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Impact of flavor condensate dark matter on accretion disk luminosity in spherical spacetimes

T0 review · 2 major / 6 minor · reviewed 2026-08-06 · deepseek-v4-flash

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Pith's one-line read Flavor-condensate dark matter changes black hole accretion disks enough to be observable.

desk verdict The disk-luminosity calculations are transparent, but the claimed FCDM derivation collapses in Appendix A and one reported ISCO contradicts the junction setup. read the letter →

arxiv 2507.03758 v1 pith:LCAVM7NH submitted 2025-07-04 gr-qc astro-ph.CO

Antonio Capolupo , Orlando Luongo , Aniello Quaranta This is my paper · ORCID
classification gr-qcastro-ph.CO MSC 83C5783C1083C25 PACS 95.35.+d04.70.-s98.62.Mw
keywords flavorcondensatedarkmatterYukawagravitationalpotentialaccretiondiskluminosityinnermoststablecircularorbitneutrinomassmixingSchwarzschildspacetimethinhalo
topics 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

Dark matter made of a neutrino flavor condensate is argued to leave a measurable imprint on black hole accretion. The condensate's energy density, $\varepsilon(r)=\varepsilon_0(1+2V(r))$, yields a Yukawa correction $V(r)=-\alpha m\,e^{-r/\delta}/r$ to the Newtonian potential, which changes the geodesics around the black hole. Using a standard thin-disk accretion model, the paper finds that the innermost stable circular orbit and the disk's flux, temperature, and spectral luminosity all deviate from the pure Schwarzschild case. For the parameter choices considered, the inner edge can move from roughly 30 au to 25-142 au, and the high-frequency luminosity is generally suppressed, which the authors propose as a way to tell condensate dark matter apart from other dark matter candidates and modified-gravity models.

What carries the argument

The load-bearing object is the linearized condensate density $\varepsilon(r)=\varepsilon_0(1+2V(r))$, derived from the flavor-vacuum expectation value of the energy-momentum tensor. Inserted into the Poisson equation $\frac{1}{r^2}\partial_r(r^2\partial_r V)=4\pi\varepsilon$, it reduces to $U''-U/\delta^2=0$ with $U=r(1+2V)$ and $\delta=1/\sqrt{8\pi\varepsilon_0}$; the decaying solution is $V(r)=C e^{-r/\delta}/r$, written as $-\alpha m e^{-r/\delta}/r$. The paper builds the spacetime by adding $2\tilde{V}$ to the Schwarzschild metric functions outside a junction radius $r_b=6M_{\rm BH}$, shifting the potential by a constant to maintain continuity, which is equivalent to replacing the mass by $M_{\rm BH}(1+\alpha e^{-r/\delta})$ outside $r_b$. This mass function enters the circular-orbit energy and angular momentum, and through the thin-disk flux integral it determines the luminosity and spectral changes.

What would settle it

Solve the Poisson equation in Appendix A without discarding the constant term (allow $V$ to tend to a nonzero constant at infinity) and recompute the ISCO; if the effective mass is no longer $M_{\rm BH}(1+\alpha e^{-r/\delta})$, the claimed luminosity shifts do not follow. Observationally, a precise continuum measurement of the inner disk edge for an accreting black hole of known mass would test the predicted ISCO location, e.g. about 63 au rather than 30 au for $\alpha=-0.92$.

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Extended reading notes

Core claim

The central claim is that a fermionic condensate generated by neutrino mass mixing behaves as a pressureless dark matter fluid whose energy density is linearly tied to the gravitational potential, $\varepsilon(r)=\varepsilon_0(1+2V(r))$, and that this relation, solved through the Poisson equation in a static spherical weak-field background, produces the Yukawa potential $V(r)=-\alpha m\,e^{-r/\delta}/r$. Matching the resulting exterior metric to a Schwarzschild interior at $r_b=6M_{\rm BH}$ gives an effective mass $m(r)=M_{\rm BH}(1+\alpha e^{-r/\delta})$ outside the junction. Circular geodesics in this metric shift the innermost stable circular orbit relative to Schwarzschild, and the standard thin-disk integrals then yield non-negligible changes in radiative flux and spectral luminosity. The authors conclude that high-precision observations of accretion disk spectra could probe whether dark matter is a particle fluid, a condensate, or a symptom of extended gravity.

