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arxiv: 2509.04028 · v3 · pith:ZX4I5BAFnew · submitted 2025-09-04 · 🌌 astro-ph.CO · gr-qc· hep-ph

Primordial black holes versus their impersonators at gravitational wave observatories

Andrea Begnoni , Stefano Profumo This is my paper

Pith reviewed 2026-05-21 22:11 UTC · model grok-4.3

classification 🌌 astro-ph.CO gr-qchep-ph
keywords primordial black holesgravitational wavesexotic compact objectstidal deformabilityneutron starsbinary mergersfuture detectors
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The pith

Next-generation gravitational wave detectors can identify sub-solar mass primordial black holes out to redshift 3 and distinguish them from neutron stars to redshift 0.2 by the absence of tidal effects.

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

The paper sets out to determine the reach of future gravitational wave observatories for spotting sub-solar mass black holes and for separating them from other compact objects that produce similar signals. It calculates how far out the lack of tidal deformation in a black hole binary can be measured with certainty compared with neutron stars or strange quark stars. A sympathetic reader would care because any confirmed sub-solar mass black hole would point to new physics, given that ordinary stellar evolution does not produce them. The work supplies concrete distance limits for reliable identification or exclusion under different mass and equation-of-state assumptions. If the limits hold, observers gain a practical test for whether a detected compact object is primordial rather than an astrophysical or exotic mimic.

Core claim

Using the Fisher matrix formalism on gravitational waveforms from binary coalescences, the analysis shows that next-generation detectors reach greater than 3 sigma sensitivity to sub-solar masses out to redshift approximately 3 and can distinguish primordial black holes from neutron stars through the absence of tidal deformability for masses up to roughly 2 solar masses out to redshift 0.2, for a range of nuclear and quark matter equations of state.

What carries the argument

The Fisher matrix formalism applied to gravitational waveforms, which forecasts the measurement precision on masses, spins, and tidal deformability parameters that differ between black holes and other compact objects.

If this is right

  • Sub-solar mass primordial black holes become detectable out to cosmological distances of redshift around 3.
  • Primordial black holes up to 2 solar masses can be separated from neutron stars by the lack of tidal effects up to redshift 0.2.
  • Quantitative luminosity distance limits are supplied for confident identification or exclusion under varied observational conditions.
  • Exotic compact object candidates such as strange quark stars and boson stars produce distinguishable signatures from black holes in the same mass range.

Where Pith is reading between the lines

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

  • A confirmed sub-solar mass detection without tidal signatures would tighten limits on the fraction of dark matter that can consist of primordial black holes.
  • The same waveform analysis could be applied to other proposed exotic objects not modeled in the paper to test additional formation channels.
  • Non-detection of sub-solar mass events at the predicted distances would constrain the allowed mass function of primordial black holes formed in the early universe.

Load-bearing premise

No astrophysical channel can produce black holes below one solar mass, so any such object must be primordial or exotic.

What would settle it

A gravitational wave detection of a sub-solar mass binary at redshift below 0.2 that exhibits measurable tidal deformability matching a neutron star equation of state would show that the claimed distinction cannot be made at the stated distance.

read the original abstract

The detection of primordial black holes (PBHs) would mark a major breakthrough, with far-reaching implications for early universe cosmology, fundamental physics, and the nature of dark matter. Gravitational wave observations have recently emerged as a powerful tool to test the existence and properties of PBHs, as these objects leave distinctive imprints on the gravitational waveform. Notably, there are no known astrophysical processes that can form sub-solar mass black holes, making their discovery a compelling signal of new physics. In addition to PBHs, we consider other exotic compact object (ECO) candidates-such as strange quark stars and boson stars-which can produce similar gravitational signatures and potentially mimic PBHs. In this work, we employ the Fisher matrix formalism to explore a broad parameter space, including binary masses, spins, and a variety of nuclear and quark matter equations of state. Our goal is to assess the ability of next-generation gravitational wave detectors-specifically Cosmic Explorer and the Einstein Telescope-to distinguish PBHs from ECOs, stellar BHs and neutron stars. We compute the maximum luminosity distances at which confident ($\geq 3\sigma$) detections of sub-solar masses or tidal effects are possible, providing quantitative benchmarks for PBH identification or exclusion under various observational scenarios. Our results indicate that next-generation detectors will be capable of probing sub-solar mass PBHs out to cosmological distances of $z \sim 3$. For heavier objects with masses up to $M \lesssim 2 M_\odot$, we show that PBHs can be distinguished from neutron stars via their lack of tidal effects up to redshifts of $z \sim 0.2$.

