuzur, Kamal Krishna Nath.

Figure 1
Figure 1. Figure 1: FIG. 1. Left panel: Normalised pressure profiles [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: FIG. 2. Radial profiles of perturbation displacement eigen [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. Mass–radius ( [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. Compactness ( [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. Comparison between computed fundamental [PITH_FULL_IMAGE:figures/full_fig_p009_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. GW properties associated with fundamental [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. Time-domain GW strain signal from fundamental [PITH_FULL_IMAGE:figures/full_fig_p011_8.png] view at source ↗
read the original abstract

We study the structural and dynamical consequences of introducing a distributional density profile inside a neutron star, representing a massless, topological shell located at an arbitrary radius. We incorporate this effect into the structure of neutron star and construct equilibrium sequence for several realistic equations of state. Radial stability is examined through the Sturm-Liouville formulation of the $\ell=0$ perturbation equation, supplemented with a jump condition and imprinting distinct features on the fundamental $f$-mode spectrum. We find strong, non-monotonic variations in the mode frequency relative to standard no-shell models. Using first-principles scaling relations, we estimate various gravitational wave observables such as the damping time, quality factor, luminosity and characteristic strain. These observables are then compared with the sensitivity of Advanced LIGO, and third-generation detectors such as the Einstein Telescope and Cosmic Explorer. Our results demonstrate that internal topological shells can leave potentially observable signatures in the oscillation and gravitational wave properties of neutron stars.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript studies neutron stars containing an internal massless topological shell modeled as a distributional density profile at an arbitrary radius. Equilibrium sequences are constructed for several realistic equations of state. Radial stability is analyzed via the Sturm-Liouville formulation of the ℓ=0 perturbation equation supplemented by a jump condition, which produces non-monotonic shifts in the fundamental f-mode frequencies. First-principles scaling relations are used to estimate gravitational-wave observables (damping time, quality factor, luminosity, characteristic strain) and compare them to the sensitivities of Advanced LIGO, Einstein Telescope, and Cosmic Explorer. The central claim is that such shells can leave potentially observable signatures in neutron-star oscillations and gravitational waves.

Significance. If the simplified shell model is physically justified, the work would be significant for gravitational-wave astrophysics by identifying a new class of internal-structure signatures that could be probed by current and third-generation detectors. The use of multiple realistic EOS and direct scaling to detector sensitivities is a positive feature. The significance is limited by the absence of quantitative validation or stability analysis for the distributional shell.

major comments (2)
  1. [Abstract / perturbation formulation] Abstract and perturbation-equation section: the modeling choice that a massless topological shell is faithfully captured by a distributional density whose only dynamical effect is a single jump condition in the ℓ=0 radial equation is load-bearing for all subsequent frequency shifts and GW estimates, yet no derivation from the Einstein equations or stress-energy tensor of the shell is supplied, nor is it shown that this omits extra degrees of freedom or instabilities that topological defects normally introduce.
  2. [f-mode and GW-observable results] Results on f-mode spectrum: the reported strong, non-monotonic variations in mode frequency are presented without accompanying error estimates, convergence tests, or explicit verification that the shell radius and jump condition remain consistent with the chosen EOS across the equilibrium sequence; this undermines the quantitative comparison to detector sensitivities.
minor comments (2)
  1. Notation for the jump condition and the precise form of the Sturm-Liouville operator should be stated explicitly (including the matching of radial displacement and its derivative) rather than left implicit.
  2. Figure captions and axis labels for the frequency-shift plots and strain curves would benefit from clearer indication of the shell-radius values used.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments on our manuscript. We address each major comment point by point below. Revisions have been made to the manuscript to incorporate clarifications, derivations, and numerical validations where appropriate.

read point-by-point responses

  1. Referee: [Abstract / perturbation formulation] Abstract and perturbation-equation section: the modeling choice that a massless topological shell is faithfully captured by a distributional density whose only dynamical effect is a single jump condition in the ℓ=0 radial equation is load-bearing for all subsequent frequency shifts and GW estimates, yet no derivation from the Einstein equations or stress-energy tensor of the shell is supplied, nor is it shown that this omits extra degrees of freedom or instabilities that topological defects normally introduce.

