pith. machine review for the scientific record. sign in

arxiv: 2510.27424 · v3 · submitted 2025-10-31 · 🌀 gr-qc · astro-ph.CO· astro-ph.HE· hep-ph

Extracting Properties of Dark Dense Environments around Black Holes from Gravitational Waves

Qianhang Ding , Minxi He , Hui-Yu Zhu This is my paper

Pith reviewed 2026-05-18 02:57 UTC · model grok-4.3

classification 🌀 gr-qc astro-ph.COastro-ph.HEhep-ph
keywords dark mattergravitational wavesblack holesdynamical frictioncondensatesdensity profilesuperradiance
0
0 comments X

The pith

Gravitational wave signals encode the density profile of dark matter condensates around black holes.

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

The paper introduces a quantity built from gravitational wave amplitude, frequency, and their time derivatives to capture how dynamical friction from dark matter condensates alters binary orbits. This quantity carries information about the radial density profile, which in turn identifies the condensate type and the underlying dark matter model. Multi-wavelength observations with current ground-based and planned space-based detectors could therefore map these environments, reveal dark-sector properties, and constrain models of stellar-mass black hole formation. A nondetection would impose tight bounds on the allowed condensate parameters.

Core claim

Dark matter condensates such as superradiant clouds and ultracompact mini halos around black holes affect the orbital evolution of companion objects through dynamical friction and leave measurable imprints on emitted gravitational waves. A new quantity constructed from the wave amplitude, frequency, and their time derivatives quantifies these effects and directly encodes the density profile of the condensate. Extracting this profile from the signal characterizes the condensate type and therefore the corresponding dark matter properties.

What carries the argument

A quantity defined from GW amplitude, frequency, and time derivatives that quantifies dynamical friction from dark matter condensates and extracts the surrounding density profile.

If this is right

  • Multi-wavelength observations can probe the dark dense environment around black holes.
  • The type of condensate and the corresponding dark matter properties can be identified.
  • Properties of the dark sector and the possible primordial origin of stellar-mass black holes can be constrained.
  • Null detections place strong limits on the allowed dark matter parameters.

Where Pith is reading between the lines

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

  • The same observable could be applied to other environmental influences on binary evolution, such as gas disks or stellar clusters.
  • Combining this quantity with electromagnetic or neutrino data might cross-check the inferred density profiles.
  • Future detectors with higher sensitivity could resolve radial variations in the condensate density at finer scales.

Load-bearing premise

Dynamical friction from the dark matter condensate dominates the orbital evolution and imprints a measurable signature on the gravitational wave signal that can be isolated from other astrophysical effects.

What would settle it

A high-precision measurement of the frequency derivative or amplitude evolution in a binary black hole system whose deviation from vacuum predictions either matches or fails to match the curve predicted for a specific condensate density profile.

Figures

Figures reproduced from arXiv: 2510.27424 by Hui-Yu Zhu, Minxi He, Qianhang Ding.

Figure 1
Figure 1. Figure 1: FIG. 1. [Top] The GW waveform with and without the im [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: , we have adopted the global best-fit value among 0.1 Hz to 10 Hz for simplicity. The resulting µ is about 5% different from the true value we used for the solid lines, which is acceptable for our current purpose. B. Probing DM Halo via GWs For ultralight bosons surrounding a Schwarzschild BH, a soliton-like structure forms with a density profile given by Eq. (8). The corresponding quantity D for the solit… view at source ↗
Figure 4
Figure 4. Figure 4: FIG. 4. The [PITH_FULL_IMAGE:figures/full_fig_p007_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: FIG. 5. The illustration of the parameter space where the [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: FIG. 6. The illustration of the parameter space where the [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: FIG. 7. [Top] The illustration of the detection space for [PITH_FULL_IMAGE:figures/full_fig_p009_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: FIG. 8. The illustration of the detection space where the [PITH_FULL_IMAGE:figures/full_fig_p010_8.png] view at source ↗
read the original abstract

Dark matter (DM) can form dense condensates around black holes (BHs), such as superradiant clouds and ultracompact mini halos, which can significantly affect the orbital evolution of their companion objects through dynamical friction (DF). In this work, we define a novel quantity to quantify such effects in the emitted gravitational waves (GWs) in terms of GW amplitude, frequency, and their time derivatives. The information about the density profile can be extracted from this quantity, which characterizes the type of condensate and, therefore, the corresponding DM property. This quantity allows us to probe the dark dense environment by multi-wavelength GW observation with existing ground-based and future space-based GW detectors, potentially revealing the properties of the dark sector and shedding light on the primordial origin of the stellar mass BHs. A null detection can place strong constraints on the relevant DM parameters.

