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REVIEW 3 major objections 4 minor 4 cited by

Do Cosmic String Segments Emit Gravitational Waves?

T0 review · 3 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read The paper argues that monopoles at the ends of metastable cosmic string segments are slowed by collisions with thermal fluctuations on the string, so the accelerated oscillations assumed in previous gravitational-wave estimates never occur.

desk verdict A novel drag mechanism that would kill the oscillating-segment GW contribution, but it leans on an assumed thermal zero-mode population; worth refereeing, not yet settled. read the letter →

arxiv 2507.12386 v1 pith:U6EZOCFP submitted 2025-07-16 hep-ph astro-ph.CO

Akifumi Chitose , Masahiro Ibe , Shunsuke Neda , Satoshi Shirai This is my paper
classification hep-phastro-ph.CO
keywords cosmicstringsmetastablegravitationalwavespulsartimingarraysmonopole-stringsegmentsthermalfluctuationsNANOGravGUTscale
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

Metastable cosmic strings, a leading candidate for the nanohertz gravitational-wave background seen by pulsar timing arrays, decay into segments whose endpoints are monopoles. Earlier work assumed these monopoles accelerate freely under string tension, oscillate, and radiate gravitational waves. This paper argues that transverse thermal fluctuations on the string act as a scattering bath: collisions drain the monopole's energy, capping its boost factor at a value far below the naive Hubble-time estimate. In the parameter region favored by pulsar-timing data, the monopole never reaches the oscillatory regime, so the gravitational-wave contribution from segments is negligible. If correct, the observed background must come from string loops rather than segments.

What carries the argument

The central object is the population of transverse zero-mode fluctuations on the string worldsheet, described as a two-dimensional massless field with a thermal Bose-Einstein distribution $f(p) \simeq 1/(e^{p/T_s}-1)$ and number density per unit length $n \simeq (T_s/\pi)\ln(M_{\mathrm{Pl}}/T_{\mathrm{fr}})$. The monopole moving along the string collides with these modes; the energy-loss rate from such collisions, once it exceeds the string tension $\mu_s$, sets the saturation boost factor $\gamma_m^{(\mathrm{cr})}$. This drag mechanism is what prevents the segment from entering the oscillation regime.

What would settle it

A numerical simulation of the $G'\rightarrow H$ symmetry-breaking transition that resolves the long-string transverse fluctuation spectrum: if the simulated power on scales well below the Hubble length is far below the assumed thermal distribution, the collisional drag vanishes and the monopole should reach $\gamma_m \sim (\mu_s/M_m)H^{-1}$, restoring the oscillatory segment emission.

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Extended reading notes

Core claim

The central claim is that string segments formed from a metastable cosmic string network do not enter the oscillatory regime. The critical boost factor at which collisional energy loss balances string tension is $\gamma_m^{(\mathrm{cr})} \simeq \max\bigl(\mu_s/(M_m T_s), \sqrt{\mu_s}/T_s\bigr)$, which is smaller than the naive $\gamma_m(H^{-1}) \simeq (\mu_s/M_m)\,H^{-1}$ by many orders of magnitude across the PTA-favored parameter space. Consequently, the endpoint monopole never reaches relativistic energies sufficient for violent oscillation; the segment shrinks at roughly constant velocity and dissipates its energy non-gravitationally through inelastic collisions and particle emission. The conclusion holds both for segments with confined magnetic flux and for those with unconfined flux, where Larmor radiation alone would otherwise allow uniform acceleration.

Load-bearing premise

The argument rests on the assumption that a long string at the decay epoch carries a thermal population of transverse zero modes with number density $n \simeq (T_s/\pi)\ln(M_{\mathrm{Pl}}/T_{\mathrm{fr}})$, as posited in Eqs. (9) through (11); if actual segments are smooth on all scales below the Hubble length, the monopole accelerates unimpeded and the segment emits gravitational waves.

