Pith. sign in

REVIEW 3 major objections 4 minor 2 cited by

Tidal Love numbers and quasi-normal modes of the ECO in a Dark Matter halo

T0 review · 3 major / 4 minor · reviewed 2026-08-15 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗ Review JSON

Pith's one-line read This paper derives first-order dark-matter corrections to the tidal Love numbers of an exotic compact object and shows that non-relativistic halos produce distinguishable gravitational-wave echoes.

desk verdict The paper cleanly extends the BH-Hernquist Love-number and echo framework to ECOs, but the central Love-number correction is underdetermined by an arbitrary f-rescaling; the truncated-halo and echo parts are the more solid contributions. read the letter →

arxiv 2509.03556 v1 pith:3YGLX5FT submitted 2025-09-03 gr-qc

Kabir Chakravarti , Chiranjeeb Singha This is my paper · ORCID
classification gr-qc
keywords tidalLovenumbersexoticcompactobjectsgravitationalwaveechoesdarkmatterhalosHernquistprofileRegge-Wheelerequationquasinormalmodesaxialandpolarperturbations
topics Dark Matter
open problems Dark Matter
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

An exotic compact object (ECO) is a black-hole mimicker with a reflective surface instead of a horizon, and this paper asks how a surrounding dark-matter halo changes its two most observable gravitational-wave signatures: the tidal Love number measured during inspiral and the echo train measured after merger. Working with two Hernquist-type halo profiles, one relativistic and one non-relativistic, the authors show perturbatively that the l=2 Love number is the vacuum ECO value plus a first-order correction linear in the dark-matter content, with explicit formulae for axial (Eq. 34) and polar (Eq. 40) perturbations. They also show that for odd-parity perturbations the non-relativistic halo moves the potential barrier outward and stretches the echo period, producing an echo train that is cleanly distinguishable from both the relativistic-halo case and the DM-free case, whereas the relativistic halo leaves echoes nearly identical to vacuum. If correct, this means gravitational-wave observations could in principle constrain dark-matter halo parameters around ECOs, although the numerical size of the Love-number correction inherits a length-scale ambiguity discussed in the paper.

What carries the argument

The machinery is a first-order perturbative split of the perturbation master variable, $X = X^{(0)} + k\,X^{(1)}$, around a spherically symmetric background with anisotropic pressure (zero radial pressure, non-zero tangential pressure). At zeroth order the two independent solutions are the vacuum axial and polar functions; the ECO boundary condition at $x = 1+\epsilon$ (reflecting surface with reflectivity $R=-1$) fixes their ratio through $\kappa(\epsilon)$, and the Love number is read off as the ratio of the coefficient of the growing external-field piece ($x^3$ axial, $x^2$ polar) to the decaying response piece ($1/x^2$ axial, $1/x^3$ polar). At first order, variation of parameters builds the particular solution $\phi$ from the halo source terms; matching across the halo cutoff $x=2$ (relativistic profile) or down to the ECO surface (non-relativistic profile) fixes the constants and yields the corrected Love numbers. For echoes, the same perturbations are promoted to time-dependent Regge-Wheeler modes with effective potential $V_{\rm eff} = f\,[\ell(\ell+1)/r^2 - 6m(r)/r^3 + 4\pi(\rho+4P_t)]$, evolved on a double-null grid, with the tortoise coordinate and potential-peak location controlling the echo period.

What would settle it

Solve the full $\ell=2$ axial and polar perturbation equations numerically for the same Hernquist halo parameters without expanding in $k$, and compare the Love numbers extracted from the exact large-$x$ asymptotics with Eq. (34) and Eq. (40) using the paper's $f$ choices; agreement is the only direct check, and disagreement at order $k$ would show that the corrected formula is not the limit of the exact theory.

Watch

Extended reading notes

Core claim

On the paper's own terms, the discovery is that dark-matter dressing of an ECO does not erase the ECO's tidal response but shifts it in a controlled way: the axial l=2 Love number is $k_2^a = k_2^{a0} + (k/5)\,[\ldots]$ and the polar one is $k_2^p = k_2^{p0} - (k/60)\,[\ldots]$, where $k$ is the small dark-matter parameter, $k_2^{a0,p0}$ are the vacuum ECO values set by the surface-basis coefficient $\kappa$, and the brackets contain halo-profile-dependent coefficients from the first-order particular solution. The same framework yields the echoes: with reflecting boundary conditions at the ECO surface, the Regge-Wheeler equation with an anisotropic-mass potential produces trains of pulses whose spacing is set by the tortoise-coordinate distance to the potential peak. For the relativistic halo profile the potential and hence the echo train are almost indistinguishable from Schwarzschild, while the non-relativistic profile shifts the peak to $\zeta \approx 100$ and gives an easily separated echo train (Fig. 4). A separate result is that truncated halos behave functionally like neutron stars, with Love numbers scaling as $(R_t^h/M_t^h)^5$, but with Love numbers of order $10^{40}$ to $10^{50}$, so they cannot be confused with neutron stars.

Load-bearing premise

The load-bearing premise is that the $1/k$ self-inconsistency in Eq. (41) can be cured by an arbitrary effective-length-scale rescaling $f$, with $f = 1/x_{DS}^2$ for the relativistic halo and $f = 2/\sqrt{x'_S}$ for the non-relativistic halo, since the numerical Love-number corrections depend on that choice.

Editorial extensions

If this is right

  • Inspiral phasing of ECO binaries in dark-matter halos acquires a dark-matter-dependent tidal contribution at first order in the DM parameter, so future detectors measuring tidal deformability could constrain halo density and scale length.
  • The non-relativistic halo's echo train is cleanly separated from both vacuum and relativistic-halo echo trains, giving ringdown echoes a concrete route to distinguishing halo profiles around ECOs.
  • The relativistic halo leaves the potential barrier and light ring effectively unchanged, so its echoes are nearly degenerate with the vacuum case; only the non-relativistic profile produces a visible signature.
  • At first order in $k$ the Love number contains no undetermined multiplicative constants, so parameter-estimation bias from this scheme enters only at second order.
  • Truncated halos mimic neutron stars functionally, with Love numbers scaling as $(R_h/M_h)^5$, but their huge Love numbers (roughly $10^{40}$ to $10^{50}$) keep them distinguishable from neutron stars.