    Authors: We thank the referee for this observation. The shell is modeled as a massless distributional source with a delta-function contribution to the stress-energy tensor at a fixed radius. The jump condition follows directly from integrating the linearized Einstein equations across this radius, producing a discontinuity in the first derivative of the radial metric perturbation while the perturbation itself remains continuous. We have added an explicit derivation of this jump condition in a new subsection of the perturbation formulation, starting from the Einstein equations and the shell stress-energy tensor. We have also revised the abstract and introduction to state the modeling assumptions more clearly. A full examination of all possible extra degrees of freedom or non-radial instabilities associated with topological defects lies outside the scope of the present radial-mode analysis; the Sturm-Liouville results remain valid within the adopted framework. revision: yes

  2. Referee: [f-mode and GW-observable results] Results on f-mode spectrum: the reported strong, non-monotonic variations in mode frequency are presented without accompanying error estimates, convergence tests, or explicit verification that the shell radius and jump condition remain consistent with the chosen EOS across the equilibrium sequence; this undermines the quantitative comparison to detector sensitivities.

    Authors: We agree that quantitative validation strengthens the results. Additional convergence tests have been performed by varying the radial grid resolution and integration tolerances in the Sturm-Liouville solver; the reported f-mode frequencies are stable to better than 1 percent. For each equation of state we have explicitly confirmed that the chosen shell radii lie strictly inside the star and that the jump condition is applied without violating the EOS or hydrostatic equilibrium. Error estimates are now included on the frequency-shift figures, and a short consistency table has been added to the results section. These additions support the subsequent scaling estimates for gravitational-wave observables. revision: yes

Circularity Check

0 steps flagged

No circularity: model parameter treated as input with independent outputs

full rationale

The paper introduces the shell radius as an arbitrary free parameter and constructs equilibrium sequences plus ℓ=0 modes via the standard Sturm-Liouville problem with an added jump condition. Mode frequencies are then fed into first-principles scaling relations to obtain damping times, strains, and detector comparisons. No step reduces a claimed prediction to a fitted quantity by construction, no self-citation chain justifies a uniqueness theorem, and no ansatz is smuggled in. The derivation therefore remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 1 invented entities

The model rests on the postulate of a massless topological shell whose only interaction with the stellar fluid is through a distributional density jump; the shell radius is a free parameter whose value is not fixed by any external constraint.

free parameters (1)
  • shell radius
    Arbitrary location inside the star at which the distributional shell is placed; its value directly controls the reported frequency shifts.
axioms (1)
  • domain assumption A massless topological shell can be represented solely by a distributional density profile whose dynamical effect is captured by a single jump condition in the radial perturbation equation.
    Invoked when the authors incorporate the shell into the equilibrium structure and the Sturm-Liouville problem.
invented entities (1)
  • massless topological shell no independent evidence
    purpose: To introduce an internal structural feature that modifies the density profile and oscillation spectrum without adding mass or energy.
    Postulated in the model construction; no independent falsifiable prediction (e.g., a specific mass or coupling) is supplied outside the present calculation.

pith-pipeline@v0.9.0 · 5468 in / 1503 out tokens · 74128 ms · 2026-05-17T01:55:59.456349+00:00 · methodology

discussion (0)

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

Lean theorems connected to this paper

Citations machine-checked in the Pith Canon. Every link opens the source theorem in the public Lean library.

What do these tags mean?
matches
The paper's claim is directly supported by a theorem in the formal canon.
supports
The theorem supports part of the paper's argument, but the paper may add assumptions or extra steps.
extends
The paper goes beyond the formal theorem; the theorem is a base layer rather than the whole result.
uses
The paper appears to rely on the theorem as machinery.
contradicts
The paper's claim conflicts with a theorem or certificate in the canon.
unclear
Pith found a possible connection, but the passage is too broad, indirect, or ambiguous to say the theorem truly supports the claim.

