pith. sign in

arxiv: 2605.22944 · v1 · pith:QVA7S3RGnew · submitted 2026-05-21 · 🌌 astro-ph.CO · hep-th

Gravitational waves from cosmic strings with friction: analytical approximations and parameter space

Sergei Mukovnikov , Lara Sousa This is my paper

Pith reviewed 2026-05-25 05:35 UTC · model grok-4.3

classification 🌌 astro-ph.CO hep-th
keywords cosmic stringsgravitational wavesfriction erastochastic backgroundanalytical approximationsultra-high-frequency peakparameter space
0
0 comments X

The pith

Analytical approximations describe the ultra-high-frequency gravitational wave peak from cosmic string loops formed in the friction era.

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

The paper derives analytical approximations for the secondary peak in the stochastic gravitational wave background produced by cosmic strings. These approximations target the contribution from loops formed during the friction-dominated era. A sympathetic reader would care because they allow quick and accurate modeling of this signature across many string parameters without full numerical simulations. The work also maps out the parameter space where this peak stands out from other contributions and shows the signature appears in more high-energy scenarios than first thought.

Core claim

We derive analytical approximations to describe the ultra-high-frequency secondary peak of the stochastic gravitational wave background generated by cosmic strings that is sourced by loops created in the friction-dominated era. We show that these approximations provide a very good description of the contribution of the friction-era loops over the relevant frequency range and for a broad range of cosmic string parameters, thus enabling a fast and accurate characterization of this signature. We also use these approximations to uncover the full parameter range in which this ultra-high-frequency peak should be distinguishable on the stochastic gravitational wave background spectrum and show that

What carries the argument

Analytical approximations for the gravitational-wave spectrum contribution from loops created during the friction-dominated era of cosmic string evolution.

If this is right

  • The approximations enable fast and accurate characterization of the ultra-high-frequency signature without repeated full simulations.
  • The peak remains distinguishable from other era contributions over the full uncovered parameter range.
  • The signature appears in a broader set of high-energy physics scenarios than first reported.
  • The forms hold for a wide range of cosmic string parameters.

Where Pith is reading between the lines

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

  • Detectors aimed at ultra-high frequencies could apply these closed forms to place tighter bounds on string parameters with less computation.
  • The same separation technique for isolated era contributions could extend to other transient phases in string network evolution.
  • Models of early-universe friction on topological defects beyond the original scenarios now become testable with the same peak signature.

Load-bearing premise

The friction-dominated era produces a distinct population of loops whose gravitational-wave contribution forms an isolated ultra-high-frequency peak that can be separated from radiation-era and matter-era contributions.

What would settle it

Direct numerical evaluation of the full stochastic gravitational wave spectrum for several values of string tension and friction strength, verifying whether the analytical peak height, width, and frequency location match the computed contribution from friction-era loops to within a few percent across the relevant band.

Figures

Figures reproduced from arXiv: 2605.22944 by Lara Sousa, Sergei Mukovnikov.

Figure 1
Figure 1. Figure 1: Evolution of a cosmic string network during the [PITH_FULL_IMAGE:figures/full_fig_p003_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: The Stochastic Gravitational Wave Background [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Analytical approximation to the SGWB generated [PITH_FULL_IMAGE:figures/full_fig_p008_3.png] view at source ↗
Figure 5
Figure 5. Figure 5: Analytical approximation to the SGWB generated [PITH_FULL_IMAGE:figures/full_fig_p009_5.png] view at source ↗
Figure 7
Figure 7. Figure 7: Analytical approximation to the SGWB gener [PITH_FULL_IMAGE:figures/full_fig_p010_7.png] view at source ↗
Figure 9
Figure 9. Figure 9: Parameter space in which there is a distinguishable signature of friction in the ultra-high frequency range of the [PITH_FULL_IMAGE:figures/full_fig_p013_9.png] view at source ↗
Figure 10
Figure 10. Figure 10: Analytical approximation to the SGWB generated [PITH_FULL_IMAGE:figures/full_fig_p014_10.png] view at source ↗
read the original abstract