Load-bearing premise

The derivation depends on $\varepsilon(r)=\varepsilon_0(1+2V(r))$ and on dropping the constant term that the Poisson solution allows; if that step is not legitimate, the pure Yukawa form and the resulting luminosity predictions lose their derivation.

Editorial extensions

If this is right

  • The innermost stable circular orbit becomes a function of the Yukawa parameters: negative $\alpha$ with $\delta\sim\mathrm{kpc}$ moves it inward (25.4 au for $\alpha=-0.2$) and slightly raises the inner flux, while large negative $\alpha$ moves it outward (63.1 au for $\alpha=-0.92$; 142.2 au for $\alpha=-0.98$) and suppresses the inner disk.
  • The effective mass formula outside $r_b$ links accretion-scale observables to halo-scale parameters, so galactic rotation-curve constraints on $\alpha$ and $\delta$ can be cross-checked against black hole disk spectra.
  • The model returns exactly the Schwarzschild result when $\alpha=0$, giving a built-in null test for the dark matter correction.
  • Except for the small-negative case, the spectral luminosity is reduced mainly at high frequencies, giving the condensate a characteristic broadband signature compared with the standard disk.

Reading between the lines

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

  • The same effective-mass trick could be applied to rotating backgrounds; if spin is added, ISCO shifts are likely to mix with spin-induced shifts, so separating the dark matter signal would require joint fits of spin and $(\alpha,\delta)$.
  • Because modified-gravity models produce the same Yukawa form with different derivations, a single luminosity curve may be degenerate; distinguishing candidates probably requires combining disk spectra with independent halo measurements such as rotation curves.
  • The assumed purely baryonic accretion flow is an idealization; if condensate dark matter also contributes to the flow, the static-envelope approximation and the computed luminosity would need revision.
  • The junction radius $r_b=6M_{\rm BH}$ is not derived; a self-consistent relativistic solution of the full field equations inside the envelope would test whether ISCO shifts inside $r_b$ (as for $\alpha=-0.2$) are real or an artifact of the piecewise matching.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 6 minor

Summary. The paper studies thin accretion disks around a Schwarzschild black hole surrounded by a 'flavor condensate dark matter' (FCDM) envelope. The authors claim that the condensate energy density, through the relation ε(r)=ε0(1+2V(r)) and the Poisson equation, generates a Yukawa correction V(r)=−αm e^{−r/δ}/r to the Newtonian potential. They join this weak-field potential to the Schwarzschild metric at r_b=6M_BH, compute circular geodesics, the ISCO, and the Novikov–Thorne disk luminosity for several choices of α and δ, and report shifts of the ISCO and non-negligible deviations in the disk luminosity relative to the pure Schwarzschild case. The central claim is that accretion disk spectra could probe the condensate nature of dark matter.

Significance. If the FCDM origin of the Yukawa potential were established, the paper would connect a particle-physics-inspired dark matter model to observable accretion disk quantities, and the parameter study would be a useful phenomenological step. The Novikov–Thorne machinery is standard and is applied in a straightforward way, and the comparison of the resulting density profile with NFW, Burkert, Einasto, and Sofue profiles in Fig. 1 is illustrative. However, the key theoretical derivation in Appendix A is mathematically inconsistent, and one of the reported ISCO values contradicts the piecewise metric used in the paper. These are load-bearing issues: without the corrected derivation, the paper is not an FCDM-based prediction but merely a phenomenological study of an ad hoc Yukawa perturbation, whose parameter values are imported from galaxy-scale fits with no demonstrated connection to accretion-disk scales.