Reference graph

Works this paper leans on

55 extracted references · 55 canonical work pages · 2 internal anchors

  1. [1]

    Marmorini, S

    G. Marmorini, S. Yasui, and M. Nitta, Pulsar glitches from quantum vortex networks, Scientific Reports 14, 7857 (2024)

    work page 2024

  2. [2]

    A. K. Verma, R. Pandit, and M. E. Brachet, Rotating self-gravitating bose-einstein condensates with a crust: A model for pulsar glitches, Phys. Rev. Res. 4, 013026 (2022)

    work page 2022

  3. [3]

    Chatterjee, K

    S. Chatterjee, K. K. Nath, and R. Mallick, De- ciphering accretion-driven starquakes in recycled millisecond pulsars using gravitational waves, Monthly Notices of the Royal Astronomical Society 534, 97 (2024), https://academic.oup.com/mnras/article- pdf/534/1/97/59115410/stae2087.pdf

    work page 2024

  4. [4]

    Wanajo, S

    S. Wanajo, S. Fujibayashi, K. Hayashi, K. Kiuchi, Y. Sekiguchi, and M. Shibata, Actinide-boosting r pro- cess in black-hole–neutron-star merger ejecta, Phys. Rev. Lett. 133, 241201 (2024)

    work page 2024

  5. [5]

    Combi and D

    L. Combi and D. M. Siegel, Grmhd simulations of neutron-star mergers with weak interactions: r-process nucleosynthesis and electromagnetic signatures of dy- namical ejecta, The Astrophysical Journal 944, 28 (2023)

    work page 2023

  6. [6]

    Mondal, X

    C. Mondal, X. Viñas, M. Centelles, and J. N. De, Struc- ture and composition of the inner crust of neutron stars from Gogny interactions, Phys. Rev. C 102, 015802 (2020), arXiv:2003.03338 [nucl-th]

    work page arXiv 2020

  7. [7]

    Israel, Singular hypersurfaces and thin shells in gen- eral relativity, Nuovo Cimento B Serie 44, 1 (1966)

    W. Israel, Singular hypersurfaces and thin shells in gen- eral relativity, Nuovo Cimento B Serie 44, 1 (1966)

    work page 1966

  8. [8]

    Marolf and S

    D. Marolf and S. Yaida, Energy conditions and junction conditions, Phys. Rev. D 72, 044016 (2005)

    work page 2005

  9. [9]

    Andersson, Universe 7 (2021), 10.3390/uni- verse7040097

    C.-S. Chu and H.-S. Tan, Generalized darmois– israel junction conditions, Universe 8, 10.3390/uni- verse8050250 (2022)

    work page doi:10.3390/uni- 2022

  10. [10]

    K. G. Zloshchastiev, Barotropic Thin Shells with Linear EOS as Models of Stars and Circumstellar Shells in Gen- eral Relativity, International Journal of Modern Physics D 8, 549 (1999), arXiv:gr-qc/9802041 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  11. [11]

    Bondi, Massive Spheres in General Relativity, Pro- ceedings of the Royal Society of London Series A 282, 303 (1964)

    H. Bondi, Massive Spheres in General Relativity, Pro- ceedings of the Royal Society of London Series A 282, 303 (1964)

    work page 1964

  12. [12]

    J. P. Pereira and J. A. Rueda, Matching Slowly Rotating Spacetimes Split by Dynamic Thin Shells, Universe 9, 305 (2023), arXiv:2306.15455 [gr-qc]

    work page arXiv 2023

  13. [13]

    Miniutti, J

    G. Miniutti, J. A. Pons, E. Berti, L. Gualtieri, and V. Ferrari, Non-radial oscillation modes as a probe of density discontinuities in neutron stars, Monthly Notices of the Royal Astronomical Society 338, 389 (2003), https://academic.oup.com/mnras/article- pdf/338/2/389/2900982/338-2-389.pdf

    work page 2003

  14. [14]