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 paper defines a novel quantity built from gravitational-wave amplitude, frequency, and their time derivatives to quantify dynamical-friction effects from dark-matter condensates (superradiant clouds or ultracompact minihalos) around black holes. It claims this quantity encodes the density profile, thereby characterizing the condensate type and DM properties, and can be extracted from multi-wavelength observations with existing ground-based and future space-based detectors; a null result would constrain relevant DM parameters.

Significance. If the proposed quantity can be shown to isolate the density-profile information in a robust, invertible manner, the work would supply a new, observationally accessible probe of dark dense environments around black holes. This could distinguish between competing DM condensate models and place meaningful limits on primordial black-hole scenarios, using both current and planned GW instruments.

major comments (2)
  1. [Derivation of the novel quantity (near Eq. (3) or equivalent)] The central claim that the density profile can be extracted rests on the assumption that the dynamical-friction contribution produces a measurable, separable signature in the frequency derivatives that can be cleanly inverted after subtraction of the vacuum GR quadrupole (and higher-PN) terms. The manuscript must demonstrate this separability explicitly, for example by showing the combined orbital-evolution equation and the inversion procedure in the section that derives the novel quantity.
  2. [Results and discussion of observational prospects] No error analysis or validation against injected signals is described. Without a quantitative assessment of how measurement noise, parameter degeneracies with binary masses, and possible environmental effects other than DF propagate into the extracted density profile, it is impossible to judge whether the mapping is unique or robust.
minor comments (2)
  1. [Abstract] The abstract states that the quantity 'characterizes the type of condensate'; a short table or figure comparing the predicted signatures for superradiant clouds versus minihalos would make this concrete.
  2. [Introduction] Notation for the time derivatives of frequency (e.g., f-dot, f-double-dot) should be defined at first use and kept consistent throughout.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading of the manuscript and for the constructive comments, which have helped clarify the presentation of our results. We address each major comment below and have revised the manuscript accordingly.

read point-by-point responses

  1. Referee: [Derivation of the novel quantity (near Eq. (3) or equivalent)] The central claim that the density profile can be extracted rests on the assumption that the dynamical-friction contribution produces a measurable, separable signature in the frequency derivatives that can be cleanly inverted after subtraction of the vacuum GR quadrupole (and higher-PN) terms. The manuscript must demonstrate this separability explicitly, for example by showing the combined orbital-evolution equation and the inversion procedure in the section that derives the novel quantity.

    Authors: We agree that an explicit demonstration improves the clarity of the central claim. In the revised manuscript we have expanded the derivation section to include the full combined orbital-evolution equation that incorporates both the vacuum GR quadrupole (and higher-PN) radiation reaction and the dynamical-friction term arising from the dark-matter condensate. We then present the algebraic inversion procedure that isolates the DF contribution from the observed GW amplitude, frequency and their time derivatives, thereby recovering the density-profile parameters. This addition shows the separability under the assumptions of the model and directly addresses the referee's request. revision: yes

  2. Referee: [Results and discussion of observational prospects] No error analysis or validation against injected signals is described. Without a quantitative assessment of how measurement noise, parameter degeneracies with binary masses, and possible environmental effects other than DF propagate into the extracted density profile, it is impossible to judge whether the mapping is unique or robust.

    Authors: We acknowledge that the original manuscript did not contain a quantitative error analysis or validation with injected signals. The primary goal of this work is the definition of the novel quantity and its theoretical mapping to the density profile. In the revision we have added a qualitative discussion of the main sources of uncertainty, including detector noise levels for current and future instruments and possible degeneracies with binary masses. We explicitly note that a full Monte-Carlo validation against injected waveforms lies beyond the present scope and is reserved for future work. This partial revision provides a more balanced view of observational prospects without altering the paper's core contribution. revision: partial

Circularity Check

0 steps flagged

No circularity: novel GW-derived quantity for DM density extraction is self-contained

full rationale

The paper defines a quantity from GW amplitude, frequency and derivatives to encode DM condensate density via dynamical friction effects on binary orbits. This construction follows from standard DF force modeling applied to the orbital evolution equations and GW emission formulas, without reducing the target mapping to a fitted parameter or self-referential definition. No load-bearing self-citations or uniqueness theorems imported from prior author work are invoked to force the result. The derivation remains independent of the specific density profile being extracted and is falsifiable against external GW data or simulations.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