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 employs the Fisher matrix formalism to forecast the reach of next-generation gravitational-wave detectors (Cosmic Explorer and Einstein Telescope) for distinguishing primordial black holes (PBHs) from exotic compact objects (ECOs such as strange quark stars and boson stars), neutron stars, and stellar black holes. It explores binary masses, spins, and a range of nuclear and quark-matter equations of state, reporting maximum luminosity distances (or redshifts) at which sub-solar-mass PBHs can be identified at ≥3σ significance (z∼3) and at which PBHs can be separated from neutron stars via the absence of tidal deformability (z∼0.2 for M≲2M⊙).

Significance. If the quantitative forecasts hold after validation, the paper supplies useful benchmark distances for PBH searches and ECO exclusion in the 2030s detector era. The explicit scan over multiple EOS and the focus on tidal effects as a discriminator constitute a strength relative to single-EOS studies.

major comments (2)
  1. [§3.2] §3.2 (Fisher-matrix implementation): The central claims for sub-solar-mass PBH reach to z∼3 and tidal distinguishability to z∼0.2 rest on Fisher-matrix error estimates for the tidal deformability parameter Λ (or its absence). For the sub-solar binaries that set the z∼3 horizon the network SNR is expected to be modest (≲10–12); in this regime the quadratic approximation systematically underestimates uncertainties for correlated parameters such as spins and EOS-dependent terms. The manuscript reports neither the SNR values at the quoted distances nor any cross-check against full Bayesian sampling or injection studies, rendering the luminosity-distance results vulnerable to inflation.
  2. [§4.1] §4.1 and associated tables: The maximum distances for ≥3σ separation are presented without accompanying SNR values, condition numbers of the Fisher matrix, or discussion of the validity of the Gaussian approximation at the quoted redshifts. This directly affects the load-bearing quantitative benchmarks for both the sub-solar and M≲2M⊙ cases.
minor comments (2)
  1. [Abstract] Abstract: The phrase 'confident (≥3σ) detections of sub-solar masses or tidal effects' should clarify whether the 3σ threshold applies to signal detection or to a parameter deviation from the PBH hypothesis.
  2. [§2] Notation: The symbol Λ is used for tidal deformability without an explicit definition or reference to the standard definition in the waveform model section; this could be clarified for readers outside the GW community.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thorough review and valuable comments on our manuscript. We address the major comments point by point below, and have revised the manuscript accordingly to improve the robustness of our forecasts.

read point-by-point responses

  1. Referee: [§3.2] §3.2 (Fisher-matrix implementation): The central claims for sub-solar-mass PBH reach to z∼3 and tidal distinguishability to z∼0.2 rest on Fisher-matrix error estimates for the tidal deformability parameter Λ (or its absence). For the sub-solar binaries that set the z∼3 horizon the network SNR is expected to be modest (≲10–12); in this regime the quadratic approximation systematically underestimates uncertainties for correlated parameters such as spins and EOS-dependent terms. The manuscript reports neither the SNR values at the quoted distances nor any cross-check against full Bayesian sampling or injection studies, rendering the luminosity-distance results vulnerable to inflation.