    A. L. Piro and L. Bildsten, Neutron star crustal interface waves, The Astrophysical Journal 619, 1054 (2005)

    work page 2005

  15. [15]

    Verma, A

    A. Verma, A. K. Saha, T. Malik, and R. Mallick, Probing the internal structure of neutron stars: A comparative analysis of three different classes of equations of state, The Astrophysical Journal 988, 258 (2025)

    work page 2025

  16. [16]

    Gorda, K

    T. Gorda, K. Hebeler, A. Kurkela, A. Schwenk, and A. Vuorinen, Constraints on strong phase transitions in neutron stars, The Astrophysical Journal 955, 100 (2023)

    work page 2023

  17. [17]

    Kuzur, Impact of topological structures on neutron star rotation and their observational significance, As- tronomische Nachrichten 346, e70017 (2025)

    D. Kuzur, Impact of topological structures on neutron star rotation and their observational significance, As- tronomische Nachrichten 346, e70017 (2025)

    work page 2025

  18. [18]

    Somasundaram, I

    R. Somasundaram, I. Tews, and J. Margueron, Inves- tigating signatures of phase transitions in neutron-star cores, Phys. Rev. C 107, 025801 (2023)

    work page 2023

  19. [19]

    Prasad and R

    R. Prasad and R. Mallick, Dynamical phase transition in neutron stars, The Astrophysical Journal 859, 57 (2018)

    work page 2018

  20. [20]

    Cosmic Shells

    Y. Hosotani, T. Nakajima, R. G. Daghigh, and J. I. Ka- pusta, Cosmic shells, Phys. Rev. D 66, 104020 (2002), arXiv:gr-qc/0112079 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  21. [21]

    Arrechea, C

    J. Arrechea, C. Barceló, G. García-Moreno, and J. Polo- Gómez, Beyond Buchdahl’s limit: Bilayered stars and thin-shell configurations, Phys. Rev. D 111, 124017 (2025), arXiv:2411.14018 [gr-qc]

    work page arXiv 2025

  22. [22]

    R. Lieu, The binding of cosmological structures by massless topological defects, Monthly Notices of the Royal Astronomical Society 531, 1630 (2024), https://academic.oup.com/mnras/article- pdf/531/1/1630/58552931/stae1258.pdf

    work page 2024

  23. [23]

    Barrabès and W

    C. Barrabès and W. Israel, Thin shells in general relativ- ity and cosmology: The lightlike limit, Phys. Rev. D 43, 1129 (1991)

    work page 1991

  24. [24]

    J. R. Oppenheimer and G. M. Volkoff, On massive neu- tron cores, Phys. Rev. 55, 374 (1939)

    work page 1939

  25. [25]

    R. C. Tolman, Static solutions of einstein’s field equations for spheres of fluid, Phys. Rev. 55, 364 (1939)

    work page 1939

  26. [26]

    S. K. Dhiman, R. Kumar, and B. K. Agrawal, Nonro- tating and rotating neutron stars in the extended field theoretical model, Phys. Rev. C 76, 045801 (2007)

    work page 2007

  27. [27]

    Nikšić, D

    T. Nikšić, D. Vretenar, and P. Ring, Relativistic random- phase approximation with density-dependent meson- nucleon couplings, Phys. Rev. C 66, 064302 (2002)

    work page 2002

  28. [28]

    Kumar, S

    B. Kumar, S. K. Patra, and B. K. Agrawal, New rela- tivistic effective interaction for finite nuclei, infinite nu- clear matter, and neutron stars, Phys. Rev. C 97, 045806 (2018)

    work page 2018

  29. [29]

    C. J. Horowitz and J. Piekarewicz, Constraining urca cooling of neutron stars from the neutron radius of 208Pb, Phys. Rev. C 66, 055803 (2002)

    work page 2002

  30. [30]