major comments (2)
  1. [Appendix A, Eq. (A6)] The Poisson equation with the density-potential relation ε(r)=ε0(1+2V(r)) does not admit the claimed Yukawa solution V(r)=−αm e^{−r/δ}/r with V(∞)=0. Setting W=1+2V and δ^2=1/(8πε0), Eq. (A6) becomes W''+(2/r)W'−W/δ^2=0, whose general solution is W=Ae^{−r/δ}/r+Be^{r/δ}/r. The boundary condition V(∞)=0 requires W(∞)=1, but the decaying branch tends to 0 and the growing branch is excluded by asymptotic flatness. The 'additive constant' discarded after Eq. (A7) is not a gauge freedom: it is forced by the ε0 source term, and dropping it changes g_tt=1+2V, which is physical. Consequently, Eq. (7) is not a consequence of Eq. (5), and the FCDM origin of the Yukawa correction and of the subsequent luminosity deviations is not established.
  2. [Section V, case 3] For the parameter choice α=−0.2, δ=δ2=10 kpc, the paper reports r_ISCO,2=25.370 au, which lies inside the junction radius r_b=6M_BH≈29.96 au. In the region r≤r_b the metric is exactly Schwarzschild by Eqs. (10), (13), and (14), so the ISCO there must be 6M_BH. The reported value is therefore inconsistent with the piecewise metric defined in the paper, and the associated claim that this parameter choice shifts the ISCO inward and enhances the radiative flux is not supported by the model as stated.
minor comments (6)
  1. [Fig. 5 caption] The caption says the radiative flux is plotted 'as a function of t', but the horizontal axis is labeled r/M_BH; this should be corrected to 'as a function of r'.
  2. [Section V, Eq. (21)] The value 6M_BH is reported as 29.598 au, but for M_BH=4.993 au the correct product is 29.958 au; please check this arithmetic and the corresponding values elsewhere.
  3. [After Eq. (6)] There is a typo: 'ε0 increseas with Λ' should read 'ε0 increases with Λ'.
  4. [Section V, case 5] The sentence 'The value of α is determined from is a rather extreme negative value' is grammatically garbled and should be rewritten.
  5. [Section V, Eq. (21c)] The mass accretion rate is given as Mdot=10^5 without specifying units; since Eq. (18) is dimensional, please clarify the units or state that the scaled quantities are independent of this value.
  6. [Section III] The metric functions in Eqs. (13) and (14) have discontinuous first derivatives at r_b, which would imply a distributional source at the junction; the authors should either justify the weak-field approximation in this regard or comment on the physical interpretation of the junction.

Circularity Check

2 steps flagged · score 6.0 of 10

The Yukawa potential is not derived in Appendix A; it is imported from the authors' prior FCDM work, so the central 'prediction' reduces to a self-cited ansatz.

  1. other [Appendix A, Eqs. (A6)-(A7)]
    "V ′′ + 2 r V ′ − 4πε0(1 + 2V ) = 0 . (A6) ... The positive root must be discarded to ensure V (r → ∞) → 0. Up to an additive constant we therefore end up with V (r) = C e− r δ r , (A7)"

    Substituting (A7) into (A6) gives V'' + (2/r)V' = V/δ², leaving the constant residual −1/(2δ²) from the 4πε0(1+2V) source, so (A7) solves only the homogeneous equation. The full decaying solution of (A6) is V = −1/2 + (B/2)e^{−r/δ}/r, which violates V(∞)=0, while an asymptotically flat solution would require the growing exponential. Thus the 'additive constant' discarded after (A6) is not a gauge freedom; the Yukawa potential is imposed, not derived from the Poisson equation.