We derive analytical approximations to describe the ultra-high-frequency secondary peak of the stochastic gravitational wave background generated by cosmic strings that is sourced by loops created in the friction-dominated era. We show that these approximations provide a very good description of the contribution of the friction-era loops over the relevant frequency range and for a broad range of cosmic string parameters, thus enabling a fast and accurate characterization of this signature. We also use these approximations to uncover the full parameter range in which this ultra-high-frequency peak should be distinguishable on the stochastic gravitational wave background spectrum and show that it should be present in a broader range of high-energy physics scenarios than originally reported in~\cite{Mukovnikov:2024zed}.

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

0 major / 3 minor

Summary. The paper derives analytical approximations for the ultra-high-frequency secondary peak in the stochastic gravitational wave background sourced by cosmic string loops formed in the friction-dominated era. It claims these forms accurately capture the friction-era contribution over relevant frequencies for a broad range of string parameters (tension and friction coefficient), enabling rapid characterization, and maps an expanded region of parameter space where the peak is distinguishable from radiation- and matter-era contributions, exceeding the range reported in Mukovnikov:2024zed.

Significance. If the approximations hold, the work supplies a practical, fast analytical tool for isolating and characterizing a distinct GW signature from friction-era loops, which could extend the set of high-energy physics models testable via stochastic GW backgrounds. The explicit mapping of the distinguishable parameter region and the claim of broader applicability constitute the main advance.

minor comments (3)
  1. The abstract states that the approximations 'provide a very good description' but the manuscript should include explicit quantitative metrics (e.g., maximum relative error or R² values) for the comparison against numerical spectra in the relevant frequency window; this would strengthen the validation claim.
  2. Notation for the friction coefficient and the transition times between eras should be defined once in §2 and used consistently; occasional redefinition in later sections risks confusion when readers compare the analytical forms to the underlying loop-production model.
  3. Figure captions for the spectra plots should explicitly state the frequency range over which the friction-era peak is isolated and the parameter values used, to allow direct visual assessment of the claimed separation from other eras.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for the positive assessment of our manuscript, the accurate summary of its contributions, and the recommendation for minor revision. We are pleased that the work is viewed as providing a practical analytical tool and an expanded parameter space mapping.

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper states that it derives analytical approximations for the ultra-high-frequency secondary peak sourced by friction-era loops, then validates that these forms describe the contribution well over the relevant frequency range and broad parameter space. The extension to a broader range of scenarios than in the self-cited prior work follows from applying the new approximations rather than from any reduction of the central result to a fit, self-definition, or load-bearing self-citation. No quoted equation or step equates a claimed prediction to its own input by construction, and the derivation is presented as independent of the cited reference.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The work rests on standard cosmic-string network evolution assumptions and the existence of a distinct friction era; no new entities are introduced.

free parameters (2)
  • cosmic string tension
    Standard model parameter varied across ranges; value not fixed by the paper.
  • friction coefficient
    Parameter controlling loop formation in the friction era; varied but not derived from first principles.
axioms (1)
  • domain assumption Cosmic string loops formed in the friction-dominated era produce a separable ultra-high-frequency gravitational-wave peak
    Core modeling premise invoked to isolate the secondary peak.

pith-pipeline@v0.9.0 · 5637 in / 1084 out tokens · 21370 ms · 2026-05-25T05:35:05.475262+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

60 extracted references · 60 canonical work pages · 15 internal anchors

  1. [1]

    Small loops When validating the approximation for small loops, for each set of parameters, the largest value ofαcon- sidered wasα= 0.1ΓGµ(represented by the orange line in Fig. 3). We then gradually decreased loop size un- til the signature disappeared completely. This behavior is inevitable since, when we decreaseα, we necessarily encounter the cut-offαL...

    work page

  2. [2]