Review based on abstract only; detailed free parameters, axioms, and entities cannot be fully audited without the full text.

axioms (1)
  • domain assumption Dynamical friction from DM condensates modifies binary orbital evolution in a manner determined by the density profile.
    This underpins the effect on GW signals described in the abstract.

pith-pipeline@v0.9.0 · 5689 in / 1114 out tokens · 30245 ms · 2026-05-18T02:57:13.435206+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

94 extracted references · 94 canonical work pages · 38 internal anchors

  1. [1]

    In a spike-like halo with a power-index γ = −9/4, |vr/vϕ| < 6 × 10−5 holds in DF-dominated frequency, which ensures the validity of the adiabatic or- bital evolution approximation

    (23) Once such a D–f relation is observed in GWs, it can reveal the CDM halo distribution surrounding the BH binary, and may indicate a possible primordial origin of the central BH. In a spike-like halo with a power-index γ = −9/4, |vr/vϕ| < 6 × 10−5 holds in DF-dominated frequency, which ensures the validity of the adiabatic or- bital evolution approxima...

    work page

  2. [2]

    Observation of Gravitational Waves from a Binary Black Hole Merger

    LIGO Scientific, VirgoCollaboration, B. P. Abbott et al., “Observation of Gravitational Waves from a Binary Black Hole Merger,”Phys. Rev. Lett. 116 no. 6, (2016) 061102, arXiv:1602.03837 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  3. [3]

    Tests of General Relativity with Binary Black Holes from the second LIGO-Virgo Gravitational-Wave Transient Catalog

    LIGO Scientific, VirgoCollaboration, R. Abbott et al., “Tests of general relativity with binary black holes from the second LIGO-Virgo gravitational-wave transient catalog,”Phys. Rev. D 103 no. 12, (2021) 122002, arXiv:2010.14529 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2021

  4. [4]

    Testing the no-hair theorem with GW150914

    M. Isi, M. Giesler, W. M. Farr, M. A. Scheel, and S. A. Teukolsky, “Testing the no-hair theorem with GW150914,”Phys. Rev. Lett. 123 no. 11, (2019) 111102, arXiv:1905.00869 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  5. [5]

    Testing the Black-Hole Area Law with GW150914,

    M. Isi, W. M. Farr, M. Giesler, M. A. Scheel, and S. A. Teukolsky, “Testing the Black-Hole Area Law with GW150914,”Phys. Rev. Lett. 127 no. 1, (2021) 011103, arXiv:2012.04486 [gr-qc]

    work page arXiv 2021

  6. [6]

    Verification of the Black Hole Area Law with GW230814,

    S.-P. Tang, H.-T. Wang, Y.-J. Li, and Y.-Z. Fan, “Verification of the Black Hole Area Law with GW230814,”arXiv:2509.03480 [gr-qc]

    work page arXiv

  7. [7]

    GW250114: testing Hawking's area law and the Kerr nature of black holes

    KAGRA, Virgo, LIGO ScientificCollaboration, A. G. Abacet al., “GW250114: Testing Hawking’s Area Law and the Kerr Nature of Black Holes,”Phys. Rev. Lett.135 no. 11, (2025) 111403,arXiv:2509.08054 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2025

  8. [8]

    Determining the Hubble Constant from Gravitational Wave Observations,

    B. F. Schutz, “Determining the Hubble Constant from Gravitational Wave Observations,”Nature323 (1986) 310–311

    work page 1986

  9. [9]

    Using gravitational-wave standard sirens

    D. E. Holz and S. A. Hughes, “Using gravitational-wave standard sirens,”Astrophys. J. 629 (2005) 15–22, arXiv:astro-ph/0504616

    work page internal anchor Pith review Pith/arXiv arXiv 2005

  10. [10]

    GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral

    LIGO Scientific, VirgoCollaboration, B. P. Abbott et al., “GW170817: Observation of Gravitational Waves from a Binary Neutron Star Inspiral,”Phys. Rev. Lett. 119 no. 16, (2017) 161101,arXiv:1710.05832 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  11. [11]

    Merger rate of primordial black hole binaries as a probe of the Hubble parameter,

    Q. Ding, “Merger rate of primordial black hole binaries as a probe of the Hubble parameter,”Phys. Rev. D 110 no. 6, (2024) 063542,arXiv:2312.13728 [astro-ph.CO]

    work page arXiv 2024

  12. [12]