    Authors: We agree that the Fisher matrix method is an approximation whose accuracy decreases at lower SNRs. To address this, we will add the network SNR values for the key benchmark distances in a new table or in the text of §3.2 and §4.1. We note that our quoted horizons are chosen such that the SNR is at least ~8-10, where the approximation is commonly used in the literature for similar forecasts. While a full Bayesian validation would be ideal, it is computationally demanding for the broad parameter space explored (multiple EOS, masses, spins); we will include a discussion of the limitations of the Fisher approach and cite relevant studies on its validity in the low-SNR regime. This constitutes a partial revision as we enhance the presentation without performing new simulations. revision: partial

  2. Referee: [§4.1] §4.1 and associated tables: The maximum distances for ≥3σ separation are presented without accompanying SNR values, condition numbers of the Fisher matrix, or discussion of the validity of the Gaussian approximation at the quoted redshifts. This directly affects the load-bearing quantitative benchmarks for both the sub-solar and M≲2M⊙ cases.

    Authors: We acknowledge the importance of these details for assessing the reliability of our results. In the revised manuscript, we will include SNR values and condition numbers (where the matrix is well-conditioned) for the reported distances in §4.1 and update the tables accordingly. Additionally, we will add a paragraph discussing the applicability of the Gaussian approximation, referencing that for SNRs above ~10 the Fisher matrix provides reasonable estimates for parameter uncertainties in GW analyses. These changes will be made to strengthen the manuscript. revision: yes

Circularity Check

0 steps flagged

No significant circularity; forecasts use standard external methods

full rationale

The paper applies the Fisher matrix formalism to standard waveform models and external detector noise curves to compute luminosity-distance reaches for PBH/ECO distinguishability. No equation or result reduces by construction to a fitted parameter defined from the same data, nor does any central claim rest on a self-citation chain, uniqueness theorem imported from the authors, or ansatz smuggled via prior work. The derivation is self-contained against external benchmarks (detector sensitivities, waveform approximants) and does not exhibit self-definitional or fitted-input-called-prediction patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 2 axioms · 0 invented entities

The central claim rests on the validity of the Fisher-matrix approximation for waveform parameter estimation and on the modeling of tidal effects under multiple nuclear and quark-matter equations of state; no new entities are introduced.

axioms (2)
  • standard math General relativity and the chosen waveform approximants accurately describe the signals from PBH and ECO binaries
    Implicit in the use of Fisher matrix on gravitational waveforms.
  • domain assumption The explored set of nuclear and quark equations of state spans the relevant range for exotic compact objects
    Paper states it considers a variety of such EOS.

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Works this paper leans on

112 extracted references · 112 canonical work pages · 45 internal anchors

  1. [1]

    Postnikov, M

    S. Postnikov, M. Prakash and J.M. Lattimer,Tidal love numbers of neutron and self-bound quark stars,Phys. Rev. D82(2010) 024016

    work page 2010

  2. [2]

    Relativistic theory of tidal Love numbers

    T. Binnington and E. Poisson,Relativistic theory of tidal Love numbers,Phys. Rev. D80 (2009) 084018 [0906.1366]. – 19 –

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  3. [3]

    Crescimbeni, G

    F. Crescimbeni, G. Franciolini, P. Pani and A. Riotto,Can we identify primordial black holes? Tidal tests for subsolar-mass gravitational-wave observations,Phys. Rev. D109(2024) 124063 [2402.18656]

    work page arXiv 2024

  4. [4]

    De Luca, G

    V. De Luca, G. Franciolini and A. Riotto,Flea on the elephant: Tidal Love numbers in subsolar primordial black hole searches,Phys. Rev. D110(2024) 104041 [2408.14207]

    work page arXiv 2024

  5. [5]

    Crescimbeni, G

    F. Crescimbeni, G. Franciolini, P. Pani and M. Vaglio,Cosmology and nuclear physics implications of a subsolar gravitational-wave event,Phys. Rev. D111(2025) 083538 [2408.14287]

    work page arXiv 2025

  6. [6]

    E.-P. Zhou, X. Zhou and A. Li,Constraints on interquark interaction parameters with GW170817 in a binary strange star scenario,Phys. Rev. D97(2018) 083015 [1711.04312]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  7. [7]

    Miao, J.-L

    Z. Miao, J.-L. Jiang, A. Li and L.-W. Chen,Bayesian Inference of Strange Star Equation of State Using the GW170817 and GW190425 Data,Astrophys. J. Lett.917(2021) L22 [2107.13997]

    work page arXiv 2021

  8. [8]