    (43) — represented by the dashed lines in Figs

    Backreaction and larger loops To validate the approximation for loops created with sizes comparable to the gravitational backreaction scale in Eq. (43) — represented by the dashed lines in Figs. 6 - 8 — we started by considering loops withα= ΓGµ(the red lines in Figs. 6 - 8). We then moved to larger loops until the signature becomes smaller than the frict...

    work page

  3. [3]

    For this reason, in App

    Transitional regime Although, the two approximations derived here pro- vide a good approximation to the SGWB generated by loops during the friction era for a wide range of param- eters, we found a range of values ofαin which they are not so accurate. For this reason, in App. B, we derive a third analytical approximation. The starting point is the approxim...

    work page doi:10.54499/ui/bd/152220/2021 2021

  4. [4]

    Mukovnikov and L

    S. Mukovnikov and L. Sousa, Ultrahigh frequency gravi- tational waves from cosmic strings with friction, Phys. Rev. D110, 063516 (2024), arXiv:2404.13213 [astro- ph.CO]

    work page arXiv 2024

  5. [5]

    Aggarwalet al., Challenges and opportunities of gravitational-wave searches at MHz to GHz frequencies, Living Rev

    N. Aggarwalet al., Challenges and opportunities of gravitational-wave searches at MHz to GHz frequencies, Living Rev. Rel.24, 4 (2021), arXiv:2011.12414 [gr-qc]

    work page arXiv 2021

  6. [6]

    Aggarwalet al., Challenges and opportunities of 15 gravitational-wave searches above 10 kHz, Living Rev

    N. Aggarwalet al., Challenges and opportunities of 15 gravitational-wave searches above 10 kHz, Living Rev. Rel.28, 10 (2025), arXiv:2501.11723 [gr-qc]

    work page arXiv 2025

  7. [7]

    M. B. Hindmarsh and T. W. B. Kibble, Cosmic strings, Reports on Progress in Physics58, 477 (1995)

    work page 1995

  8. [8]

    Vilenkin and E

    A. Vilenkin and E. P. S. Shellard,Cosmic Strings and Other Topological Defects(Cambridge University Press, 2000)

    work page 2000

  9. [9]

    Witten, Superconducting Strings, Nucl

    E. Witten, Superconducting Strings, Nucl. Phys. B249, 557 (1985)

    work page 1985

  10. [10]

    How generic is cosmic string formation in SUSY GUTs

    R. Jeannerot, J. Rocher, and M. Sakellariadou, How generic is cosmic string formation in SUSY GUTs, Phys. Rev. D68, 103514 (2003), arXiv:hep-ph/0308134

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  11. [11]

    Cosmic String Production Towards the End of Brane Inflation

    S. Sarangi and S. H. H. Tye, Cosmic string production towards the end of brane inflation, Phys. Lett. B536, 185 (2002), arXiv:hep-th/0204074

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  12. [12]

    Vilenkin, Gravitational radiation from cosmic strings, Phys

    A. Vilenkin, Gravitational radiation from cosmic strings, Phys. Lett. B107, 47 (1981)

    work page 1981

  13. [13]

    C. J. Hogan and M. J. Rees, Gravitational interactions of cosmic strings, Nature311, 109 (1984)

    work page 1984

  14. [14]

    F. S. Accetta and L. M. Krauss, The stochastic gravita- tional wave spectrum resulting from cosmic string evolu- tion, Nucl. Phys. B319, 747 (1989)

    work page 1989

  15. [15]

    J. J. Blanco-Pillado, K. D. Olum, and B. Shlaer, The number of cosmic string loops, Phys. Rev. D89, 023512 (2014), arXiv:1309.6637 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  16. [16]

    Stochastic Gravitational Wave Background generated by Cosmic String Networks: Velocity-Dependent One-Scale model versus Scale-Invariant Evolution

    L. Sousa and P. P. Avelino, Stochastic Gravitational Wave Background generated by Cosmic String Net- works: Velocity-Dependent One-Scale model versus Scale-Invariant Evolution, Phys. Rev. D88, 023516 (2013), arXiv:1304.2445 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  17. [17]