Reading between the lines

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

  • If the arbitrary $f$ rescaling is a genuine ambiguity rather than a bookkeeping choice, then the Love-number predictions in Eqs. (34) and (40) are not unique; a future exact computation or a matched asymptotic treatment would be needed to fix the physical value, a point the paper notes but does not resolve.
  • The non-relativistic halo's shift of the light ring to $r_{\rm lr} \approx 3M(1 + M M_{\rm DM}/r_S^2)$ implies the ringdown frequency itself shifts by roughly ten percent for the paper's benchmark masses, suggesting that ringdown-only tests, not just echoes, may carry halo information.
  • A natural next step, not taken here, is a Bayesian parameter-estimation study over the echo waveform to determine which halo parameters are measurable and how strongly the $f$ ambiguity propagates into inferred dark-matter density.
  • The same perturbative machinery could be applied to rotating ECOs, where spin would couple halo-induced corrections to frame-dragging effects and possibly break the degeneracy between halo parameters and ECO surface reflectivity.
Share X Bluesky LinkedIn Reddit HN

Signed reviews

No signed human review yet.

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. The manuscript studies an exotic compact object (ECO) of mass M embedded in a Hernquist-type dark-matter halo, using the relativistic halo construction of [70] and the non-relativistic Einstein construction of [28]. For time-independent even- and odd-parity perturbations it derives formal expressions, Eqs. (34) and (40), for the l=2 tidal Love number as the vacuum ECO value plus a first-order correction proportional to the DM parameter k, and evaluates the required coefficients in Eqs. (41)-(43). For truncated halos it argues that Love numbers scale as (R/M)^5 and cannot be confused with neutron stars. For time-dependent odd-parity perturbations it evolves the Regge-Wheeler equation (48) in double-null coordinates and presents echo trains (Fig. 4) for vacuum, relativistic-halo, and non-relativistic-halo cases, concluding that the non-relativistic DM halo yields clearly distinguishable echoes.

Significance. If the Love-number formulas were well defined, the paper would supply a concrete prediction for environmental corrections to ECO tidal deformability, relevant for inspiral tests of compact-object nature and dark-matter environments. The echo calculation is a useful proof-of-concept for environment-dependent ringdown signatures, and the authors are transparent about the difficulty in Eq. (41). However, the central quantitative Love-number result is not uniquely defined because it depends on an underived rescaling parameter f, and the logarithmic term in the axial coefficient makes that coefficient cutoff dependent. These issues are load-bearing for the main claim, so the significance of the paper as a calculation of ECO-DM Love numbers is not currently established; the echo part remains an interesting numerical demonstration.

major comments (3)
  1. [§3.5, Eqs. (41)-(42)] The coefficients α^p_-3 and α^a_-2 in Eq. (41) carry explicit 1/k prefactors; with the natural identification k=1/p the displayed terms scale as 1/p and 1/p^2 rather than as first-order corrections, so the split X=X^(0)+kX^(1) in Eq. (11) is internally inconsistent. The paper acknowledges this and multiplies by f^3 or f^2 in Eq. (42), with f=1/x_DS^2 for the relativistic profile and f=2/sqrt(x'_S) for the non-relativistic profile. These choices are not derived from the model, and the numerical Love-number correction depends on them, so Eqs. (34) and (40) do not provide a unique prediction.
  2. [§3.5, Eq. (41), α^a_-2] The axial coefficient α^a_-2 contains a term proportional to log(x). Because the Love number is read off from the coefficient of 1/x^2 evaluated at x_B >> x'_S, this logarithmic contribution makes the extracted 1/x^2 coefficient depend on the arbitrary outer cutoff x_B unless the log term is shown to cancel or be absorbed into a renormalized coupling. The paper does not demonstrate such a cancellation, so the axial Love number in Eq. (34) is not well defined as stated.
  3. [§2, §3, and §5, Eqs. (7), (11), and Fig. 4 parameters] The small parameter of the perturbative expansion is not fixed consistently. The text says k is chosen as M_DM/r_S and that a realistic value is p∼10^-4, but with p=2M/M_DM this corresponds to k∼10^4 rather than a small parameter; moreover, the echo setup in Section 5 adopts M=20M_sun, M_DM=50M_sun, which gives p=0.8. Since the first-order Love-number correction in Eqs. (34) and (40) relies on a definite small expansion parameter, this ambiguity further undermines the central claim.
minor comments (4)
  1. [§3.3, Eq. (28)] The expansion κa(ϵ)=-ϵ+4(13/12+logϵ)ϵ^2+O(ϵ^2) has a remainder that should not be O(ϵ^2) after the explicit ϵ^2 term; the next-order remainder should be at least O(ϵ^3) (possibly with logarithms).
  2. [§3.4, Eq. (38)] Equation (38) writes κa(ϵ)=24ϵ^2+O(ϵ^3), but in the polar subsection this should be κp(ϵ); the superscript appears to be a typo.
  3. [§4, Fig. 2 and Love-number estimate] The estimate that truncated-halo Love numbers reach 10^40-10^50 is presented without explicitly stating the halo and ECO parameters used in Fig. 2; these parameters should be listed so the reader can reproduce the numerical magnitude.
  4. [§5, Eqs. (51)-(52), Fig. 4] The numerical echo evolution does not report grid resolution, domain size, or convergence tests; since the distinguishability claim for the non-relativistic halo is based on this numerical integration, at least a convergence check and the chosen step size should be stated.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the Love-number and echo derivations are genuine perturbative calculations, with an acknowledged scheme ambiguity that affects robustness but does not reduce outputs to inputs.