  2. self citation load bearing [Sec. II A, Eqs. (5)-(7), citing Ref. [53]]
    "As reported explicitly in Appendix A, the energy density turns out to be [53] ε(r) = ε0(1 + 2V (r)), ... δ(Λ) = 1p 8πε0(Λ) . ... intimately related to the corresponding Yukawa potential V (r) = −αm e− r δ(Λ) r , (7)"

    Eqs. (5)-(7) already assert the Yukawa form before any derivation, citing the authors' own Ref. [53] (Capolupo, Capozziello, Pisacane, Quaranta, with overlapping authorship). The coefficient 2 in (5) and the definition δ^{-2}=8πε0 are exactly what make e^{-r/δ}/r the homogeneous solution, so the Appendix A 'derivation' returns the same Yukawa ansatz that was put in. The parameters α and δ are not predicted by the model: Section V selects α from Refs. [53,64,65,67] and δ from chosen cutoffs Λ, i.e. the free parameters are imported or fitted. Hence the central claim that FCDM induces a Yukawa correction is not an independent first-principles result; it is the self-cited input restated.

full rationale

The accretion-disk part (Sects. III-V) is a forward computation: given a Yukawa-perturbed metric (11)-(14), the geodesic quantities and Novikov-Thorne luminosity integrals are evaluated and compared with Schwarzschild; no luminosity data are fitted, so those curves are not circular. However, the paper's advertised first-principles result—that the flavor-condensate energy-momentum tensor induces the Yukawa potential (7)—is not independently derived. Appendix A's Poisson equation (A6) does not admit the claimed asymptotically flat Yukawa solution; the decaying homogeneous mode leaves a forced −1/2 constant, so discarding it is equivalent to assuming (7). The density-potential relation (5) and the potential (7) are taken from the authors' own Ref. [53], and the parameters α and δ are imported from rotation-curve fits. Thus the central Yukawa prediction reduces by construction to a self-cited ansatz, while the luminosity phenomenology that follows from it remains a valid but conditional exploration. This earns a partial-circularity score of 6.

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

The central calculation rests on the FCDM energy density relation ε = ε0(1+2V), which is assumed from prior work and is not independently derived here. The Poisson solution in Appendix A requires discarding a constant term to yield the Yukawa form, an ad hoc step. The disk observables also depend on α and δ chosen from galaxy fits, so the 'prediction' is conditional on these fitted inputs.

free parameters (5)
  • α (Yukawa coupling) = -0.92, -0.2, 0.8, -0.98, 0.4
    Free coupling strength of the Yukawa correction; values chosen from galaxy rotation curve and elliptical galaxy analyses (Refs. [53,64,65,67]), not predicted by the model.
  • Λ (cutoff) / δ (Yukawa range) = 10 GeV (δ=333 au), 1.6 keV (δ=10 kpc), 4 GeV (δ=832 au), 15.425 keV (δ=1.06 kpc)
    The UV cutoff Λ sets the condensate scale ε0 and hence δ via δ = 1/√(8πε0); the authors choose Λ to produce δ values of interest for accretion, effectively fitting δ.
  • rb (junction radius) = 6 MBH
    Inner radius of the dark matter envelope; chosen arbitrarily to make the weak field approximation hold (Section V).
  • MBH = 4.993 au
    Example black hole mass chosen for the numerical analysis; not derived.
  • Mdot (accretion rate) = 10^5 (geometric units)
    Assumed constant accretion rate of baryonic matter; chosen for illustration.
assumptions (5)
  • domain assumption Flavor vacuum stress-energy is pressureless dust (T^{μν} = diag(ε,0,0,0)).
    Taken from Refs. [51-54]; underpins the weak-field treatment.
  • domain assumption Energy density is linear in the potential: ε(r) = ε0(1 + 2V(r)).
    Eq. (5); the central input that produces the Yukawa potential after solving Poisson.
  • standard math The Poisson equation relates V to ε.
    Used in Appendix A to derive the potential from the density.
  • ad hoc to paper The positive exponential root of the Poisson solution is discarded and the constant -1/2 is dropped.
    Appendix A: 'up to an additive constant' removes the forced -1/2 term, which is not justified.
  • domain assumption Thin disk in Novikov-Thorne formalism with constant baryonic accretion rate.
    Standard model assumptions; the disk radiates as a blackbody and does not feed back on the metric.