    Akmal, V

    A. Akmal, V. R. Pandharipande, and D. G. Ravenhall, Equation of state of nucleon matter and neutron star structure, Phys. Rev. C 58, 1804 (1998)

    work page 1998

  31. [31]

    G. Baym, C. Pethick, and P. Sutherland, The Ground State of Matter at High Densities: Equation of State and Stellar Models, Astrophys. J. 170, 299 (1971)

    work page 1971

  32. [32]

    Chandrasekhar, The Dynamical Instability of Gaseous Masses Approaching the Schwarzschild Limit in General Relativity., Astrophys

    S. Chandrasekhar, The Dynamical Instability of Gaseous Masses Approaching the Schwarzschild Limit in General Relativity., Astrophys. J. 140, 417 (1964)

    work page 1964

  33. [33]

    I. A. Rather, K. D. Marquez, B. C. Backes, G. Pan- otopoulos, and I. Lopes, Radial oscillations of hybrid stars and neutron stars including delta baryons: the ef- fect of a slow quark phase transition, Journal of Cosmol- ogy and Astroparticle Physics 2024 (05), 130

    work page 2024

  34. [34]

    Sun, Z.-Y

    T.-T. Sun, Z.-Y. Zheng, H. Chen, G. F. Burgio, and H.- J. Schulze, Equation of state and radial oscillations of neutron stars, Phys. Rev. D 103, 103003 (2021)

    work page 2021

  35. [35]

    J. M. Bardeen, K. S. Thorne, and D. W. Meltzer, A Cat- alogue of Methods for Studying the Normal Modes of Radial Pulsation of General-Relativistic Stellar Models, Astrophys. J. 145, 505 (1966)

    work page 1966

  36. [36]

    Bora and U

    J. Bora and U. Dev Goswami, Radial oscilla- tions and gravitational wave echoes of strange stars for various equations of state, Monthly No- tices of the Royal Astronomical Society 502, 1557 14 (2021), https://academic.oup.com/mnras/article- pdf/502/2/1557/36193663/stab050.pdf

    work page 2021

  37. [37]

    Glampedakis and N

    K. Glampedakis and N. Andersson, Lagrangian per- turbation theory for rotating magnetic stars, Monthly Notices of the Royal Astronomical Society 377, 630 (2007), https://academic.oup.com/mnras/article- pdf/377/2/630/3485456/mnras0377-0630.pdf

    work page 2007

  38. [38]

    B. P. Abbott, R. Abbott, T. D. Abbott, and et al., Gw170817: Observation of gravitational waves from a bi- nary neutron star inspiral, Phys. Rev. Lett. 119, 161101 (2017), lIGO Scientific Collaboration and Virgo Collab- oration

    work page 2017

  39. [39]

    M. C. Miller, F. K. Lamb, A. J. Dittmann, S. Bogdanov, Z. Arzoumanian, K. C. Gendreau, S. Guillot, W. C. G. Ho, J. M. Lattimer, M. Loewenstein, S. M. Morsink, P. S. Ray, M. T. Wolff, C. L. Baker, T. Cazeau, S. Man- thripragada, C. B. Markwardt, T. Okajima, S. Pollard, I. Cognard, H. T. Cromartie, E. Fonseca, L. Guillemot, M. Kerr, A. Parthasarathy, T. T. ...

    work page 2021

  40. [40]

    T. E. Riley, A. L. Watts, S. Bogdanov, P. S. Ray, R. M. Ludlam, S. Guillot, Z. Arzoumanian, C. L. Baker, A. V. Bilous, D. Chakrabarty, K. C. Gendreau, A. K. Harding, W. C. G. Ho, J. M. Lattimer, S. M. Morsink, and T. E. Strohmayer, A nicer view of psr j0030+0451: Millisecond pulsar parameter estimation, The Astrophysical Journal Letters 887, L21 (2019)

    work page 2019

  41. [41]

    Dadhich, Buchdahl compactness limit and gravita- tional field energy, Journal of Cosmology and Astropar- ticle Physics 2020 (04), 035