    Probing Cosmic Superstrings with Gravitational Waves

    L. Sousa and P. P. Avelino, Probing Cosmic Superstrings with Gravitational Waves, Phys. Rev. D94, 063529 (2016), arXiv:1606.05585 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  18. [18]

    Sousa, P

    L. Sousa, P. P. Avelino, and G. S. F. Guedes, Full ana- lytical approximation to the stochastic gravitational wave background generated by cosmic string networks, Phys. Rev. D101, 103508 (2020), arXiv:2002.01079 [astro- ph.CO]

    work page arXiv 2020

  19. [19]

    Hindmarsh, J

    M. Hindmarsh, J. Lizarraga, A. Urio, and J. Urrestilla, Loop decay in Abelian-Higgs string networks, Phys. Rev. D104, 043519 (2021), arXiv:2103.16248 [astro-ph.CO]

    work page arXiv 2021

  20. [20]

    Buchmuller, V

    W. Buchmuller, V. Domcke, and K. Schmitz, Metastable cosmic strings, JCAP11, 020, arXiv:2307.04691 [hep- ph]

    work page arXiv

  21. [21]

    I. Y. Rybak and L. Sousa, Stochastic gravitational wave background from chiral superconducting cosmic strings, Phys. Rev. D111, 083502 (2025), arXiv:2412.17154 [astro-ph.CO]

    work page arXiv 2025

  22. [22]

    Y. Cui, M. Lewicki, D. E. Morrissey, and J. D. Wells, Probing the pre-BBN universe with gravitational waves from cosmic strings, JHEP01, 081, arXiv:1808.08968 [hep-ph]

    work page internal anchor Pith review Pith/arXiv arXiv

  23. [23]

    Gouttenoire, G

    Y. Gouttenoire, G. Servant, and P. Simakachorn, Beyond the Standard Models with Cosmic Strings, JCAP07, 032, arXiv:1912.02569 [hep-ph]

    work page arXiv 1912

  24. [24]

    Auclairet al., Probing the gravitational wave back- ground from cosmic strings with LISA, JCAP04, 034, arXiv:1909.00819 [astro-ph.CO]

    P. Auclairet al., Probing the gravitational wave back- ground from cosmic strings with LISA, JCAP04, 034, arXiv:1909.00819 [astro-ph.CO]

    work page arXiv 1909

  25. [25]

    J. J. Blanco-Pillado, Y. Cui, S. Kuroyanagi, M. Lewicki, G. Nardini, M. Pieroni, I. Y. Rybak, L. Sousa, and J. M. Wachter (LISA Cosmology Working Group), Gravita- tional waves from cosmic strings in LISA: reconstruc- tion pipeline and physics interpretation, JCAP05, 006, arXiv:2405.03740 [astro-ph.CO]

    work page arXiv

  26. [26]

    Garriga and M

    J. Garriga and M. Sakellariadou, Effects of friction on cosmic strings, Phys. Rev. D48, 2502 (1993), arXiv:hep- th/9303024

    work page arXiv 1993

  27. [27]

    J. Li, M. Li, N. Yang, L. Wang, H. Yu, Y. Huang, K. Lin, Z.-C. Lin, and F. Li, The constraints on the stochastic gravitational wave background from cosmic strings by an electromagnetic resonance system, Eur. Phys. J. C85, 1049 (2025), arXiv:2505.13891 [gr-qc]

    work page arXiv 2025

  28. [28]

    Planck 2018 results. VI. Cosmological parameters

    N. Aghanimet al.(Planck), Planck 2018 results. VI. Cosmological parameters, Astron. Astrophys.641, A6 (2020), [Erratum: Astron.Astrophys. 652, C4 (2021)], arXiv:1807.06209 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  29. [29]

    C. J. A. P. Martins and E. P. S. Shellard, Quantita- tive string evolution, Phys. Rev. D54, 2535 (1996), arXiv:hep-ph/9602271