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Pith. "Pith review of Impact of flavor condensate dark matter on accretion disk luminosity in spherical spacetimes." pith.science (2026). https://pith.science/paper/LCAVM7NH

@misc{pith2026250703758,
  author       = {Pith},
  title        = {Pith review of: Impact of flavor condensate dark matter on accretion disk luminosity in spherical spacetimes},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/LCAVM7NH}},
  note         = {Machine review of arXiv:2507.03758}
}
read the original abstract

We investigate the impact of dark matter condensates on the emission and thermodynamic properties of accretion disks, in a spherically-symmetric and static background. We focus on a class of models where dark matter originates from a genuine mass mixing among neutrino fields and compute the corrections to the dark matter's potential within galactic halo. We find a corresponding Yukawa correction induced by the dark matter energy-momentum tensor over the Newtonian potential. In so doing, employing Schwarzschild coordinates, and adopting the Novikov-Thorne formalism, we compute the geodesic structure and the corresponding disk-integrated luminosity profiles. Assuming a constant mass accretion rate, constituted solely by baryonic matter, we find non-negligible deviations in both the disk structure and radiative output, as compared to the standard Schwarzschild case. Afterwards, we discuss physical consequences of our Yukawa correction, comparing it with recent literature, predicting similar potentials, albeit derived from extended theories of gravity. Accordingly, we thus speculate to use our results to distinguish among candidates of dark matter. Indeed, our findings suggest that incoming high-precision observations of accretion disk spectra may provide a tool to probe dark matter's nature under the form of particles, extended theories of gravity or condensates.

Figures

Figures reproduced from arXiv: 2507.03758 by the authors.

Figure 1
Figure 1. FIG. 1. Logarithmic scale plot of the Energy density [PITH_FULL_IMAGE:figures/full_fig_p004_1.png] view at source ↗
Figure 2
Figure 2. FIG. 2. Rescaled angular velocity Ω [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. FIG. 3. Specific energy [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figures from the paper (3 more)
Figure 4
Figure 4. Figure 4: FIG. 4. Specific angular momentum [PITH_FULL_IMAGE:figures/full_fig_p006_4.png]
Figure 6
Figure 6. Figure 6: FIG. 6. Differential Luminosity [PITH_FULL_IMAGE:figures/full_fig_p007_6.png]
Figure 7
Figure 7. Figure 7: FIG. 7. Logarithmic scale plot of the spectral Luminosity [PITH_FULL_IMAGE:figures/full_fig_p007_7.png]

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Reference graph

Works this paper leans on

77 extracted references · 76 canonical work pages · cited by 1 Pith paper

  1. [1]

    All the scale lengths are r0 = 12 kpc

    with ε0,B = 11 .1 × 10−3 M⊙/pc3; the Einasto profile ε(r) = ε0,Ee 2(1−(r/r0 )σ ) σ with ε0,E = 20 .1 × 10−3 M⊙/pc3 and σ = 0 .12. All the scale lengths are r0 = 12 kpc. We have employed the values reported in [62] for the Milky Way. - theories that generically modify gravity, e.g., in [67] where a good agreement with the Milky way data is found in corresp...

    work page

  2. [2]

    Here, the metric in Eq

    α = 0. Here, the metric in Eq. (9) reduces to Schwarzschild everywhere, yielding ordinary accre- tion around a Schwarzschild black hole, having an ISCO as rISCO = rISCO, 0 = 6 MBH = 29 .598 au, for our chosen mass

    work page

  3. [3]