    Vines and É

    J. Vines and É. Flanagan,Post-1-newtonian tidal effects in the gravitational waveform from binary inspirals,Phys. Rev. D83(2011) 084051

    work page 2011

  9. [10]

    Z. Ji, J. Chen and G. Wu,Insights into Neutron Star Matter: EoS Models and Observations, 2505.05241

    work page arXiv

  10. [11]

    Tidal Deformabilities and Neutron Star Mergers

    T. Zhao and J.M. Lattimer,Tidal Deformabilities and Neutron Star Mergers,Phys. Rev. D 98(2018) 063020 [1808.02858]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  11. [12]

    Vaglio, C

    M. Vaglio, C. Pacilio, A. Maselli and P. Pani,Bayesian parameter estimation on boson-star binary signals with a coherent inspiral template and spin-dependent quadrupolar corrections, Physical Review D108(2023) 023021

    work page 2023

  12. [13]

    Sennett, T

    N. Sennett, T. Hinderer, J. Steinhoff, A. Buonanno and S. Ossokine,Distinguishing Boson Stars from Black Holes and Neutron Stars from Tidal Interactions in Inspiraling Binary Systems,Physical Review D96(2017) 024002

    work page 2017

  13. [14]

    Pacilio, A

    C. Pacilio, A. Maselli, M. Fasano and P. Pani,Ranking Love Numbers for the Neutron Star Equation of State: The Need for Third-Generation Detectors,Phys. Rev. Lett.128(2022) 101101 [2104.10035]

    work page arXiv 2022

  14. [15]

    Pompili, E

    L. Pompili, E. Maggio, H.O. Silva and A. Buonanno,Parametrized spin-precessing inspiral-merger-ringdown waveform model for tests of general relativity,Phys. Rev. D111 (2025) 124040 [2504.10130]

    work page arXiv 2025

  15. [16]

    Ghosh and M

    S. Ghosh and M. Hannam,On the Identification of Exotic Compact Binaries with Gravitational Waves: a Phenomenological approach,2505.16380

    work page arXiv

  16. [17]

    Maximum mass and radius of strange stars in the linear approximation of the EOS

    T. Harko and K.S. Cheng,Maximum mass and radius of strange stars in the linear approximation of the EOS,Astron. Astrophys.385(2002) 947 [astro-ph/0203033]

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  17. [18]

    Zhang, Y.-F

    X.-L. Zhang, Y.-F. Huang and Z.-C. Zou,Recent progresses in strange quark stars, 2404.00363

    work page arXiv

  18. [19]

    Takátsy and P

    J. Takátsy and P. Kovács,Comment on ”Tidal Love numbers of neutron and self-bound quark stars”,Phys. Rev. D102(2020) 028501 [2007.01139]

    work page arXiv 2020

  19. [20]

    Tidal deformability and I-Love-Q relations for gravastars with polytropic thin shells

    N. Uchikata, S. Yoshida and P. Pani,Tidal deformability and I-Love-Q relations for gravastars with polytropic thin shells,Phys. Rev. D94(2016) 064015 [1607.03593]. – 20 –

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  20. [21]

    Gamba, M

    R. Gamba, M. Breschi, S. Bernuzzi, M. Agathos and A. Nagar,Waveform systematics in the gravitational-wave inference of tidal parameters and equation of state from binary neutron star signals,Phys. Rev. D103(2021) 124015 [2009.08467]

    work page arXiv 2021

  21. [22]

    Koehn, T

    H. Koehn, T. Wouters, H. Rose, P.T.H. Pang, R. Somasundaram, I. Tews et al.,Probe and Prejudice: Classification of compact objects and model comparison using EOS knowledge, Physical Review D110(2024) 103015

    work page 2024

  22. [23]

    Magnall, C

    S.J. Magnall, C. Ecker, L. Rezzolla, P.D. Lasky and S.R. Goode,Physics-informed Priors Improve Gravitational-wave Constraints on Neutron-star Matter,Astrophys. J. Lett.988 (2025) L75 [2504.21526]

    work page arXiv 2025

  23. [24]