Editorial extensions

If this is right

  • If the claim is correct, the stochastic gravitational-wave background from metastable cosmic strings is generated almost entirely by string loops, not by decaying segments.
  • The distinction between the NANOGrav META-L and META-LS scenarios loses its practical significance for gravitational-wave predictions, since segment emission is negligible in either case.
  • The energy stored in a segment is converted into particle production near the electroweak scale and eventually into light particles, rather than into gravitational radiation.
  • The late-time injection of Standard Model particles from segment decay is estimated to be below current big-bang nucleosynthesis bounds, though anisotropic or ultrahigh-energy injection effects remain unexamined.
  • The endpoint monopoles may remain relevant as sources of ultra-high-energy cosmic rays rather than gravitational waves.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A quantitative test of the central assumption could come from lattice field-theory simulations of the symmetry-breaking transition: if the simulated long-string transverse fluctuation spectrum is far sparser than the assumed thermal distribution, the collisional drag would shut off and the segment oscillation regime would return.
  • The same drag mechanism might apply to other string-like objects with endpoint particles, such as superconducting strings or necklaces, implying that their gravitational-wave emission could also be suppressed relative to naive estimates.
  • The paper's perturbative treatment breaks down when the center-of-mass energy approaches $\sqrt{\mu_s}$; the authors note that segments could even become black holes if the monopole energy grew unchecked. A non-perturbative treatment of microscopic loop formation would likely strengthen the energy-dissipation conclusion, but this remains to be shown.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. This Letter argues that the endpoint monopoles of metastable cosmic string segments do not undergo the violent oscillations previously assumed in gravitational wave (GW) estimates. The authors propose that thermal fluctuations of the string worldsheet act as scattering centers that drain the monopole's energy, so the monopole boost saturates at a critical value gamma_cr given by Eq. (17), far below the naive gamma_m(H^-1) obtained from uninterrupted Hubble-time acceleration. They conclude that string segments contribute negligibly to the GW background, including in the parameter region favored by recent pulsar timing array (PTA) data, and that the segment energy is instead dissipated non-gravitationally. The argument is presented through order-of-magnitude estimates for the zero-mode population, the per-collision energy loss, and the resulting drag force, with a parameter scan in Figure 3.

Significance. If the mechanism is correct, the paper removes a currently uncertain contribution to the PTA stochastic GW background from metastable cosmic string segments and sharpens the interpretation of NANOGrav's META-L and META-LS scenarios. The analysis is transparent, internally coherent at the order-of-magnitude level, and does not tune free parameters to obtain the suppression; the parameter scan in Figure 3 covers the PTA-favored region. I also credit the authors for explicitly flagging in the Discussion that their perturbative treatment may break down and that nonperturbative effects are expected to further enhance dissipation. However, the two load-bearing ingredients, the assumed thermal zero-mode population of Eqs. (9)-(11) and the energy-loss formula of Eqs. (15)-(16), are not derived from a specified microscopic model, so the central claim is currently a conditional one.

major comments (3)
  1. [Fluctuations on cosmic strings, Eqs. (9)-(11)] The drag force in Eq. (16) is proportional to the zero-mode number density n defined in Eq. (11), so the entire suppression of gamma_m relative to gamma_m(H^-1) rests on the thermal occupation assumed in Eq. (9). After Eq. (8), the paper states only that it is 'reasonable to assume' a Bose-Einstein distribution; no derivation from the Nambu-Goto action together with the plasma coupling, or from the string formation history, is supplied. If a real segment is smooth below the Hubble scale (n=0), dE_m/dt|_coll vanishes and the endpoint monopole accelerates unimpeded to gamma_m(H^-1), restoring the standard k^-1 segment GW spectrum. The remark that weaker coupling leaves finer fluctuations is a monotonicity statement with respect to coupling strength, but it does not establish a lower bound on the baseline population. Please derive the zero-mode spectrum from a microphysical model, cite a calculation that does, or explicitly frame the thermal population as an assumption and quantify how the GW suppression depends on it.
  2. [Limit on monopole acceleration, Eqs. (15)-(16)] Equations (15) and (16) are the quantitative core of the paper, but they are introduced as estimates rather than derived from a specified monopole-zero-mode interaction. Equation (14) gives only the center-of-mass energy; converting it into an energy loss per collision requires a scattering model (the coupling, the impact parameter, and whether the zero modes are coherent worldsheet fluctuations or particle-like excitations). Since the balance condition Eq. (17) follows from setting dE_m/dt|_coll equal to the string tension, the central result inherits this model dependence. Please derive Eq. (15) from an effective action with an explicit endpoint coupling, or clearly present it as an order-of-magnitude ansatz and test the sensitivity of gamma_cr to the assumed kinematics.
  3. [Fate of string segments and Discussion] The final paragraph concedes that the perturbative treatment is not sufficient and that within the treatment the segments may become black holes. As written, this does not invalidate the GW-negligibility conclusion, because nonperturbative dissipation would only strengthen the damping; however, the manuscript should make that logical point explicitly. It should also state whether the inelastic channel in Eq. (19) is the assumed dominant energy-loss mechanism or a placeholder. Without such clarification, the reader cannot tell whether the 'Fate of string segments' section is a prediction or a consistency warning.
minor comments (4)
  1. [Discussion] The word 'Schwarzhshild' in the final paragraph should be 'Schwarzschild'.
  2. [Figure 2 and text] The notation for the freeze-out temperature is inconsistent: the text uses T_fr, while the Figure 2 caption uses T_f and Tf; please unify the notation.
  3. [Equation (15)] The frame in which Eq. (15) is expressed should be stated more carefully; the text says 'measured in the rest frame of the thermal bath,' but the expression itself is not manifestly frame-invariant, and a brief definition of the incoming zero-mode momentum would help.
  4. [Fluctuations on cosmic strings, Eq. (12)] The infrared cutoff p_fr/T_fr ~ T_fr/M_Pl is introduced without derivation; the paper says the result is insensitive to it, but a sentence explaining its origin would improve readability.