    This value of α is that of Ref

    α = −0.92, Λ = Λ 1 = 10 GeV → δ = δ1 = 333 au. This value of α is that of Ref. [64]. The cutoff Λ is chosen to reproduce δ of the order of a few hundreds of au. The ISCO is rISCO, 1 = 63.085 au

    work page

  4. [4]

    These values are compatible with those analyzed in Ref

    α = −0.2, Λ = Λ 2 = 1.6 keV → δ = δ2 = 10 kpc. These values are compatible with those analyzed in Ref. [65]. The ISCO is rISCO, 2 = 25.370 au

    work page

  5. [5]

    These values are compatible with those analyzed in [65]

    α = 0 .8, Λ = Λ 3 = 1 .6 keV → δ = δ3 = 10 kpc. These values are compatible with those analyzed in [65]. The ISCO is rISCO, 3 = 42.06 au

    work page

  6. [6]

    α = −0.98, Λ = Λ 4 = 4 GeV → δ = δ4 = 832 au. The value of α is determined from is a rather ex- treme negative value, compatible with the values discussed in [67], whereas δ is chosen to be around 103 au as an intermediate value between the disk region (a few au) and the galactic scale ( ≃ kpc). The ISCO is rISCO, 4 = 142.183 au

    work page

  7. [7]

    These values are obtained from the anal- ysis of the rotation curves of galaxies [53] and are likewise compatible with the analysis presented in [67]

    α = 0 .4, Λ = Λ 5 = 15 .425 keV → δ = δ5 = 1.06 kpc. These values are obtained from the anal- ysis of the rotation curves of galaxies [53] and are likewise compatible with the analysis presented in [67]. The ISCO is rISCO, 5 = 36.562 au In Fig. 2 we plot the angular velocity as a function ofr. The effect of the FCDM potential (7) is more pronounced at sma...

    work page

  8. [8]

    Italian Research Center on High- Performance Computing, Big Data and Quantum Com- puting

    The differential luminosity is indeed seen to vanish for the large negative values α = −0.98, −0.92, in the regions r < 30 MBH , r <10 MBH . All the values con- sidered, except α = −0.2, δ= δ2 = 10 kpc, yield a re- duced luminosity at radii r <15 MBH , as compared to the Schwarzschild case. In general, the presence of the FCDM leads to re- duced luminosit...

    work page

Show all 77 references
  1. [9]

    The Event Horizon Telescope Collaboration and K. et al. Akiyama. First m87 event horizon telescope results. i. the shadow of the supermassive black hole.The Astrophysical Journal Letters, 875(1):L1, apr 2019

    2019

  2. [10]

    Pesce, Daniel C

    Dominic W. Pesce, Daniel C. M. Palumbo, Ramesh Narayan, Lindy Blackburn, Sheperd S. Doeleman, Michael D. Johnson, Chung-Pei Ma, Neil M. Nagar, Priyamvada Natarajan, and Angelo Ricarte. Toward de- termining the number of observable supermassive black hole shadows. The Astrophys...

    2021

  3. [11]

    The persistent shadow of the supermassive black hole of m87 - i

    The Event Horizon Telescope Collaboration and Akiyama, Kazunori et al. The persistent shadow of the supermassive black hole of m87 - i. observations, calibra- tion, imaging, and analysis. A&A, 681:A79, 2024

    2024

  4. [12]

    Tests for the existence of black holes through gravitational wave echoes

    Vitor Cardoso and Paolo Pani. Tests for the existence of black holes through gravitational wave echoes. Nature Astronomy, 1(9):586–591, Sep 2017

    2017

  5. [13]

    B. P. et al. Abbott. Observation of gravitational waves from a binary black hole merger. Phys. Rev. Lett. , 116:061102, Feb 2016

    2016

  6. [14]

    Haehnelt

    Martin G. Haehnelt. Low-frequency gravitational waves from supermassive black holes. Monthly Notices of the Royal Astronomical Society, 269(1):199–208, 07 1994