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  30. [30]

    T. W. B. Kibble, Topology of Cosmic Domains and Strings, J. Phys. A9, 1387 (1976)

    work page 1976

  31. [31]

    E. W. Kolb and M. S. Turner,The Early Universe, Vol. 69 (1990)

    work page 1990

  32. [32]

    Vilenkin, Cosmic string dynamics with friction, Phys

    A. Vilenkin, Cosmic string dynamics with friction, Phys. Rev. D43, 1060 (1991)

    work page 1991

  33. [33]

    M. G. Alford and F. Wilczek, Aharonov-Bohm Interac- tion of Cosmic Strings with Matter, Phys. Rev. Lett.62, 1071 (1989)

    work page 1989

  34. [34]

    C. J. A. P. Martins and E. P. S. Shellard, Extending the velocity dependent one scale string evolution model, Phys. Rev. D65, 043514 (2002), arXiv:hep-ph/0003298

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  35. [35]

    C. J. A. P. Martins, P. Peter, I. Y. Rybak, and E. P. S. Shellard, Generalized velocity-dependent one-scale model for current-carrying strings, Phys. Rev. D103, 043538 (2021), arXiv:2011.09700 [astro-ph.CO]

    work page arXiv 2021

  36. [36]

    T. O. Miranda and L. Sousa, A velocity-dependent two- scale model for cosmic string networks with small-scale structure, (2026), arXiv:2603.23619 [astro-ph.CO]

    work page arXiv 2026

  37. [37]

    Scaling from gauge and scalar radiation in Abelian Higgs string networks

    M. Hindmarsh, J. Lizarraga, J. Urrestilla, D. Daverio, and M. Kunz, Scaling from gauge and scalar radiation in Abelian Higgs string networks, Phys. Rev. D96, 023525 (2017), arXiv:1703.06696 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  38. [38]

    J. J. Blanco-Pillado, D. Jim´ enez-Aguilar, J. M. Queiruga, and J. Urrestilla, The dynamics of domain wall strings, JCAP05, 011, arXiv:2209.12945 [hep-th]

    work page arXiv

  39. [39]

    J. J. Blanco-Pillado, D. Jim´ enez-Aguilar, J. Lizarraga, A. Lopez-Eiguren, K. D. Olum, A. Urio, and J. Ur- restilla, Nambu-Goto dynamics of field theory cosmic string loops, JCAP05, 035, arXiv:2302.03717 [hep-th]

    work page arXiv

  40. [40]

    C. J. Burden, Gravitational Radiation From a Particular Class of Cosmic Strings, Phys. Lett. B164, 277 (1985)

    work page 1985

  41. [41]

    Allen and E

    B. Allen and E. P. S. Shellard, Gravitational radiation from cosmic strings, Phys. Rev. D45, 1898 (1992)

    work page 1992

  42. [42]

    Garfinkle and T

    D. Garfinkle and T. Vachaspati, Fields due to kinky, cus- pless, cosmic loops, Phys. Rev. D37, 257 (1988)

    work page 1988

  43. [43]

    Allen, P

    B. Allen, P. Casper, and A. Ottewill, Analytic results for the gravitational radiation from a class of cosmic string loops, Phys. Rev. D50, 3703 (1994), arXiv:gr- qc/9405037

    work page arXiv 1994

  44. [44]

    Gravitational wave bursts from cosmic strings

    T. Damour and A. Vilenkin, Gravitational wave bursts from cosmic strings, Phys. Rev. Lett.85, 3761 (2000), arXiv:gr-qc/0004075

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  45. [45]

    J. J. Blanco-Pillado, K. D. Olum, and B. Shlaer, Cos- mic string loop shapes, Phys. Rev. D92, 063528 (2015), arXiv:1508.02693 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  46. [46]

    Vachaspati and A

    T. Vachaspati and A. Vilenkin, Gravitational Radiation from Cosmic Strings, Phys. Rev. D31, 3052 (1985)

    work page 1985

  47. [47]