Circularity Check

0 steps flagged · score 0.0 of 10

No circularity: the suppression of segment GW emission follows from an explicit zero-mode distribution and a force-balance condition; no fitted parameter is later called a prediction, and self-citations are non-load-bearing.

full rationale

The derivation chain is self-contained and non-circular. The central result, gamma_cr in Eq. (17), is obtained by balancing the string tension mu_s against the collision energy-loss rate in Eq. (16), which is constructed from two-body kinematics (Eq. (15)) and the zero-mode number density n in Eq. (11). That density is an input assumption: after Eq. (8), the paper states it is 'reasonable to assume' a Bose-Einstein distribution at T_fr, and the subsequent redshifted distribution in Eq. (10) follows from free streaming. This assumption is physically debatable, as the Skeptic headline notes, but it is not circular: it is not defined in terms of the target conclusion, and no equation makes gamma_cr depend on the GW spectrum or makes n depend on the absence of oscillations. No parameter is fitted to PTA data to produce the suppression; the PTA contours in Fig. 3 only identify the region where the derived ratio gamma_cr/gamma_m(H^-1) is small. The paper's self-citations (Refs. [14], [28], and [29]) are not load-bearing: the decay rate in Eq. (1) rests on Preskill-Vilenkin [8], Ref. [28] is only an example of models with extra modes, and the SM equation-of-state reference is standard thermodynamics. The Discussion's admission that the perturbative analysis is insufficient and that segments could become black holes is a stated limitation, not a circular step; if anything, it makes the conclusion more conservative. Thus there is no circular reduction to report.

Assumptions & free parameters 0 free parameters · 4 assumptions · 0 invented entities

The paper introduces no new particles or forces. Its central claim depends on the assumed existence and thermal population of transverse string zero modes, which are known objects in string theory, and on a heuristic collision model for the monopole endpoint. No parameters are fitted to data; the main inputs are physical masses and temperatures with stated ranges.

assumptions (4)
  • domain assumption Transverse zero modes on long cosmic strings are thermally populated with a Bose-Einstein distribution at freeze-out temperature Tfr, and redshift freely thereafter.
    Assumed in the section 'Fluctuations on cosmic strings', Eqs. (9) and (10). The number density of these modes sets the collision rate and is load-bearing for the central result. The authors argue the assumption is conservative, but it is not derived from a specific microphysical formation model.
  • ad hoc to paper The endpoint monopole interacts with each zero mode as a 1+1 dimensional scattering event and loses energy per collision according to Eq. (15), yielding the drag force in Eq. (16).
    This collision model is posited rather than derived from the Nambu-Goto action. The coupling of the monopole to the worldsheet fluctuations and the scattering cross-section are not specified, which is a major gap in the derivation.
  • domain assumption Metastable strings decay suddenly when the Hubble rate H equals sqrt(Gamma_d).
    Used to evaluate gamma_m(H^-1) and to construct the contour plot in Figure 3. This sudden-decay approximation is standard in the metastable string literature.
  • domain assumption The string segment is straight enough over the length scale Delta_l = (M_m/mu_s) gamma_cr for the drag argument to apply, despite Hubble-scale curvature.
    Invoked in the 'Limit on monopole acceleration' section. The argument requires local straightness only over a short scale, which the authors show is much less than the Hubble length.