full rationale

The paper's central quantitative claims, Eqs. (34) and (40), are obtained by a genuine perturbative reduction: X = X^(0) + k X^(1), solving the first-order equation by variation of parameters, imposing ECO inner boundary conditions, matching across x = 2 for the relativistic profile, and taking outer asymptotic ratios. The vacuum ECO Love numbers are derived from the standard y1, y2 solutions and reflectivity boundary conditions, not assumed from the DM result. The DM-dependent corrections are linear combinations of the boundary coefficient mu, the matching coefficients chi, and particular-solution coefficients alpha; none of these is defined in terms of the final Love number. The echo calculation is an independent numerical evolution of the Regge-Wheeler equation with the effective potential of Eq. (49), benchmarked against the no-DM Schwarzschild barrier. The manuscript itself flags the main weakness: Eq. (41) contains 1/k and log(x) factors, making the first-order split apparently self-inconsistent, and Eq. (42) rescales the alpha coefficients using an arbitrary f = 2M/R chosen so that B^4 f^2 respects the perturbative ordering. This is a real scheme-dependence and omitted-derivation limitation, and it should be weighed in any robustness assessment of the numerical Love-number corrections. However, it is not circularity: f is not fitted to the target Love numbers and then renamed as a prediction, and the final formulas are not equivalent to the consistency condition by construction. The derivation is benchmarked against the external BH-Hernquist framework of Ref. [70], and self-citations such as Refs. [76] and [81] appear only as background. No load-bearing self-citation or by-construction reduction is present.

Assumptions & free parameters 3 free parameters · 5 assumptions · 0 invented entities

The central claims rest on the standard ECO boundary-condition picture, the Hernquist-halo background from [28,70], and a perturbative split inherited from [70]. The only genuinely ad hoc element is the f-rescaling introduced to fix the self-inconsistency of the quoted alpha coefficients. No new particles, forces, or exotic entities are introduced.

free parameters (3)
  • f = 2M/R (effective length-scale ratio) = 1/x_DS^2 (relativistic), 2/sqrt(x'_S) (non-relativistic)
    Introduced in Section 3.5 to remove the 1/k self-inconsistency in Eq. (41). The final Love-number corrections depend on this choice, and no independent physical constraint is given.
  • epsilon (ECO surface offset, r_epsilon = 2M(1+epsilon)) = small, unspecified
    Characterizes the ECO surface in Eq. (1). It determines kappa and hence the zero-DM Love numbers through Eqs. (28), (38), and (43).
  • Halo profile constants w, q, rho0 (and derived B^4) = values from Table I of [70]
    Enter through the density profile Eq. (6) and the asymptotic coefficient B^4 in Eq. (22). The paper reproduces these from [70] rather than deriving or measuring them.
assumptions (5)
  • domain assumption The background is static and spherically symmetric with line element ds^2/(2M)^2 = -e^{2N} dt_hat^2 + dx^2/g + x^2 dOmega^2 and energy-momentum T^mu_nu = diag(-rho, 0, Pt, Pt).
    Adopted from [28,70]. All perturbation equations, including the Love-number master equation and the Regge-Wheeler potential, assume this matter sector with vanishing radial pressure.
  • domain assumption An ECO is modeled by replacing the Schwarzschild horizon with a reflective surface at r = 2M(1+epsilon) with reflectivity R = -1.
    Used in Eq. (16) to relate the two independent perturbation solutions. This boundary condition is what produces nonzero Love numbers and echoes; no microphysical model of the ECO surface is provided.
  • domain assumption Perturbations can be decomposed as X = X0 + k X1 with k small, and the first-order source terms gamma and beta from [70] remain valid for the ECO-DM background.
    Equations (11)-(13) and the Appendix source terms. The entire Love-number calculation is built on this split and on the validity of those source terms.
  • domain assumption Asymptotic Love numbers are defined for observers inside the halo, at x_B >> x'_S where m(x) tends to M + M_DM and Mx >> m(x).
    Section 3, paragraph before Eq. (21). The matching to define the Love number uses the halo's total mass and ignores contributions beyond the arbitrary cutoff x_B.
  • ad hoc to paper The self-inconsistency in Eq. (41) is cured by choosing an arbitrary effective length scale R, with f = 2M/R, taking f = 1/x_DS^2 or f = 2/sqrt(x'_S).
    Equation (42) and surrounding text. No independent derivation is given, yet the numerical values of the Love-number corrections depend on this choice.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Tidal Love numbers and quasi-normal modes of the ECO in a Dark Matter halo." pith.science (2026). https://pith.science/paper/3YGLX5FT

@misc{pith2026250903556,
  author       = {Pith},
  title        = {Pith review of: Tidal Love numbers and quasi-normal modes of the ECO in a Dark Matter halo},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/3YGLX5FT}},
  note         = {Machine review of arXiv:2509.03556}
}
read the original abstract

It is well-known that exotic compact objects (ECOs) are a class of objects categorised as Black Hole (BH) mimickers. ECOs have been shown to possess signatures distinguishing them from BHs. However, in our universe, no object exists in complete isolation. Consequently, any compact object, whether a BH or an ECO, must reside within some environment that inevitably influences the surrounding spacetime geometry due to back-reaction. In this paper, we investigate a scenario where an ECO is embedded in an environment of dark matter (DM). In this work, we assume two different models of the DM halo profile. We compute the Love numbers and GW echoes of this composite system to assess the impact of the surrounding dark matter halo. To analyze the echoes, we focus on odd-parity perturbations, while for calculating the tidal Love numbers, we consider both even and odd parity perturbations. We aim to understand how the DM properties couple to the ECO signatures in the Love number or the GW-echo signal, both of which have a strong bearing as observables in future-generation detectors.