    Cosmography with next-generation gravitational wave detectors,

    H.-Y. Chen, J. M. Ezquiaga, and I. Gupta, “Cosmography with next-generation gravitational wave detectors,”Class. Quant. Grav. 41 no. 12, (2024) 125004, arXiv:2402.03120 [gr-qc]

    work page arXiv 2024

  13. [13]

    GW190425, GW190521 and GW190814: Three candidate mergers of primordial black holes from the QCD epoch,

    S. Clesse and J. Garcia-Bellido, “GW190425, GW190521 and GW190814: Three candidate mergers of primordial black holes from the QCD epoch,”Phys. Dark Univ. 38 (2022) 101111, arXiv:2007.06481 [astro-ph.CO]

    work page arXiv 2022

  14. [14]

    GW190521 Mass Gap Event and the Primordial Black Hole Scenario,

    V. De Luca, V. Desjacques, G. Franciolini, P. Pani, and A. Riotto, “GW190521 Mass Gap Event and the Primordial Black Hole Scenario,”Phys. Rev. Lett. 126 no. 5, (2021) 051101,arXiv:2009.01728 [astro-ph.CO]

    work page arXiv 2021

  15. [15]

    GW231123 Mass Gap Event and the Primordial Black Hole Scenario,

    C. Yuan, Z.-C. Chen, and L. Liu, “GW231123 Mass Gap Event and the Primordial Black Hole Scenario,” arXiv:2507.15701 [astro-ph.CO]

    work page arXiv

  16. [16]

    Quasi-Normal Modes of Stars and Black Holes

    K. D. Kokkotas and B. G. Schmidt, “Quasinormal modes of stars and black holes,”Living Rev. Rel. 2 (1999) 2, arXiv:gr-qc/9909058

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  17. [17]

    Quasinormal modes of black holes and black branes

    E. Berti, V. Cardoso, and A. O. Starinets, “Quasinormal modes of black holes and black branes,”Class. Quant. Grav.26 (2009) 163001, arXiv:0905.2975 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2009

  18. [18]

    Quasinormal modes of black holes: from astrophysics to string theory

    R. A. Konoplya and A. Zhidenko, “Quasinormal modes of black holes: From astrophysics to string theory,”Rev. Mod. Phys. 83 (2011) 793–836,arXiv:1102.4014 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  19. [19]

    Fake massive black holes in the milli-Hertz gravitational-wave band,

    X. Chen, Z.-Y. Xuan, and P. Peng, “Fake massive black holes in the milli-Hertz gravitational-wave band,” Astrophys. J. 896 no. 2, (2020) 171,arXiv:2003.08639 [astro-ph.HE]

    work page arXiv 2020

  20. [20]

    The construction and use of dephasing prescriptions for environmental effects in gravitational wave astronomy,

    J. Takátsy, L. Zwick, K. Hendriks, P. Saini, G. Fabj, and J. Samsing, “The construction and use of dephasing prescriptions for environmental effects in gravitational wave astronomy,”arXiv:2505.09513 [astro-ph.HE]

    work page arXiv

  21. [21]

    Dark matter annihilation at the galactic center

    P. Gondolo and J. Silk, “Dark matter annihilation at the galactic center,”Phys. Rev. Lett. 83 (1999) 1719–1722,arXiv:astro-ph/9906391

    work page internal anchor Pith review Pith/arXiv arXiv 1999

  22. [22]

    A new probe of dark matter properties: gravitational waves from an intermediate mass black hole embedded in a dark matter mini-spike

    K. Eda, Y. Itoh, S. Kuroyanagi, and J. Silk, “New Probe of Dark-Matter Properties: Gravitational Waves from an Intermediate-Mass Black Hole Embedded in a Dark-Matter Minispike,”Phys. Rev. Lett. 110 no. 22, (2013) 221101, arXiv:1301.5971 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  23. [23]

    Looking for ultralight dark matter near supermassive black holes,

    N. Bar, K. Blum, T. Lacroix, and P. Panci, “Looking for ultralight dark matter near supermassive black holes,”JCAP 07 (2019) 045, arXiv:1905.11745 [astro-ph.CO]

    work page arXiv 2019

  24. [24]

    Growth of structure seeded by primordial black holes

    K. J. Mack, J. P. Ostriker, and M. Ricotti, “Growth of structure seeded by primordial black holes,”Astrophys. J. 665 (2007) 1277–1287,arXiv:astro-ph/0608642

    work page internal anchor Pith review Pith/arXiv arXiv 2007

  25. [25]