    1994

  7. [15]

    Fox, Chad Hanna, and Kohta Murase

    P´ eter M´ esz´ aros, Derek B. Fox, Chad Hanna, and Kohta Murase. Multi-messenger astrophysics. Nature Reviews Physics, 1(10):585–599, Oct 2019

    2019

  8. [16]

    Supermassive black holes in the early universe

    Aaron Smith and Volker Bromm and. Supermassive black holes in the early universe. Contemporary Physics, 60(2):111–126, 2019

    2019

  9. [17]

    Fan Zou, Zhibo Yu, W. N. Brandt, Hyungsuk Tak, Guang Yang, and Qingling Ni. Mapping the growth of super- massive black holes as a function of galaxy stellar mass and redshift. The Astrophysical Journal, 964(2):183, mar 2024

    2024

  10. [18]

    Growth of high-redshift supermassive black holes from heavy seeds in the brahma cosmo- logical simulations: implications of overmassive black holes

    Aklant K Bhowmick, Laura Blecha, Paul Torrey, Rachel S Somerville, Luke Zoltan Kelley, Mark Vogels- berger, Rainer Weinberger, Lars Hernquist, and Aneesh Sivasankaran. Growth of high-redshift supermassive black holes from heavy seeds in the brahma cosmo- logical simulations: i...

    1907

  11. [19]

    T. R. Marsh, E. L. Robinson, and J. H. Wood. Spec- troscopy of $a0620-00$: the mass of the black hole and an image of its accretion disc. Monthly Notices of the 9 Royal Astronomical Society, 266(1):137–154, 01 1994

    1994

  12. [20]

    R. J. McLure and M. J. Jarvis. Measuring the black hole masses of high-redshift quasars. Monthly Notices of the Royal Astronomical Society, 337(1):109–116, 11 2002

    2002

  13. [21]

    Calderone, G

    G. Calderone, G. Ghisellini, M. Colpi, and M. Dotti. Black hole mass estimate for a sample of radio-loud narrow-line seyfert 1 galaxies. Monthly Notices of the Royal Astronomical Society, 431(1):210–239, 03 2013

    2013

  14. [22]

    McKinney, Alexander Tchekhovskoy, and Roger D

    Jonathan C. McKinney, Alexander Tchekhovskoy, and Roger D. Blandford. General relativistic magnetohy- drodynamic simulations of magnetically choked accretion flows around black holes. Monthly Notices of the Royal Astronomical Society, 423(4):3083–3117, 07 2012

    2012

  15. [23]

    Gammie and Robert Popham

    Charles F. Gammie and Robert Popham. Advection- dominated accretion flows in the kerr metric. i. basic equations. The Astrophysical Journal , 498(1):313, may 1998

    1998

  16. [24]

    Robert Popham and Charles F. Gammie. Advection- dominated accretion flows in the kerr metric. ii. steady state global solutions. The Astrophysical Journal , 504(1):419, sep 1998

    1998

  17. [25]

    Abramowicz and P

    Marek A. Abramowicz and P. Chris Fragile. Foundations of black hole accretion disk theory. Living Reviews in Relativity, 16(1):1, Jan 2013

    2013

  18. [26]

    I. D. Novikov and K. S. Thorne. Astrophysics of black holes. In C. Dewitt and B. S. Dewitt, editors,Black Holes (Les Astres Occlus), pages 343–450, January 1973

    1973

  19. [27]

    Page and Kip S

    Don N. Page and Kip S. Thorne. Disk-Accretion onto a Black Hole. Time-Averaged Structure of Accretion Disk. Astrophys. J., 191:499–506, July 1974

    1974

  20. [28]

    A review of bondi–hoyle–lyttleton accre- tion

    Richard Edgar. A review of bondi–hoyle–lyttleton accre- tion. New Astronomy Reviews , 48(10):843–859, 2004

    2004

  21. [29]