Figures

Figures reproduced from arXiv: 2509.03556 by the authors.

Figure 1
Figure 1. Radial profiles of the DM density ρ(x) (left) and mass m(x) for the non-relativistic and the relativistic DM formulations as a function of x = r/2M. The non-relativistic DM is taken from [28] while the relativistic one is from [70]. Also shown as vertical lines are three dimensionless parameters 1/p, xDS and x ′ S which are connected to three separate length-scales. in [PITH_FULL_IMAGE:figures/full_fig_p005_1.png] view at source ↗
Figure 2
Figure 2. This plot shows the scaling of the factor ( [PITH_FULL_IMAGE:figures/full_fig_p014_2.png] view at source ↗
Figure 3
Figure 3. Effective potential Veff from our chosen ECO-DM with relativistic and non-relativistic DM profiles plotted as a function of the tortoise radial coordinate r∗. The Schwarschild barrier is shown for reference. The cut-off of the relativistic DM at r/M = 4 appears as a small irregular feature. Note the displacement of the non-relativistic barrier. The gray shaded region on the far right is the inaccessible region below… view at source ↗
Figures from the paper (1 more)
Figure 4
Figure 4. Figure 4: This plot shows the GW-Echoes from our ECO-DM systems. The Schwarschild case represents [PITH_FULL_IMAGE:figures/full_fig_p017_4.png]

Discussion (0). Continue with ORCID to comment.

Forward citations

Cited by 2 Pith papers

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

  1. The Ringdown and the Tide: Fingerprints of Dark Matter Halo Profiles

    gr-qc 2026-08 conditional novelty 6.0 of 10

    For black holes in generalized (alpha,beta,gamma) dark matter halos, the axial ringdown shift is set by a single redshift integral, while the tidal Love number depends on an outer radial moment, making the two observa...

  2. Tidal deformation of an accreting compact object

    gr-qc 2026-07 conditional novelty 5.0 of 10

    For perfectly reflecting Schwarzschild-like ECOs, the log-compactness scaling of static scalar and spin-1 Love numbers survives a thin accretion disk, which mainly amplifies the response magnitude.

Reference graph

Works this paper leans on

80 extracted references · 6 canonical work pages · cited by 2 Pith papers

  1. [70]

    Tidal Love numbers and quasi-normal modes of the Schwarzschild-Hernquist black hole,

    S. Chakraborty, G. Comp` ere, and L. Machet, “Tidal Love numbers and quasi-normal modes of the Schwarzschild-Hernquist black hole,” arXiv:2412.14831 [gr-qc] . 24

    arXiv

  2. [28]

    Black holes in galaxies: Environmental impact on gravitational-wave generation and propagation,

    V. Cardoso, K. Destounis, F. Duque, R. P. Macedo, and A. Maselli, “Black holes in galaxies: Environmental impact on gravitational-wave generation and propagation,” Phys. Rev. D 105 no. 6, (2022) L061501, arXiv:2109.00005 [gr-qc]

    arXiv 2022

  3. [1]

    Observation of Gravitational Waves from a Binary Black Hole Merger,

    LIGO Scientific, Virgo Collaboration, 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]

    arXiv 2016

  4. [2]

    GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run,

    KAGRA, VIRGO, LIGO Scientific Collaboration, R. Abbott et al. , “GWTC-3: Compact Binary Coalescences Observed by LIGO and Virgo during the Second Part of the Third Observing Run,” Phys. Rev. X 13 no. 4, (2023) 041039, arXiv:2111.03606 [gr-qc]

    arXiv 2023

  5. [3]

    Tests of General Relativity with GWTC-3,

    LIGO Scientific, VIRGO, KAGRA Collaboration, R. Abbott et al. , “Tests of General Relativity with GWTC-3,” arXiv:2112.06861 [gr-qc]

    arXiv

  6. [4]

    Science Case for the Einstein Telescope,

    ET Collaboration, M. Maggiore et al. , “Science Case for the Einstein Telescope,” JCAP 03 (2020) 050, arXiv:1912.02622 [astro-ph.CO]

    arXiv 2020

  7. [5]

    LISA Definition Study Report,

    LISA Collaboration, M. Colpi et al. , “LISA Definition Study Report,” arXiv:2402.07571 [astro-ph.CO]

    arXiv

  8. [6]

    A Horizon Study for Cosmic Explorer: Science, Observatories, and Community,

    M. Evans et al. , “A Horizon Study for Cosmic Explorer: Science, Observatories, and Community,” arXiv:2109.09882 [astro-ph.IM]

    arXiv

Show all 80 references
  1. [7]

    Gravitational Radiation from Post-Newtonian Sources and Inspiralling Compact Binaries,

    L. Blanchet, “Gravitational Radiation from Post-Newtonian Sources and Inspiralling Compact Binaries,” Living Rev. Rel. 17 (2014) 2, arXiv:1310.1528 [gr-qc]

    2014 arXiv

  2. [8]

    Evolution of binary black hole spacetimes,

    F. Pretorius, “Evolution of binary black hole spacetimes,” Phys. Rev. Lett. 95 (2005) 121101, arXiv:gr-qc/0507014

    2005 arXiv

  3. [9]

    Testing general relativity with present and future astrophysical observations,

    E. Berti et al. , “Testing general relativity with present and future astrophysical observations,” Class. Quant. Grav. 32 (2015) 243001, arXiv:1501.07274 [gr-qc]

    2015 arXiv

  4. [10]

    New horizons for fundamental physics with LISA,

    LISA Collaboration, K. G. Arun et al. , “New horizons for fundamental physics with LISA,” Living Rev. Rel. 25 no. 1, (2022) 4, arXiv:2205.01597 [gr-qc]

    2022 arXiv

  5. [11]

    Axion cloud evaporation during inspiral of black hole binaries: The effects of backreaction and radiation,

    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] . 20

    2022 arXiv

  6. [12]