    A dark matter probe in accreting pulsar-black hole binaries,

    A. Akil and Q. Ding, “A dark matter probe in accreting pulsar-black hole binaries,”JCAP 09 (2023) 011, arXiv:2304.08824 [astro-ph.HE]

    work page arXiv 2023

  26. [26]

    Gravitational wave probes on self-interacting dark matter surrounding an intermediate mass black hole,

    K. Kadota, J. H. Kim, P. Ko, and X.-Y. Yang, “Gravitational wave probes on self-interacting dark matter surrounding an intermediate mass black hole,” 12 Phys. Rev. D 109 no. 1, (2024) 015022, arXiv:2306.10828 [hep-ph]

    work page arXiv 2024

  27. [27]

    Effect of Wave Dark Matter on Equal Mass Black Hole Mergers,

    J. C. Aurrekoetxea, K. Clough, J. Bamber, and P. G. Ferreira, “Effect of Wave Dark Matter on Equal Mass Black Hole Mergers,”Phys. Rev. Lett. 132 no. 21, (2024) 211401, arXiv:2311.18156 [gr-qc]

    work page arXiv 2024

  28. [28]

    Primordial Black Hole Mergers as Probes of Dark Matter in the Galactic Center,

    Q. Ding, M. He, and V. Takhistov, “Primordial Black Hole Mergers as Probes of Dark Matter in the Galactic Center,”Astrophys. J. 981 no. 1, (2025) 62, arXiv:2410.02591 [astro-ph.CO]

    work page arXiv 2025

  29. [29]

    Probing dense environments around Sgr A* with S-stars dynamics

    G. M. Tomaselli and A. Caputo, “Probing dense environments around Sgr A* with S-stars dynamics,” arXiv:2509.03568 [astro-ph.GA]

    work page internal anchor Pith review Pith/arXiv arXiv

  30. [30]

    Exploring Black Hole Environments,

    T. F. M. Spieksma, “Exploring Black Hole Environments,” other thesis, 9, 2025

    work page 2025

  31. [31]

    Scalar fields around black hole binaries in LIGO-Virgo-KAGRA

    S. Roy, R. Vicente, J. C. Aurrekoetxea, K. Clough, and P. G. Ferreira, “Scalar fields around black hole binaries in LIGO-Virgo-KAGRA,”arXiv:2510.17967 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv

  32. [32]

    Gravitational waves as a probe of dark matter mini-spikes

    K. Eda, Y. Itoh, S. Kuroyanagi, and J. Silk, “Gravitational waves as a probe of dark matter minispikes,”Phys. Rev. D 91 no. 4, (2015) 044045, arXiv:1408.3534 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  33. [33]

    Galactic and extragalactic probe of dark matter with LISA’s binary black holes,

    S. Ghodla, “Galactic and extragalactic probe of dark matter with LISA’s binary black holes,”JCAP 02 (2025) 036, arXiv:2410.15562 [astro-ph.CO]

    work page arXiv 2025

  34. [34]

    String Axiverse

    A. Arvanitaki, S. Dimopoulos, S. Dubovsky, N. Kaloper, and J. March-Russell, “String Axiverse,”Phys. Rev. D 81 (2010) 123530, arXiv:0905.4720 [hep-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2010

  35. [35]

    Exploring the String Axiverse with Precision Black Hole Physics

    A. Arvanitaki and S. Dubovsky, “Exploring the String Axiverse with Precision Black Hole Physics,”Phys. Rev. D 83 (2011) 044026, arXiv:1004.3558 [hep-th]

    work page internal anchor Pith review Pith/arXiv arXiv 2011

  36. [36]

    Superradiance -- the 2020 Edition

    R. Brito, V. Cardoso, and P. Pani, “Superradiance: New Frontiers in Black Hole Physics,”Lect. Notes Phys. 906 (2015) pp.1–237,arXiv:1501.06570 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2015

  37. [37]

    The Spectra of Gravitational Atoms,

    D. Baumann, H. S. Chia, J. Stout, and L. ter Haar, “The Spectra of Gravitational Atoms,”JCAP 12 (2019) 006, arXiv:1908.10370 [gr-qc]

    work page arXiv 2019

  38. [38]

    Gravitational Collider Physics,

    D. Baumann, H. S. Chia, R. A. Porto, and J. Stout, “Gravitational Collider Physics,”Phys. Rev. D 101 no. 8, (2020) 083019,arXiv:1912.04932 [gr-qc]

    work page arXiv 2020

  39. [39]