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Cite this review

Pith. "Pith review of Do Cosmic String Segments Emit Gravitational Waves?." pith.science (2026). https://pith.science/paper/U6EZOCFP

@misc{pith2026250712386,
  author       = {Pith},
  title        = {Pith review of: Do Cosmic String Segments Emit Gravitational Waves?},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/U6EZOCFP}},
  note         = {Machine review of arXiv:2507.12386}
}
read the original abstract

Cosmic strings are predicted in various extensions of the Standard Model, including grand unified theories. Depending on the symmetry-breaking pattern, they can be either topologically stable or metastable. Intriguingly, metastable strings have been proposed as a possible origin of the gravitational wave (GW) background observed by recent pulsar timing array experiments. When metastable strings decay, they fragment into segments with monopoles and antimonopoles attached at their endpoints. The monopole and antimonopole are strongly pulled by the string tension. Violent oscillations of these segments have been considered as a potential GW source, in addition to contributions from string loops. We show that, in realistic situations, the monopoles frequently collide with thermal fluctuations on the string segments, which act as a resistance and prevent the oscillation. As a result, we find that the contribution from string segments to the GW background is negligible.

Figures

Figures reproduced from arXiv: 2507.12386 by the authors.

Figure 1
Figure 1. FIG. 1. Schematic illustration of a cosmic string, showing [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. The monopole energy loss rate divided by the drag [PITH_FULL_IMAGE:figures/full_fig_p003_2.png] view at source ↗
Figure 3
Figure 3. shows the ratio between the critical boost factor (17) with the na¨ıve one (6) with ℓ = H−1 in the parameter space of (GNµs, √ κ). In the figure, we as￾sume the sudden decay at H = √ Γd. Figure shows that γ (cr) m /γm(H−1 ) ≪ 1 in the entire parameter space. In the figure, we also show the posterior distributions of (GNµs, √ κ) favored by the PTA signal reported in Ref. [15] for the META-L and the META-LS scenarios … view at source ↗

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Forward citations

Cited by 4 Pith papers

Reviewed papers in the Pith corpus that reference this work. Sorted by Pith novelty score. Full citation record

  1. Metastable cosmic strings are broken at the start

    hep-ph 2026-01 conditional novelty 7.0 of 10

    Metastable cosmic-string networks are typically broken within a Hubble time of formation by finite-temperature effects or by pre-existing monopoles, so matching NANOGrav requires m_M^2/μ ≳ 10^3.

  2. LISA Reconstruction Landscape for Metastable Cosmic Strings

    hep-ph 2026-07 conditional novelty 6.0 of 10

    LISA can reconstruct metastable cosmic-string tension and lifetime when it samples the tail-to-plateau transition, with residual κ_CS sensitivity possible even in high-SNR plateau-like spectra.

  3. Cosmic string gravitational wave backgrounds at LISA: I. Signal survey, template reconstruction, and model comparison

    astro-ph.CO 2025-08 unverdicted novelty 5.0 of 10

    As provided, the manuscript body (random lasing) does not correspond to the abstract (cosmic string gravitational wave backgrounds at LISA), leaving the abstract's quantitative claims unsupported by any accessible text.

  4. Monopoles, Strings, Walls and Gravitational waves

    hep-ph 2026-07 conditional novelty 4.0 of 10

    Breaking SU(2) flavor gauge symmetry stepwise to nothing leaves monopoles, strings, and walls; collapsing walls can form composite strings whose gravitational-wave spectra fit PTA data and lie within reach of LVK and ...