    Deci-Hz gravitational waves from the self-interacting axion cloud around a rotating stellar mass black hole,

    H. Omiya, T. Takahashi, T. Tanaka, and H. Yoshino, “Deci-Hz gravitational waves from the self-interacting axion cloud around a rotating stellar mass black hole,” Phys. Rev. D 110 no. 4, (2024) 044002, arXiv:2404.16265 [gr-qc]

    2024 arXiv

  7. [13]

    Can environmental effects spoil precision gravitational-wave astrophysics?,

    E. Barausse, V. Cardoso, and P. Pani, “Can environmental effects spoil precision gravitational-wave astrophysics?,” Phys. Rev. D 89 no. 10, (2014) 104059, arXiv:1404.7149 [gr-qc]

    2014 arXiv

  8. [14]

    Gravitational waves as a probe of dark matter minispikes,

    K. Eda, Y. Itoh, S. Kuroyanagi, and J. Silk, “Gravitational waves as a probe of dark matter minispikes,” Phys. Rev. Lett. 110 (2013) 221101, arXiv:1301.5971 [gr-qc]

    2013 arXiv

  9. [16]

    Probing the nature of dark matter with gravitational waves,

    O. S. Hannuksela et al. , “Probing the nature of dark matter with gravitational waves,” Phys. Rev. Lett. 123 (2019) 161102, arXiv:1906.11845 [astro-ph.CO]

    2019 arXiv

  10. [17]

    Black holes as particle detectors: evolution of superradiant instabilities,

    R. Brito, V. Cardoso, and P. Pani, “Black holes as particle detectors: evolution of superradiant instabilities,” Class. Quant. Grav. 32 no. 13, (2015) 134001, arXiv:1411.0686 [gr-qc]

    2015 arXiv

  11. [18]

    Binary pulsars as dark-matter probes,

    P. Pani, “Binary pulsars as dark-matter probes,” Phys. Rev. D 92 no. 12, (2015) 123530, arXiv:1512.01236 [astro-ph.HE]

    2015 arXiv

  12. [19]

    Quasinormal modes of relativistic stars and interacting fields,

    C. F. B. Macedo, V. Cardoso, L. C. B. Crispino, and P. Pani, “Quasinormal modes of relativistic stars and interacting fields,” Phys. Rev. D 93 no. 6, (2016) 064053, arXiv:1603.02095 [gr-qc]

    2016 arXiv

  13. [20]

    Gravitational-wave signatures of exotic compact objects and of quantum corrections at the horizon scale,

    V. Cardoso, S. Hopper, C. F. B. Macedo, C. Palenzuela, and P. Pani, “Gravitational-wave signatures of exotic compact objects and of quantum corrections at the horizon scale,” Phys. Rev. D 94 no. 8, (2016) 084031, arXiv:1608.08637 [gr-qc]

    2016 arXiv

  14. [21]

    Testing strong-field gravity with tidal Love numbers,

    V. Cardoso, E. Franzin, A. Maselli, P. Pani, and G. Raposo, “Testing strong-field gravity with tidal Love numbers,” Phys. Rev. D 95 no. 8, (2017) 084014, arXiv:1701.01116 [gr-qc] . [Addendum: Phys.Rev.D 95, 089901 (2017)]

    2017 arXiv

  15. [22]

    Tests for the existence of black holes through gravitational wave echoes,

    V. Cardoso and P. Pani, “Tests for the existence of black holes through gravitational wave echoes,” Nature Astron. 1 no. 9, (2017) 586–591, arXiv:1709.01525 [gr-qc]

    2017 arXiv

  16. [23]

    Probing the existence of ultralight bosons with a single gravitational-wave measurement,

    O. A. Hannuksela, K. W. K. Wong, R. Brito, E. Berti, and T. G. F. Li, “Probing the existence of ultralight bosons with a single gravitational-wave measurement,” Nature Astron. 3 no. 5, (2019) 447–451, arXiv:1804.09659 [astro-ph.HE]

    2019 arXiv

  17. [24]

    Ultralight boson cloud depletion in binary systems,

    E. Berti, R. Brito, C. F. B. Macedo, G. Raposo, and J. L. Rosa, “Ultralight boson cloud depletion in binary systems,” Phys. Rev. D 99 no. 10, (2019) 104039, arXiv:1904.03131 [gr-qc]

    2019 arXiv

  18. [25]

    Testing the nature of dark compact objects: a status report,

    V. Cardoso and P. Pani, “Testing the nature of dark compact objects: a status report,” Living Rev. Rel. 22 no. 1, (2019) 4, arXiv:1904.05363 [gr-qc]

    2019 arXiv

  19. [26]

    Detecting dark matter around black holes with gravitational waves: Effects of dark-matter dynamics on the gravitational waveform,

    B. J. Kavanagh, D. A. Nichols, G. Bertone, and D. Gaggero, “Detecting dark matter around black holes with gravitational waves: Effects of dark-matter dynamics on the gravitational waveform,” Phys. Rev. D 102 no. 8, (2020) 083006, arXiv:2002.12811 [gr-qc] . 21

    2020 arXiv

  20. [27]

    Probing dark matter spikes with gravitational-wave signals from extreme mass-ratio inspirals,

    A. Coogan, P. D. Lasky, T. L. Smith, and E. Thrane, “Probing dark matter spikes with gravitational-wave signals from extreme mass-ratio inspirals,” Phys. Rev. D 105 no. 2, (2022) 023009, arXiv:2111.06447 [astro-ph.CO]

    2022 arXiv

  21. [29]

    Love numbers and magnetic susceptibility of charged black holes,

    D. Pere˜ niguez and V. Cardoso, “Love numbers and magnetic susceptibility of charged black holes,” Phys. Rev. D 105 no. 4, (2022) 044026, arXiv:2112.08400 [gr-qc]

    2022 arXiv

  22. [30]