    Huang,Model-independent Determination of the Tidal Deformability of a 1.4 M○ Neutron Star from Gravitational-wave Measurements,Astrophys

    C. Huang,Model-independent Determination of the Tidal Deformability of a 1.4 M○ Neutron Star from Gravitational-wave Measurements,Astrophys. J.985(2025) 216 [2505.14822]

    work page arXiv 2025

  24. [25]

    Markin, A

    I. Markin, A. Neuweiler, A. Abac, S.V. Chaurasia, M. Ujevic, M. Bulla et al., General-relativistic hydrodynamics simulation of a neutron star–sub-solar-mass black hole merger,Physical Review D108(2023) 064025

    work page 2023

  25. [26]

    Franciolini, R

    G. Franciolini, R. Cotesta, N. Loutrel, E. Berti, P. Pani and A. Riotto,How to assess the primordial origin of single gravitational-wave events with mass, spin, eccentricity, and deformability measurements,Phys. Rev. D105(2022) 063510 [2112.10660]

    work page arXiv 2022

  26. [27]

    Gasparotto, G

    S. Gasparotto, G. Franciolini and V. Domcke,Gravitational Wave Memory of Primordial Black Hole Mergers,2505.01356

    work page arXiv

  27. [29]

    Laskos-Patkos and C.C

    P. Laskos-Patkos and C.C. Moustakidis,XTE J1814-338: A potential hybrid star candidate, Phys. Rev. D111(2025) 063058 [2410.18498]

    work page arXiv 2025

  28. [30]

    Begnoni, S

    A. Begnoni, S. Anselmi, M. Pieroni, A. Renzi and A. Ricciardone,Detectability and Parameter Estimation for Einstein Telescope Configurations with GWJulia,2506.21530

    work page arXiv

  29. [31]

    Use and Abuse of the Fisher Information Matrix in the Assessment of Gravitational-Wave Parameter-Estimation Prospects

    M. Vallisneri,Use and abuse of the Fisher information matrix in the assessment of gravitational-wave parameter-estimation prospects,Phys. Rev. D77(2008) 042001 [gr-qc/0703086]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  30. [32]

    Inadequacies of the Fisher Information Matrix in gravitational-wave parameter estimation

    C.L. Rodriguez, B. Farr, W.M. Farr and I. Mandel,Inadequacies of the Fisher Information Matrix in gravitational-wave parameter estimation,Phys. Rev. D88(2013) 084013 [1308.1397]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  31. [33]

    Detection, Measurement and Gravitational Radiation

    L.S. Finn,Detection, measurement and gravitational radiation,Phys. Rev. D46(1992) 5236 [gr-qc/9209010]

    work page internal anchor Pith review Pith/arXiv arXiv 1992

  32. [34]

    Gravitational Waves from Mergin Compact Binaries: How Accurately Can One Extract the Binary's Parameters from the Inspiral Waveform?

    C. Cutler and E.E. Flanagan,Gravitational waves from merging compact binaries: How accurately can one extract the binary’s parameters from the inspiral wave form?,Phys. Rev. D 49(1994) 2658 [gr-qc/9402014]

    work page internal anchor Pith review Pith/arXiv arXiv 1994

  33. [35]

    Iacovelli, M

    F. Iacovelli, M. Mancarella, S. Foffa and M. Maggiore,Forecasting the Detection Capabilities of Third-generation Gravitational-wave Detectors Using GWFAST,Astrophys. J.941(2022) 208 [2207.02771]

    work page arXiv 2022

  34. [36]

    Dupletsa, J

    U. Dupletsa, J. Harms, B. Banerjee, M. Branchesi, B. Goncharov, A. Maselli et al.,gwfish: A simulation software to evaluate parameter-estimation capabilities of gravitational-wave detector networks,Astron. Comput.42(2023) 100671 [2205.02499]

    work page arXiv 2023

  35. [37]