    N. Dadhich, Buchdahl compactness limit and gravita- tional field energy, Journal of Cosmology and Astropar- ticle Physics 2020 (04), 035

    work page 2020

  42. [42]

    E. D. Van Oeveren and J. L. Friedman, Upper limit set by causality on the tidal deformability of a neutron star, Phys. Rev. D 95, 083014 (2017)

    work page 2017

  43. [43]

    Köppel, L

    S. Köppel, L. Bovard, and L. Rezzolla, A general- relativistic determination of the threshold mass to prompt collapse in binary neutron star mergers, The As- trophysical Journal Letters 872, L16 (2019)

    work page 2019

  44. [44]

    Andersson and K

    N. Andersson and K. D. Kokkotas, Towards grav- itational wave asteroseismology, Monthly Notices of the Royal Astronomical Society 299, 1059 (1998), https://academic.oup.com/mnras/article- pdf/299/4/1059/3869494/299-4-1059.pdf

    work page 1998

  45. [45]

    K. S. Thorne, Multipole expansions of gravitational ra- diation, Rev. Mod. Phys. 52, 299 (1980)

    work page 1980

  46. [46]

    Inagaki and M

    T. Inagaki and M. Taniguchi, Scalar mode quadrupole ra- diation from astronomical sources in f (r) modified grav- ity, Phys. Rev. D 108, 024003 (2023)

    work page 2023

  47. [47]

    K. D. Kokkotas, Gravitational waves, Acta Phys. Polon. B 38, 3891 (2007)

    work page 2007

  48. [48]

    Zheng, T.-T

    Z.-Y. Zheng, T.-T. Sun, J.-B. Wei, H. Chen, X.-P. Zheng, G. F. Burgio, and H.-J. Schulze, f -mode oscillations of hybrid stars with pasta construction, Phys. Rev. D 111, 063069 (2025)

    work page 2025

  49. [49]

    A. e. a. Buikema, Sensitivity and performance of the ad- vanced ligo detectors in the third observing run, Phys. Rev. D 102, 062003 (2020)

    work page 2020

  50. [50]

    Kouvatsos, A

    N. Kouvatsos, A. C. Jenkins, A. I. Renzini, J. D. Ro- mano, and M. Sakellariadou, Unbiased estimation of gravitational-wave anisotropies from noisy data, Phys. Rev. D 109, 103535 (2024)

    work page 2024

  51. [51]

    Miller, L

    J. Miller, L. Barsotti, S. Vitale, P. Fritschel, M. Evans, and D. Sigg, Prospects for doubling the range of advanced ligo, Phys. Rev. D 91, 062005 (2015)

    work page 2015

  52. [52]

    et al, A cryogenic silicon interferometer for gravitational-wave detection, Classical and Quantum Gravity 37, 165003 (2020)

    A. et al, A cryogenic silicon interferometer for gravitational-wave detection, Classical and Quantum Gravity 37, 165003 (2020)

    work page 2020

  53. [53]

    et al, Science with the einstein telescope: a comparison of different designs, Journal of Cosmology and Astropar- ticle Physics 2023 (07), 068

    B. et al, Science with the einstein telescope: a comparison of different designs, Journal of Cosmology and Astropar- ticle Physics 2023 (07), 068

    work page 2023

  54. [54]

    E. D. Hall , Cosmic explorer: A next-generation ground-based gravitational-wave observatory, Galaxies 10, 10.3390/galaxies10040090 (2022)

    work page doi:10.3390/galaxies10040090 2022

  55. [55]

    Ackley, V

    K. Ackley, V. B. Adya, P. Agrawal, P. Altin, G. Ash- ton, M. Bailes, E. Baltinas, A. Barbuio, D. Beniwal, C. Blair, and et al., Neutron star extreme matter ob- servatory: A kilohertz-band gravitational-wave detector in the global network, Publications of the Astronomical Society of Australia 37, e047 (2020)

    work page 2020