Reference graph

Works this paper leans on

32 extracted references · 5 canonical work pages · cited by 4 Pith papers

  1. [1]

    Agazie et al

    G. Agazie et al. (NANOGrav), The NANOGrav 15 yr Data Set: Evidence for a Gravitational-wave 5 Background, Astrophys. J. Lett. 951, L8 (2023), arXiv:2306.16213 [astro-ph.HE]

    arXiv 2023

  2. [2]

    Antoniadis et al

    J. Antoniadis et al. (EPTA, InPTA:), The second data release from the European Pulsar Timing Array - III. Search for gravitational wave signals, Astron. Astrophys. 678, A50 (2023), arXiv:2306.16214 [astro-ph.HE]

    arXiv 2023

  3. [3]

    D. J. Reardon et al. , Search for an Isotropic Gravitational-wave Background with the Parkes Pul- sar Timing Array, Astrophys. J. Lett. 951, L6 (2023), arXiv:2306.16215 [astro-ph.HE]

    arXiv 2023

  4. [4]

    Xu et al., Searching for the Nano-Hertz Stochastic Gravitational Wave Background with the Chinese Pulsar Timing Array Data Release I, Res

    H. Xu et al., Searching for the Nano-Hertz Stochastic Gravitational Wave Background with the Chinese Pulsar Timing Array Data Release I, Res. Astron. Astrophys. 23, 075024 (2023), arXiv:2306.16216 [astro-ph.HE]

    arXiv 2023

  5. [5]

    Vilenkin and E

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

    2000

  6. [6]

    Vilenkin, COSMOLOGICAL EVOLUTION OF MONOPOLES CONNECTED BY STRINGS, Nucl

    A. Vilenkin, COSMOLOGICAL EVOLUTION OF MONOPOLES CONNECTED BY STRINGS, Nucl. Phys. B 196, 240 (1982)

    work page 1982

  7. [7]

    Chitose, M

    A. Chitose, M. Ibe, S. Shirai, and Y. Wen, Cosmic Strings in Multi-Step Symmetry Breaking, (2025), arXiv:2506.15194 [hep-ph]

    arXiv 2025

  8. [8]

    Preskill and A

    J. Preskill and A. Vilenkin, Decay of metastable topo- logical defects, Phys. Rev. D 47, 2324 (1993), arXiv:hep- ph/9209210

    arXiv 1993

Show all 32 references
  1. [9]

    Leblond, B

    L. Leblond, B. Shlaer, and X. Siemens, Gravitational Waves from Broken Cosmic Strings: The Bursts and the Beads, Phys. Rev. D 79, 123519 (2009), arXiv:0903.4686 [astro-ph.CO]

    2009 arXiv

  2. [10]

    Buchmuller, V

    W. Buchmuller, V. Domcke, H. Murayama, and K. Schmitz, Probing the scale of grand unification with gravitational waves, Phys. Lett. B 809, 135764 (2020), arXiv:1912.03695 [hep-ph]

    2020 arXiv

  3. [11]

    Buchmuller, V

    W. Buchmuller, V. Domcke, and K. Schmitz, From NANOGrav to LIGO with metastable cosmic strings, Phys. Lett. B 811, 135914 (2020), arXiv:2009.10649 [astro-ph.CO]

    2020 arXiv

  4. [12]

    Buchmuller, V

    W. Buchmuller, V. Domcke, and K. Schmitz, Stochastic gravitational-wave background from metastable cosmic strings, JCAP 12 (12), 006, arXiv:2107.04578 [hep-ph]

    arXiv

  5. [13]

    Buchmuller, V

    W. Buchmuller, V. Domcke, and K. Schmitz, Metastable cosmic strings, JCAP 11, 020, arXiv:2307.04691 [hep- ph]

    arXiv

  6. [14]

    Chitose, M

    A. Chitose, M. Ibe, Y. Nakayama, S. Shirai, and K. Watanabe, Revisiting metastable cosmic string break- ing, JHEP 04, 068, arXiv:2312.15662 [hep-ph]

    arXiv

  7. [15]

    Afzal et al.(NANOGrav), The NANOGrav 15 yr Data Set: Search for Signals from New Physics, Astrophys

    A. Afzal et 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]

    2023 arXiv

  8. [16]

    Berezinsky, X

    V. Berezinsky, X. Martin, and A. Vilenkin, High-energy particles from monopoles connected by strings, Phys. Rev. D 56, 2024 (1997), arXiv:astro-ph/9703077

    1997 arXiv

  9. [17]