    Pieroni, A

    M. Pieroni, A. Ricciardone and E. Barausse,Detectability and parameter estimation of stellar origin black hole binaries with next generation gravitational wave detectors,Sci. Rep.12 (2022) 17940 [2203.12586]. – 21 –

    work page arXiv 2022

  36. [38]

    Borhanian,GWBENCH: a novel Fisher information package for gravitational-wave benchmarking,Class

    S. Borhanian,GWBENCH: a novel Fisher information package for gravitational-wave benchmarking,Class. Quant. Grav.38(2021) 175014 [2010.15202]

    work page arXiv 2021

  37. [39]

    Borhanian and B.S

    S. Borhanian and B.S. Sathyaprakash,Listening to the Universe with next generation ground-based gravitational-wave detectors,Phys. Rev. D110(2024) 083040 [2202.11048]

    work page arXiv 2024

  38. [40]

    de Souza and R

    J.M.S. de Souza and R. Sturani,GWDALI: A Fisher-matrix based software for gravitational wave parameter-estimation beyond Gaussian approximation,Astron. Comput.45(2023) 100759 [2307.10154]

    work page arXiv 2023

  39. [41]

    Y. Li, I.S. Heng, M.L. Chan, C. Messenger and X. Fan,Exploring the sky localization and early warning capabilities of third generation gravitational wave detectors in three-detector network configurations,Phys. Rev. D105(2022) 043010 [2109.07389]

    work page arXiv 2022

  40. [42]

    The Science of the Einstein Telescope

    A. Abac et al.,The Science of the Einstein Telescope,2503.12263. [46]Planckcollaboration,Planck 2018 results. VI. Cosmological parameters,Astron. Astrophys. 641(2020) A6 [1807.06209]

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  41. [43]

    Witten,Cosmic Separation of Phases,Phys

    E. Witten,Cosmic Separation of Phases,Phys. Rev. D30(1984) 272

    work page 1984

  42. [44]

    Bodmer,Collapsed nuclei,Phys

    A.R. Bodmer,Collapsed nuclei,Phys. Rev. D4(1971) 1601

    work page 1971

  43. [45]

    Strange stars - linear approximation of the EOS and maximum QPO frequency

    J.L. Zdunik,On the mass of moderately rotating strange stars,Astron. Astrophys.359(2000) 311 [astro-ph/0004375]

    work page internal anchor Pith review Pith/arXiv arXiv 2000

  44. [46]

    Color-flavor locked strange matter

    G. Lugones and J.E. Horvath,Color-flavor locked strange matter,Phys. Rev. D66(2002) 074017 [hep-ph/0211070]

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  45. [47]

    How to identify a Strange Star

    J. Madsen,How to identify a strange star,Phys. Rev. Lett.81(1998) 3311 [astro-ph/9806032]

    work page internal anchor Pith review Pith/arXiv arXiv 1998

  46. [48]

    Small quark stars in the chromodielectric model

    M. Malheiro, E.O. Azevedo, L.G. Nuss, M. Fiolhais and A.R. Taurines,Small quark stars in the chromodielectric model,AIP Conf. Proc.631(2002) 658 [hep-ph/0111148]

    work page internal anchor Pith review Pith/arXiv arXiv 2002

  47. [49]

    Benvenuto and G

    O.G. Benvenuto and G. Lugones,The properties of strange stars in the quark mass-density-dependent model,Int. J. Mod. Phys. D7(1998) 29

    work page 1998

  48. [50]

    Superconducting phases of strange quark matter in the NJL model

    L. Paulucci, J.E. Horvath, E.J. Ferrer and V. de la Incera,Superconducting phases of strange quark matter in the NJL model, inCompact Stars in the QCD Phase Diagram III, 7, 2013 [1307.2290]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  49. [51]

    W.-L. Yuan, A. Li, Z. Miao, B. Zuo and Z. Bai,Interacting ud and uds quark matter at finite densities and quark stars,Phys. Rev. D105(2022) 123004 [2203.04798]

    work page arXiv 2022

  50. [52]

    Relativistic Shapiro delay measurements of an extremely massive millisecond pul- sar,