    R. J. Scherrer, J. M. Quashnock, D. N. Spergel, and 16 W. H. Press, Properties of Realistic Cosmic String Loops, Phys. Rev. D42, 1908 (1990)

    work page 1908

  48. [48]

    J. M. Quashnock and D. N. Spergel, Gravitational Self- interactions of Cosmic Strings, Phys. Rev. D42, 2505 (1990)

    work page 1990

  49. [49]

    T. W. B. Kibble, Evolution of a system of cosmic strings, Nucl. Phys. B252, 227 (1985), [Erratum: Nucl.Phys.B 261, 750 (1985)]

    work page 1985

  50. [50]

    S. A. Sanidas, R. A. Battye, and B. W. Stappers, Con- straints on cosmic string tension imposed by the limit on the stochastic gravitational wave background from the European Pulsar Timing Array, Phys. Rev. D85, 122003 (2012), arXiv:1201.2419 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  51. [51]

    Planck Collaboration XXV, Planck 2013 results. XXV. Searches for cosmic strings and other topological defects, Astron. Astrophys. 571, A25 (2014)

    work page 2013

  52. [52]

    The Stochastic Gravitational Wave Background Generated by Cosmic String Networks: the Small-Loop Regime

    L. Sousa and P. P. Avelino, Stochastic gravitational wave background generated by cosmic string networks: The small-loop regime, Phys. Rev. D89, 083503 (2014), arXiv:1403.2621 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  53. [53]

    Caloni, R

    L. Caloni, R. Z. Ferreira, L. Sousa, and C. Winckler, Cosmic strings and domain walls: the impact of CMB B-mode data, (2026), arXiv:2602.20050 [astro-ph.CO]

    work page arXiv 2026

  54. [54]

    Raidal, A

    J. Raidal, A. Avgoustidis, E. Copeland, and A. Moss, CMB anisotropies from cosmic (super)strings in light of ACT DR6, (2026), arXiv:2602.18272 [astro-ph.CO]

    work page arXiv 2026

  55. [55]

    A. Ito, K. Kohri, and K. Nakayama, Probing high fre- quency gravitational waves with pulsars, Phys. Rev. D 109, 063026 (2024), arXiv:2305.13984

    work page arXiv 2024

  56. [56]

    T. Liu, J. Ren, and C. Zhang, Limits on High-Frequency Gravitational Waves in Planetary Magnetospheres, Phys. Rev. Lett.132, 131402 (2024), arXiv:2305.01832

    work page arXiv 2024

  57. [57]

    Y. He, S. K. Giri, R. Sharma, S. Mtchedlidze, and I. Georgiev, Inverse Gertsenshtein effect as a probe of high-frequency gravitational waves, JCAP05, 051, arXiv:2312.17636 [astro-ph.CO]

    work page arXiv

  58. [58]

    Vacalis, G

    G. Vacalis, G. Marocco, J. Bamber, R. Bingham, and G. Gregori, Detection of high-frequency gravitational waves using high-energy pulsed lasers, Class. Quant. Grav.40, 155006 (2023), arXiv:2301.08163

    work page arXiv 2023

  59. [59]

    Antoniadis et al

    J. Antoniadiset al.(EPTA, InPTA), The second data release from the European Pulsar Timing Array - IV. Implications for massive black holes, dark matter, and the early Universe, Astron. Astrophys.685, A94 (2024), arXiv:2306.16227 [astro-ph.CO]

    work page arXiv 2024

  60. [60]

    The NANOGrav 15-year Data Set: Search for Signals from New Physics

    A. Afzalet al.(NANOGrav), The NANOGrav 15 yr Data Set: Search for Signals from New Physics, Astrophys. J. Lett.951, L11 (2023), [Erratum: Astrophys.J.Lett. 971, L27 (2024), Erratum: Astrophys.J. 971, L27 (2024)], arXiv:2306.16219 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2023