    Impact of relativistic corrections on the detectability of dark-matter spikes with gravitational waves,

    N. Speeney, A. Antonelli, V. Baibhav, and E. Berti, “Impact of relativistic corrections on the detectability of dark-matter spikes with gravitational waves,” Phys. Rev. D 106 no. 4, (2022) 044027, arXiv:2204.12508 [gr-qc]

    2022 arXiv

  23. [31]

    Modeling frequency-dependent tidal deformability for environmental black hole mergers,

    V. De Luca, A. Maselli, and P. Pani, “Modeling frequency-dependent tidal deformability for environmental black hole mergers,” Phys. Rev. D 107 no. 4, (2023) 044058, arXiv:2212.03343 [gr-qc]

    2023 arXiv

  24. [32]

    Gravitational-wave imprints of compact and galactic-scale environments in extreme-mass-ratio binaries,

    K. Destounis, A. Kulathingal, K. D. Kokkotas, and G. O. Papadopoulos, “Gravitational-wave imprints of compact and galactic-scale environments in extreme-mass-ratio binaries,” Phys. Rev. D 107 no. 8, (2023) 084027, arXiv:2210.09357 [gr-qc]

    2023 arXiv

  25. [33]

    Constraining properties of asymmetric dark matter candidates from gravitational-wave observations,

    D. Singh, A. Gupta, E. Berti, S. Reddy, and B. S. Sathyaprakash, “Constraining properties of asymmetric dark matter candidates from gravitational-wave observations,” Phys. Rev. D 107 no. 8, (2023) 083037, arXiv:2210.15739 [gr-qc]

    2023 arXiv

  26. [34]

    Comparing accretion disks and dark matter spikes in intermediate mass ratio inspirals,

    N. Becker and L. Sagunski, “Comparing accretion disks and dark matter spikes in intermediate mass ratio inspirals,” Phys. Rev. D 107 no. 8, (2023) 083003, arXiv:2211.05145 [gr-qc]

    2023 arXiv

  27. [35]

    Nonlinearities in the tidal Love numbers of black holes,

    V. De Luca, J. Khoury, and S. S. C. Wong, “Nonlinearities in the tidal Love numbers of black holes,” Phys. Rev. D 108 no. 2, (2023) 024048, arXiv:2305.14444 [gr-qc]

    2023 arXiv

  28. [36]

    Parametrized Love numbers of nonrotating black holes,

    T. Katagiri, T. Ikeda, and V. Cardoso, “Parametrized Love numbers of nonrotating black holes,” Phys. Rev. D 109 no. 4, (2024) 044067, arXiv:2310.19705 [gr-qc]

    2024 arXiv

  29. [37]

    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]

    2023 arXiv

  30. [38]

    Black holes surrounded by generic dark matter profiles: Appearance and gravitational-wave emission,

    E. Figueiredo, A. Maselli, and V. Cardoso, “Black holes surrounded by generic dark matter profiles: Appearance and gravitational-wave emission,” Phys. Rev. D 107 no. 10, (2023) 104033, arXiv:2303.08183 [gr-qc]

    2023 arXiv

  31. [39]

    Relativistic drag forces on black holes from scalar dark matter clouds of all sizes,

    D. Traykova, R. Vicente, K. Clough, T. Helfer, E. Berti, P. G. Ferreira, and L. Hui, “Relativistic drag forces on black holes from scalar dark matter clouds of all sizes,” Phys. Rev. D 108 no. 12, (2023) L121502, arXiv:2305.10492 [gr-qc]

    2023 arXiv

  32. [40]

    Secondary accretion of dark matter in intermediate mass-ratio inspirals: Dark-matter dynamics and gravitational-wave phase,

    D. A. Nichols, B. A. Wade, and A. M. Grant, “Secondary accretion of dark matter in intermediate mass-ratio inspirals: Dark-matter dynamics and gravitational-wave phase,” Phys. Rev. D 108 no. 12, (2023) 124062, arXiv:2309.06498 [gr-qc] . 22

    2023 arXiv

  33. [41]

    Extreme mass-ratio inspirals into black holes surrounded by scalar clouds,

    R. Brito and S. Shah, “Extreme mass-ratio inspirals into black holes surrounded by scalar clouds,” Phys. Rev. D 108 no. 8, (2023) 084019, arXiv:2307.16093 [gr-qc] . [Erratum: Phys.Rev.D 110, 109902 (2024)]

    2023 arXiv

  34. [42]

    Black-hole spectroscopy: quasinormal modes, ringdown stability and the pseudospectrum,

    K. Destounis and F. Duque, “Black-hole spectroscopy: quasinormal modes, ringdown stability and the pseudospectrum,” 8, 2023. arXiv:2308.16227 [gr-qc]

    2023 arXiv

  35. [43]

    Extreme-Mass-Ratio Inspirals in Ultralight Dark Matter,

    F. Duque, C. F. B. Macedo, R. Vicente, and V. Cardoso, “Extreme-Mass-Ratio Inspirals in Ultralight Dark Matter,” Phys. Rev. Lett. 133 no. 12, (2024) 121404, arXiv:2312.06767 [gr-qc]

    2024 arXiv

  36. [44]

    Black holes surrounded by generic matter distributions: Polar perturbations and energy flux,

    N. Speeney, E. Berti, V. Cardoso, and A. Maselli, “Black holes surrounded by generic matter distributions: Polar perturbations and energy flux,” Phys. Rev. D 109 no. 8, (2024) 084068, arXiv:2401.00932 [gr-qc]

    2024 arXiv

  37. [45]

    First constraints on binary black hole environments with LIGO-Virgo observations,

    G. C. Santoro, S. Roy, R. Vicente, M. Haney, O. J. Piccinni, W. Del Pozzo, and M. Martinez, “First constraints on binary black hole environments with LIGO-Virgo observations,” PoS EPS-HEP2023 (2024) 068