    H.T. Cromartie and et al.,Relativistic Shapiro delay measurements of an extremely massive millisecond pulsar,Nature Astronomy4(2020) 72 [1904.06759]

    work page arXiv 2020

  51. [53]

    Effects of color superconductivity on the nucleation of quark matter in neutron stars

    I. Bombaci, G. Lugones and I. Vidana,Effects of color superconductivity on the nucleation of quark matter in neutron stars,Astron. Astrophys.462(2007) 1017 [astro-ph/0603644]. [58]LIGO Scientific, Virgocollaboration,GW170817: Measurements of neutron star radii and equation of state,Phys. Rev. Lett.121(2018) 161101 [1805.11581]

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  52. [54]

    Liu and Z.-W

    Z. Liu and Z.-W. Tang,Probing ultralight isospin-violating mediators at GW170817,JHEP 06(2024) 090 [2402.06209]

    work page arXiv 2024

  53. [55]

    Z. Wang, Y. Gao, D. Liang, J. Zhao and L. Shao,Vetting quark-star models with gravitational waves in the hierarchical Bayesian framework,JCAP11(2024) 038 [2409.11103]

    work page arXiv 2024

  54. [56]

    Perot and N

    L. Perot and N. Chamel,Role of Quark Matter and Color Superconductivity in the Structure and Tidal Deformability of Strange Dwarfs,Universe9(2023) 382

    work page 2023

  55. [57]

    Yang, C.-M

    S.-H. Yang, C.-M. PI, X.-P. Zheng and F. Weber,Non-Newtonian Gravity in Strange Quark Stars and Constraints from the Observations of PSR J0740+6620 and GW170817,Astrophys. J.902(2020) 32 [1909.00933]. – 22 –

    work page arXiv 2020

  56. [58]

    Kumar, V.B

    A. Kumar, V.B. Thapa and M. Sinha,Compact star merger events with stars composed of interacting strange quark matter,Mon. Not. Roy. Astron. Soc.513(2022) 3788 [2204.11034]

    work page arXiv 2022

  57. [59]

    Fast spinning strange stars: possible ways to constrain interacting quark matter parameters

    S. Bhattacharyya, I. Bombaci, D. Logoteta and A.V. Thampan,Fast spinning strange stars: possible ways to constrain interacting quark matter parameters,Mon. Not. Roy. Astron. Soc. 457(2016) 3101 [1601.06120]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  58. [60]

    Yoshida and Y

    S. Yoshida and Y. Eriguchi,Rotating boson stars in general relativity,Phys. Rev. D56(1997) 762

    work page 1997

  59. [61]

    TOPICAL REVIEW: General relativistic boson stars

    F.E. Schunck and E.W. Mielke,General relativistic boson stars,Class. Quant. Grav.20 (2003) R301 [0801.0307]

    work page internal anchor Pith review Pith/arXiv arXiv 2003

  60. [62]

    Colpi, S.L

    M. Colpi, S.L. Shapiro and I. Wasserman,Boson Stars: Gravitational Equilibria of Selfinteracting Scalar Fields,Phys. Rev. Lett.57(1986) 2485

    work page 1986

  61. [63]

    Kaup,Klein-Gordon Geon,Phys

    D.J. Kaup,Klein-Gordon Geon,Phys. Rev.172(1968) 1331

    work page 1968

  62. [64]

    Mass-radius relation of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions: I. Analytical results

    P.-H. Chavanis,Mass-radius relation of Newtonian self-gravitating Bose-Einstein condensates with short-range interactions: I. Analytical results,Phys. Rev. D84(2011) 043531 [1103.2050]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  63. [65]

    Chavanis,Self-gravitating Bose-Einstein condensates and their connection to dark matter,Phys

    P.-H. Chavanis,Self-gravitating Bose-Einstein condensates and their connection to dark matter,Phys. Rev. D106(2022) 123014 [2209.03852]

    work page arXiv 2022

  64. [66]

    Stable Phases of Boson Stars

    B. Kleihaus, J. Kunz and S. Schneider,Stable Phases of Boson Stars,Phys. Rev. D85(2012) 024045 [1109.5858]

    work page internal anchor Pith review Pith/arXiv arXiv 2012

  65. [67]