    Martin and A

    X. Martin and A. Vilenkin, Gravitational radiation from monopoles connected by strings, Phys. Rev. D 55, 6054 (1997), arXiv:gr-qc/9612008

    1997 arXiv

  10. [18]

    Servant and P

    G. Servant and P. Simakachorn, Ultrahigh frequency pri- mordial gravitational waves beyond the kHz: The case of cosmic strings, Phys. Rev. D 109, 103538 (2024), arXiv:2312.09281 [hep-ph]

    2024 arXiv

  11. [19]

    C. L. Carilli and S. Rawlings, Science with the Square Kilometer Array: Motivation, key science projects, stan- dards and assumptions, New Astron. Rev.48, 979 (2004), arXiv:astro-ph/0409274

    2004 arXiv

  12. [20]

    Janssen et al., Gravitational wave astronomy with the SKA, PoS AASKA14, 037 (2015), arXiv:1501.00127 [astro-ph.IM]

    G. Janssen et al., Gravitational wave astronomy with the SKA, PoS AASKA14, 037 (2015), arXiv:1501.00127 [astro-ph.IM]

    2015 arXiv

  13. [21]

    Weltman et al., Fundamental physics with the Square Kilometre Array, Publ

    A. Weltman et al., Fundamental physics with the Square Kilometre Array, Publ. Astron. Soc. Austral. 37, e002 (2020), arXiv:1810.02680 [astro-ph.CO]

    2020 arXiv

  14. [22]

    Amaro-Seoane et al

    P. Amaro-Seoane et al. (LISA), Laser Interferometer Space Antenna, (2017), arXiv:1702.00786 [astro-ph.IM]

    2017 arXiv

  15. [23]

    Baker et al., The Laser Interferometer Space Antenna: Unveiling the Millihertz Gravitational Wave Sky, (2019), arXiv:1907.06482 [astro-ph.IM]

    J. Baker et al., The Laser Interferometer Space Antenna: Unveiling the Millihertz Gravitational Wave Sky, (2019), arXiv:1907.06482 [astro-ph.IM]

    2019 arXiv

  16. [24]

    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, JCAP 05, 006, arXi...

    arXiv

  17. [25]

    Abac et al., The Science of the Einstein Telescope, (2025), arXiv:2503.12263 [gr-qc]

    A. Abac et al., The Science of the Einstein Telescope, (2025), arXiv:2503.12263 [gr-qc]

    2025 arXiv

  18. [26]

    A. D. Linde, Axions in inflationary cosmology, Phys. Lett. B 259, 38 (1991)

    1991

  19. [27]

    A. D. Linde, Hybrid inflation, Phys. Rev. D 49, 748 (1994), arXiv:astro-ph/9307002

    1994 arXiv

  20. [28]

    Chitose, M

    A. Chitose, M. Ibe, S. Neda, and S. Shirai, Gravitational waves from metastable cosmic strings in supersymmetric new inflation model, JCAP 04, 010, arXiv:2411.13299 [hep-ph]

    arXiv

  21. [29]

    Saikawa and S

    K. Saikawa and S. Shirai, Primordial gravitational waves, precisely: The role of thermodynamics in the Standard Model, JCAP 05, 035, arXiv:1803.01038 [hep-ph]; Pre- cise WIMP Dark Matter Abundance and Standard Model Thermodynamics, JCAP 08, 011, arXiv:2005.03544 [hep- ph]

    2005 arXiv

  22. [30]

    Babichev, V

    E. Babichev, V. Dokuchaev, and M. Kachelriess, Gravita- tional radiation from rotating monopole-string systems, Phys. Rev. D71, 044028 (2005), arXiv:astro-ph/0411794

    2005 arXiv

  23. [31]

    Kawasaki, K

    M. Kawasaki, K. Kohri, T. Moroi, and Y. Takaesu, Re- visiting Big-Bang Nucleosynthesis Constraints on Long- Lived Decaying Particles, Phys. Rev. D 97, 023502 (2018), arXiv:1709.01211 [hep-ph]

    2018 arXiv

  24. [32]

    Berezinsky, P

    V. Berezinsky, P. Blasi, and A. Vilenkin, Ultrahigh- energy gamma-rays as signature of topological defects, Phys. Rev. D58, 103515 (1998), arXiv:astro-ph/9803271

    1998 arXiv

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