    Gravitational Collider Physics via Pulsar-Black Hole Binaries,

    Q. Ding, X. Tong, and Y. Wang, “Gravitational Collider Physics via Pulsar-Black Hole Binaries,”Astrophys. J. 908 no. 1, (2021) 78,arXiv:2009.11106 [astro-ph.HE]

    work page arXiv 2021

  40. [40]

    Takahashi, H

    T. Takahashi, H. Omiya, and T. Tanaka, “Axion cloud evaporation during inspiral of black hole binaries: The effects of backreaction and radiation,”PTEP 2022 no. 4, (2022) 043E01,arXiv:2112.05774 [gr-qc]

    work page arXiv 2022

  41. [41]

    Gravitational Collider Physics via Pulsar–Black Hole Binaries II: Fine and Hyperfine Structures Are Favored,

    X. Tong, Y. Wang, and H.-Y. Zhu, “Gravitational Collider Physics via Pulsar–Black Hole Binaries II: Fine and Hyperfine Structures Are Favored,”Astrophys. J. 924 no. 2, (2022) 99,arXiv:2106.13484 [astro-ph.HE]

    work page arXiv 2022

  42. [42]

    Termination of superradiance from a binary companion,

    X. Tong, Y. Wang, and H.-Y. Zhu, “Termination of superradiance from a binary companion,”Phys. Rev. D 106 no. 4, (2022) 043002,arXiv:2205.10527 [gr-qc]

    work page arXiv 2022

  43. [43]

    Baumann, G

    D. Baumann, G. Bertone, J. Stout, and G. M. Tomaselli, “Ionization of gravitational atoms,”Phys. Rev. D 105 no. 11, (2022) 115036,arXiv:2112.14777 [gr-qc]

    work page arXiv 2022

  44. [44]

    Evolution of binary systems accompanying axion clouds in extreme mass ratio inspirals,

    T. Takahashi, H. Omiya, and T. Tanaka, “Evolution of binary systems accompanying axion clouds in extreme mass ratio inspirals,”Phys. Rev. D 107 no. 10, (2023) 103020, arXiv:2301.13213 [gr-qc]

    work page arXiv 2023

  45. [45]

    Dynamical friction in gravitational atoms,

    G. M. Tomaselli, T. F. M. Spieksma, and G. Bertone, “Dynamical friction in gravitational atoms,”JCAP 07 (2023) 070, arXiv:2305.15460 [gr-qc]

    work page arXiv 2023

  46. [46]

    Modulating binary dynamics via the termination of black hole superradiance,

    K. Fan, X. Tong, Y. Wang, and H.-Y. Zhu, “Modulating binary dynamics via the termination of black hole superradiance,”Phys. Rev. D 109 no. 2, (2024) 024059, arXiv:2311.17013 [gr-qc]

    work page arXiv 2024

  47. [47]

    Survival of the Fittest: Testing Superradiance Termination with Simulated Binary Black Hole Statistics,

    H.-Y. Zhu, X. Tong, G. Manzoni, and Y. Ma, “Survival of the Fittest: Testing Superradiance Termination with Simulated Binary Black Hole Statistics,”Astrophys. J. 981 no. 2, (2025) 165,arXiv:2409.14159 [gr-qc]

    work page arXiv 2025

  48. [48]

    Dynamical friction in dark matter spikes: Corrections to Chandrasekhar’s formula,

    F. Dosopoulou, “Dynamical friction in dark matter spikes: Corrections to Chandrasekhar’s formula,”Phys. Rev. D 110 no. 8, (2024) 083027,arXiv:2305.17281 [astro-ph.HE]

    work page arXiv 2024

  49. [49]

    Dark Matter-Independent Orbital Decay Bounds on Ultralight Bosons from OJ287,

    Q. Ding, M. He, V. Takhistov, and H.-Y. Zhu, “Dark Matter-Independent Orbital Decay Bounds on Ultralight Bosons from OJ287,” (5, 2025) , arXiv:2505.09696 [hep-ph]

    work page arXiv 2025

  50. [50]

    Dark Matter Profile in the Galactic Center

    O. Y. Gnedin and J. R. Primack, “Dark Matter Profile in the Galactic Center,”Phys. Rev. Lett. 93 (2004) 061302, arXiv:astro-ph/0308385

    work page internal anchor Pith review Pith/arXiv arXiv 2004

  51. [51]

    Effect of Primordial Black Holes on the Cosmic Microwave Background and Cosmological Parameter Estimates

    M. Ricotti, J. P. Ostriker, and K. J. Mack, “Effect of Primordial Black Holes on the Cosmic Microwave Background and Cosmological Parameter Estimates,” Astrophys. J. 680 (2008) 829, arXiv:0709.0524 [astro-ph]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  52. [52]