    2024

  38. [46]

    Relativistic aerodynamics of spinning black holes,

    C. Dyson, J. Redondo-Yuste, M. van de Meent, and V. Cardoso, “Relativistic aerodynamics of spinning black holes,” Phys. Rev. D 109 no. 10, (2024) 104038, arXiv:2402.07981 [gr-qc]

    2024 arXiv

  39. [47]

    Accreting Schwarzschild-like compact object: Plasma-photon interaction and stability,

    A. Chowdhury, S. Biswas, and S. Chakraborty, “Accreting Schwarzschild-like compact object: Plasma-photon interaction and stability,” Phys. Rev. D 110 no. 6, (2024) 064072, arXiv:2405.04006 [gr-qc]

    2024 arXiv

  40. [48]

    Probing the quantum nature of black holes with ultralight boson environments,

    S. Mitra, S. Chakraborty, R. Vicente, and J. C. Feng, “Probing the quantum nature of black holes with ultralight boson environments,” Phys. Rev. D 110 no. 8, (2024) 084012, arXiv:2312.06783 [gr-qc]

    2024 arXiv

  41. [49]

    Dark matter, black holes, and gravitational waves,

    G. Bertone, “Dark matter, black holes, and gravitational waves,” Nucl. Phys. B 1003 (2024) 116487, arXiv:2404.11513 [astro-ph.CO]

    2024 arXiv

  42. [50]

    Dynamical friction from self-interacting dark matter,

    M. S. Fischer and L. Sagunski, “Dynamical friction from self-interacting dark matter,” Astron. Astrophys. 690 (2024) A299, arXiv:2405.19392 [astro-ph.CO]

    2024 arXiv

  43. [51]

    Probing dark-matter effects with gravitational waves using the parametrized post-Einsteinian framework,

    E. Wilcox, D. A. Nichols, and K. Yagi, “Probing dark-matter effects with gravitational waves using the parametrized post-Einsteinian framework,” Phys. Rev. D 110 no. 12, (2024) 124009, arXiv:2409.10846 [gr-qc]

    2024 arXiv

  44. [52]

    Impact of a plasma on the relaxation of black holes,

    E. Cannizzaro, T. F. M. Spieksma, V. Cardoso, and T. Ikeda, “Impact of a plasma on the relaxation of black holes,” Phys. Rev. D 110 no. 2, (2024) L021302, arXiv:2405.05315 [gr-qc]

    2024 arXiv

  45. [53]

    Dark Matter,

    M. Cirelli, A. Strumia, and J. Zupan, “Dark Matter,” arXiv:2406.01705 [hep-ph]

    arXiv

  46. [54]

    Measurable parameter combinations of environmentally-dephased EMRI gravitational-wave signals,

    M. I. B. Rivera and R. C. Reyes, “Measurable parameter combinations of environmentally-dephased EMRI gravitational-wave signals,” New Astron. 112 (2024) 102263, arXiv:2406.15971 [gr-qc]

    2024 arXiv

  47. [55]

    Phenomenology of ultralight bosons around compact objects: In-medium suppression,

    E. Cannizzaro and T. F. M. Spieksma, “Phenomenology of ultralight bosons around compact objects: In-medium suppression,” Phys. Rev. D 110 no. 8, (2024) 084021, arXiv:2406.17016 [hep-ph]. 23

    2024 arXiv

  48. [56]

    Deciphering the Instability of the Black Hole Ringdown Quasinormal Spectrum,

    A. Ianniccari, A. J. Iovino, A. Kehagias, P. Pani, G. Perna, D. Perrone, and A. Riotto, “Deciphering the Instability of the Black Hole Ringdown Quasinormal Spectrum,” Phys. Rev. Lett. 133 no. 21, (2024) 211401, arXiv:2407.20144 [gr-qc]

    2024 arXiv

  49. [57]

    Black hole spectroscopy in environments: detectability prospects,

    T. F. M. Spieksma, V. Cardoso, G. Carullo, M. Della Rocca, and F. Duque, “Black hole spectroscopy in environments: detectability prospects,” arXiv:2409.05950 [gr-qc]

    arXiv

  50. [58]

    The dynamical response of viscous objects to gravitational waves,

    V. Boyanov, V. Cardoso, K. D. Kokkotas, and J. Redondo-Yuste, “The dynamical response of viscous objects to gravitational waves,” arXiv:2411.16861 [gr-qc]

    arXiv

  51. [59]

    Tidal Love numbers and approximate universal relations for fermion soliton stars,

    E. Berti, V. De Luca, L. Del Grosso, and P. Pani, “Tidal Love numbers and approximate universal relations for fermion soliton stars,” Phys. Rev. D 109 no. 12, (2024) 124008, arXiv:2404.06979 [gr-qc]

    2024 arXiv

  52. [60]

    Tidal Love numbers and Green’s functions in black hole spacetimes,

    V. De Luca, A. Garoffolo, J. Khoury, and M. Trodden, “Tidal Love numbers and Green’s functions in black hole spacetimes,” Phys. Rev. D 110 no. 6, (2024) 064081, arXiv:2407.07156 [gr-qc]

    2024 arXiv

  53. [61]

    Flea on the elephant: Tidal Love numbers in subsolar primordial black hole searches,

    V. De Luca, G. Franciolini, and A. Riotto, “Flea on the elephant: Tidal Love numbers in subsolar primordial black hole searches,” Phys. Rev. D 110 no. 10, (2024) 104041, arXiv:2408.14207 [gr-qc]

    2024 arXiv

  54. [62]

    Tidal deformability of black holes surrounded by thin accretion disks,

    E. Cannizzaro, V. De Luca, and P. Pani, “Tidal deformability of black holes surrounded by thin accretion disks,” Phys. Rev. D 110 no. 12, (2024) 123004, arXiv:2408.14208 [astro-ph.HE]

    2024

  55. [63]