    Models of rotating boson stars and geodesics around them: new type of orbits

    P. Grandclement, C. Somé and E. Gourgoulhon,Models of rotating boson stars and geodesics around them: new type of orbits,Phys. Rev. D90(2014) 024068 [1405.4837]

    work page internal anchor Pith review Pith/arXiv arXiv 2014

  66. [68]

    Vaglio, C

    M. Vaglio, C. Pacilio, A. Maselli and P. Pani,Multipolar structure of rotating boson stars, Phys. Rev. D105(2022) 124020 [2203.07442]

    work page arXiv 2022

  67. [69]

    Herdeiro, I

    C. Herdeiro, I. Perapechka, E. Radu and Y. Shnir,Asymptotically flat spinning scalar, Dirac and Proca stars,Phys. Lett. B797(2019) 134845 [1906.05386]

    work page arXiv 2019

  68. [70]

    The Physics of Neutron Stars

    J.M. Lattimer and M. Prakash,The physics of neutron stars,Science304(2004) 536 [astro-ph/0405262]

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  69. [71]

    Neutron Star Structure and the Equation of State

    J.M. Lattimer and M. Prakash,Neutron star structure and the equation of state,Astrophys. J. 550(2001) 426 [astro-ph/0002232]

    work page internal anchor Pith review Pith/arXiv arXiv 2001

  70. [72]

    Heintzmann and E

    H. Heintzmann and E. Hilf,Neutron star matter and neutron star models,Zeitschrift für Naturforschung A29(1974) 269–279

    work page 1974

  71. [73]

    Carr, A.M

    B. Carr, A.M. Green and F. Kuhnel,Primordial Black Holes as a Probe of Cosmology and High Energy Physics,Phys. Rept.1054(2024) 1 [2306.03903]

    work page arXiv 2024

  72. [74]

    Primordial Black Holes as a dark matter candidate

    A.M. Green and B.J. Kavanagh,Primordial Black Holes as a dark matter candidate,J. Phys. G48(2021) 043001 [2007.10722]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  73. [75]

    Hawking,Gravitationally collapsed objects of very low mass,Mon

    S. Hawking,Gravitationally collapsed objects of very low mass,Mon. Not. Roy. Astron. Soc. 152(1971) 75

    work page 1971

  74. [76]

    Carr and S.W

    B.J. Carr and S.W. Hawking,Black holes in the early Universe,Mon. Not. Roy. Astron. Soc. 168(1974) 399

    work page 1974

  75. [77]

    B. Carr, F. Kuhnel and L. Sandstad,Primordial Black Holes as Dark Matter,Phys. Rev. D 94(2016) 083504 [1607.06077]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  76. [78]

    Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914

    M. Sasaki, T. Suyama, T. Tanaka and S. Yokoyama,Primordial Black Hole Scenario for the Gravitational-Wave Event GW150914,Phys. Rev. Lett.117(2016) 061101 [1603.08338]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  77. [79]

    Y. Suwa, T. Yoshida, M. Shibata, H. Umeda and K. Takahashi,On the minimum mass of neutron stars,Mon. Not. Roy. Astron. Soc.481(2018) 3305 [1808.02368]. – 23 –

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  78. [80]

    Kacanja and A.H

    K. Kacanja and A.H. Nitz,A Search for Low-mass Neutron Stars in the Third Observing Run of Advanced LIGO and Virgo,Astrophys. J.984(2025) 61 [2412.05369]

    work page arXiv 2025

  79. [81]

    Relativistic tidal properties of neutron stars

    T. Damour and A. Nagar,Relativistic tidal properties of neutron stars,Phys. Rev. D80 (2009) 084035 [0906.0096]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  80. [82]

    SL(2,Z)-invariance and D-instanton contributions to the $D^6 R^4$ interaction

    E. Poisson,Tidal deformation of a slowly rotating black hole,Phys. Rev. D91(2015) 044004 [1404.2192]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

Showing first 80 references.