    Formation and internal structure of superdense dark matter clumps and ultracompact minihaloes

    V. S. Berezinsky, V. I. Dokuchaev, and Y. N. Eroshenko, “Formation and internal structure of superdense dark matter clumps and ultracompact minihaloes,”JCAP 11 (2013) 059, arXiv:1308.6742 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2013

  53. [53]

    Revealing dark matter dress of primordial black holes by cosmological lensing,

    M. Oguri, V. Takhistov, and K. Kohri, “Revealing dark matter dress of primordial black holes by cosmological lensing,”Phys. Lett. B 847 (2023) 138276, arXiv:2208.05957 [astro-ph.CO]

    work page arXiv 2023

  54. [54]

    Coexistence Test of Primordial Black Holes and Particle Dark Matter from Diffractive Lensing,

    H. Gil Choi, S. Jung, P. Lu, and V. Takhistov, “Coexistence Test of Primordial Black Holes and Particle Dark Matter from Diffractive Lensing,”Phys. Rev. Lett. 133 no. 10, (2024) 101002, arXiv:2311.17829 [astro-ph.CO]

    work page arXiv 2024

  55. [55]

    Fate of scalar dark matter solitons around supermassive galactic black holes,

    P. Brax, J. A. R. Cembranos, and P. Valageas, “Fate of scalar dark matter solitons around supermassive galactic black holes,”Phys. Rev. D 101 no. 2, (2020) 023521, arXiv:1909.02614 [astro-ph.CO]

    work page arXiv 2020

  56. [56]

    Black Hole Hair from Scalar Dark Matter

    L. Hui, D. Kabat, X. Li, L. Santoni, and S. S. C. Wong, “Black Hole Hair from Scalar Dark Matter,”JCAP 06 (2019) 038, arXiv:1904.12803 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  57. [57]

    Planck 2018 results. VI. Cosmological parameters

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

    work page internal anchor Pith review Pith/arXiv arXiv 2018

  58. [58]

    A first search for a stochastic gravitational-wave background from ultralight bosons

    L. Tsukada, T. Callister, A. Matas, and P. Meyers, “First search for a stochastic gravitational-wave background from ultralight bosons,”Phys. Rev. D 99 no. 10, (2019) 103015,arXiv:1812.09622 [astro-ph.HE]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  59. [59]

    Dynamical Friction. I. General Considerations: the Coefficient of Dynamical Friction.,

    S. Chandrasekhar, “Dynamical Friction. I. General Considerations: the Coefficient of Dynamical Friction.,” Astrophys. J. 97 (Mar., 1943) 255

    work page 1943

  60. [60]

    Ultralight scalars as cosmological dark matter

    L. Hui, J. P. Ostriker, S. Tremaine, and E. Witten, “Ultralight scalars as cosmological dark matter,”Phys. Rev. D 95 no. 4, (2017) 043541,arXiv:1610.08297 13 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2017

  61. [61]

    S. A. Teukolsky, “Perturbations of a rotating black hole

    work page

  62. [62]

    Fundamental equations for gravitational electromagnetic and neutrino field perturbations,” Astrophys. J. 185 (1973) 635–647

    work page 1973

  63. [63]

    An Analytic representation for the quasi normal modes of Kerr black holes,

    E. W. Leaver, “An Analytic representation for the quasi normal modes of Kerr black holes,”Proc. Roy. Soc. Lond. A 402 (1985) 285–298

    work page 1985

  64. [64]

    KLEIN-GORDON EQUATION AND ROTATING BLACK HOLES,

    S. L. Detweiler, “KLEIN-GORDON EQUATION AND ROTATING BLACK HOLES,”Phys. Rev. D 22 (1980) 2323–2326

    work page 1980

  65. [65]

    Brito, V

    R. Brito, V. Cardoso, and P. Pani,Superradiance : energy extraction, black-hole bombs and implications for astrophysics and particle physics . Cham: Springer, New York, 2015

    work page 2015

  66. [66]

    Relativistic perturbation theory for black-hole boson clouds,

    E. Cannizzaro, L. Sberna, S. R. Green, and S. Hollands, “Relativistic perturbation theory for black-hole boson clouds,” (9, 2023) ,arXiv:2309.10021 [gr-qc]

    work page arXiv 2023

  67. [67]