    Probing dark matter halo profiles with multi-band observations of gravitational waves,

    D. Tahelyani, A. Bhattacharyya, and A. S. Sengupta, “Probing dark matter halo profiles with multi-band observations of gravitational waves,” arXiv:2411.14063 [gr-qc]

    arXiv

  56. [64]

    On relativistic dynamical tides: subtleties and calibration,

    T. Katagiri, K. Yagi, and V. Cardoso, “On relativistic dynamical tides: subtleties and calibration,” arXiv:2409.18034 [gr-qc]

    arXiv

  57. [65]

    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

    1999 arXiv

  58. [66]

    Dark matter distributions around massive black holes: A general relativistic analysis,

    L. Sadeghian, F. Ferrer, and C. M. Will, “Dark matter distributions around massive black holes: A general relativistic analysis,” Phys. Rev. D 88 no. 6, (2013) 063522, arXiv:1305.2619 [astro-ph.GA]

    2013 arXiv

  59. [67]

    Dark matter spikes in the vicinity of Kerr black holes,

    F. Ferrer, A. M. da Rosa, and C. M. Will, “Dark matter spikes in the vicinity of Kerr black holes,” Phys. Rev. D 96 no. 8, (2017) 083014, arXiv:1707.06302 [astro-ph.CO]

    2017 arXiv

  60. [68]

    New probe of dark-matter properties: Gravitational waves from an intermediate-mass black hole embedded in a dark-matter minispike,

    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. D 91 no. 4, (2015) 044045, arXiv:1408.3534 [gr-qc]

    2015 arXiv

  61. [69]

    Gravitational Waves from Extreme-Mass-Ratio Systems in Astrophysical Environments,

    V. Cardoso, K. Destounis, F. Duque, R. Panosso Macedo, and A. Maselli, “Gravitational Waves from Extreme-Mass-Ratio Systems in Astrophysical Environments,” Phys. Rev. Lett. 129 no. 24, (2022) 241103, arXiv:2210.01133 [gr-qc]

    2022 arXiv

  62. [71]

    Is the gravitational-wave ringdown a probe of the event horizon?,

    V. Cardoso, E. Franzin, and P. Pani, “Is the gravitational-wave ringdown a probe of the event horizon?,” Phys. Rev. Lett. 116 no. 17, (2016) 171101, arXiv:1602.07309 [gr-qc] . [Erratum: Phys.Rev.Lett. 117, 089902 (2016)]

    2016 arXiv

  63. [72]

    A recipe for echoes from exotic compact objects,

    Z. Mark, A. Zimmerman, S. M. Du, and Y. Chen, “A recipe for echoes from exotic compact objects,” Phys. Rev. D 96 no. 8, (2017) 084002, arXiv:1706.06155 [gr-qc]

    2017 arXiv

  64. [73]

    Characterization of echoes: A Dyson-series representation of individual pulses,

    M. R. Correia and V. Cardoso, “Characterization of echoes: A Dyson-series representation of individual pulses,” Phys. Rev. D 97 no. 8, (2018) 084030, arXiv:1802.07735 [gr-qc]

    2018 arXiv

  65. [74]

    Echoes of Kerr-like wormholes,

    P. Bueno, P. A. Cano, F. Goelen, T. Hertog, and B. Vercnocke, “Echoes of Kerr-like wormholes,” Phys. Rev. D 97 no. 2, (2018) 024040, arXiv:1711.00391 [gr-qc]

    2018 arXiv

  66. [75]

    Echoes from the Abyss: Tentative evidence for Planck-scale structure at black hole horizons,

    J. Abedi, H. Dykaar, and N. Afshordi, “Echoes from the Abyss: Tentative evidence for Planck-scale structure at black hole horizons,” Phys. Rev. D 96 no. 8, (2017) 082004, arXiv:1612.00266 [gr-qc]

    2017 arXiv

  67. [76]

    Signature of nonuniform area quantization on black hole echoes,

    K. Chakravarti, R. Ghosh, and S. Sarkar, “Signature of nonuniform area quantization on black hole echoes,” Phys. Rev. D 105 no. 4, (2022) 044046, arXiv:2112.10109 [gr-qc]

    2022 arXiv

  68. [77]

    Galactic wormholes: Geometry, stability, and echoes,

    S. Biswas, C. Singha, and S. Chakraborty, “Galactic wormholes: Geometry, stability, and echoes,” Phys. Rev. D 109 no. 6, (2024) 064043, arXiv:2307.04836 [gr-qc]

    2024 arXiv

  69. [78]

    An Analytical Model for Spherical Galaxies and Bulges,

    L. Hernquist, “An Analytical Model for Spherical Galaxies and Bulges,” Astrophys. J. 356 (June,

  70. [79]

    Tidal Love numbers of neutron stars,

    T. Hinderer, “Tidal Love numbers of neutron stars,” Astrophys. J. 677 (2008) 1216–1220, arXiv:0711.2420 [astro-ph] . [Erratum: Astrophys.J. 697, 964 (2009)]

    2008 arXiv

  71. [80]

    Gravitational-wave signal from binary neutron stars: a systematic analysis of the spectral properties,

    L. Rezzolla and K. Takami, “Gravitational-wave signal from binary neutron stars: a systematic analysis of the spectral properties,” Phys. Rev. D 93 no. 12, (2016) 124051, arXiv:1604.00246 [gr-qc]

    2016 arXiv

  72. [81]

    Signatures of extra dimensions in gravitational waves from black hole quasinormal modes,

    S. Chakraborty, K. Chakravarti, S. Bose, and S. SenGupta, “Signatures of extra dimensions in gravitational waves from black hole quasinormal modes,” Phys. Rev. D 97 no. 10, (2018) 104053, arXiv:1710.05188 [gr-qc] . 25

    2018 arXiv

Pith tools

Reviewed August 15, 2026 · model on record in the stance chip above.