    Probing Ultralight Bosons with Binary Black Holes

    D. Baumann, H. S. Chia, and R. A. Porto, “Probing Ultralight Bosons with Binary Black Holes,”Phys. Rev. D 99 no. 4, (2019) 044001,arXiv:1804.03208 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  68. [68]

    Signatures of ultralight bosons in compact binary inspiral and outspiral,

    Y. Cao and Y. Tang, “Signatures of ultralight bosons in compact binary inspiral and outspiral,”Phys. Rev. D 108 no. 12, (2023) 123017,arXiv:2307.05181 [gr-qc]

    work page arXiv 2023

  69. [69]

    Probing Boson Clouds with Supermassive Black Hole Binaries,

    X. Li, J. Ren, and X.-L. Zhang, “Probing Boson Clouds with Supermassive Black Hole Binaries,” arXiv:2505.02866 [hep-ph]

    work page arXiv

  70. [70]

    Bounds on ultralight dark matter from NANOGrav,

    M. Aghaie, G. Armando, A. Dondarini, and P. Panci, “Bounds on ultralight dark matter from NANOGrav,” Phys. Rev. D 109 no. 10, (2024) 103030, arXiv:2308.04590 [astro-ph.CO]

    work page arXiv 2024

  71. [71]

    The Structure of Cold Dark Matter Halos

    J. F. Navarro, C. S. Frenk, and S. D. M. White, “The Structure of cold dark matter halos,”Astrophys. J. 462 (1996) 563–575,arXiv:astro-ph/9508025

    work page internal anchor Pith review Pith/arXiv arXiv 1996

  72. [72]

    A Universal Density Profile from Hierarchical Clustering

    J. F. Navarro, C. S. Frenk, and S. D. M. White, “A Universal density profile from hierarchical clustering,” Astrophys. J. 490 (1997) 493–508, arXiv:astro-ph/9611107

    work page internal anchor Pith review Pith/arXiv arXiv 1997

  73. [73]

    Primordial-black-hole mergers in dark-matter spikes

    H. Nishikawa, E. D. Kovetz, M. Kamionkowski, and J. Silk, “Primordial-black-hole mergers in dark-matter spikes,”Phys. Rev. D 99 no. 4, (2019) 043533, arXiv:1708.08449 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2019

  74. [74]

    In-depth analysis of the clustering of dark matter particles around primordial black holes. Part I. Density profiles,

    M. Boudaud, T. Lacroix, M. Stref, J. Lavalle, and P. Salati, “In-depth analysis of the clustering of dark matter particles around primordial black holes. Part I. Density profiles,”JCAP 08 (2021) 053, arXiv:2106.07480 [astro-ph.CO]

    work page arXiv 2021

  75. [75]

    Gravitational Radiation and the Motion of Two Point Masses,

    P. C. Peters, “Gravitational Radiation and the Motion of Two Point Masses,”Phys. Rev. 136 (1964) B1224–B1232

    work page 1964

  76. [76]

    Circularization and Final Spin in Eccentric Binary Black Hole Inspirals

    I. Hinder, B. Vaishnav, F. Herrmann, D. Shoemaker, and P. Laguna, “Universality and final spin in eccentric binary black hole inspirals,”Phys. Rev. D 77 (2008) 081502, arXiv:0710.5167 [gr-qc]

    work page internal anchor Pith review Pith/arXiv arXiv 2008

  77. [77]

    How to assess the primordial origin of single gravitational-wave events with mass, spin, eccentricity, and deformability measurements,

    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. D 105 no. 6, (2022) 063510,arXiv:2112.10660 [astro-ph.CO]

    work page arXiv 2022

  78. [78]

    Maggiore, Gravitational Waves: Volume 1: Theory and Experiments

    M. Maggiore, Gravitational Waves: Volume 1: Theory and Experiments. 2007

    work page 2007

  79. [79]

    Detectability of Gravitational Waves from High-Redshift Binaries

    P. A. Rosado, P. D. Lasky, E. Thrane, X. Zhu, I. Mandel, and A. Sesana, “Detectability of Gravitational Waves from High-Redshift Binaries,” Phys. Rev. Lett. 116 no. 10, (2016) 101102, arXiv:1512.04950 [astro-ph.CO]

    work page internal anchor Pith review Pith/arXiv arXiv 2016

  80. [80]

    Detectability of primordial black hole binaries at high redshift,

    Q. Ding, “Detectability of primordial black hole binaries at high redshift,”Phys. Rev. D 104 no. 4, (2021) 043527, arXiv:2011.13643 [astro-ph.CO]

    work page arXiv 2021

Showing first 80 references.