    Bondi accretion in the early universe

    Massimo Ricotti. Bondi accretion in the early universe. The Astrophysical Journal , 662(1):53, jun 2007

    2007

  22. [30]

    Bondi accretion onto cosmological black holes

    Janusz Karkowski and Edward Malec. Bondi accretion onto cosmological black holes. Phys. Rev. D , 87:044007, Feb 2013

    2013

  23. [31]

    Impact of extended gravity theories on accre- tion dynamics and observables in black hole

    Shahid Chaudhary, Shahi Rome, Muhammad Dan- ish Sultan, Ahmadjon Abdujabbarov, Awatef Abidi, Yousef Mohammad Alanazi, and Abdulrahman Bin Jumah. Impact of extended gravity theories on accre- tion dynamics and observables in black hole. Annals of Physics, 477:170006, 2025

    2025

  24. [32]

    Boshkayev, T

    K. Boshkayev, T. Konysbayev, Ye. Kurmanov, O. Lu- ongo, and D. Malafarina. Accretion disk luminosity for black holes surrounded by dark matter with tangential pressure. The Astrophysical Journal, 936(2):96, sep 2022

    2022

  25. [33]

    Accretion disc luminosity for black holes surrounded by dark matter

    K Boshkayev, A Idrissov, O Luongo, and D Malafarina. Accretion disc luminosity for black holes surrounded by dark matter. Monthly Notices of the Royal Astronomical Society, 496(2):1115–1123, 06 2020

    2020

  26. [34]

    Kurmanov, K

    E. Kurmanov, K. Boshkayev, R. Giamb` o, T. Konysbayev, O. Luongo, D. Malafarina, and H. Quevedo. Accretion disk luminosity for black holes surrounded by dark mat- ter with anisotropic pressure. The Astrophysical Journal, 925(2):210, feb 2022

    2022

  27. [35]

    Yfantis, and Kostas D

    Sourabh Nampalliwar, Aristomenis I. Yfantis, and Kostas D. Kokkotas. Extending grmhd for thin disks to non-kerr spacetimes. Phys. Rev. D , 106:063009, Sep 2022

    2022

  28. [36]

    The Final stages of accretion onto non-Kerr compact objects

    Cosimo Bambi and Enrico Barausse. The Final stages of accretion onto non-Kerr compact objects. Phys. Rev. D , 84:084034, 2011

    2011

  29. [37]

    Luminosity of accretion disks in compact objects with a quadrupole

    Kuantay Boshkayev, Talgar Konysbayev, Ergali Kur- manov, Orlando Luongo, Daniele Malafarina, and Her- nando Quevedo. Luminosity of accretion disks in compact objects with a quadrupole. Phys. Rev. D , 104(8):084009, 2021

    2021

  30. [38]

    Particle dy- namics and the accretion disk around a Self-dual Black Hole immersed in a magnetic field in Loop Quantum Gravity

    Uktamjon Uktamov, Mirzabek Alloqulov, Sanjar Shay- matov, Tao Zhu, and Bobomurat Ahmedov. Particle dy- namics and the accretion disk around a Self-dual Black Hole immersed in a magnetic field in Loop Quantum Gravity. Phys. Dark Univ. , 47:101743, 2025

    2025

  31. [39]

    Joshi, Dipanjan Dey, and Pankaj S

    Divya Tahelyani, Ashok B. Joshi, Dipanjan Dey, and Pankaj S. Joshi. Comparing thin accretion disk prop- erties of naked singularities and black holes. Phys. Rev. D, 106(4):044036, 2022

    2022

  32. [40]

    Accretion disk luminosity around ro- tating naked singularities

    Yergali Kurmanov, Kuantay Boshkayev, Talgar Konys- bayev, Marco Muccino, Orlando Luongo, Ainur Uraza- lina, Anar Dalelkhankyzy, Farida Belissarova, and Mad- ina Alimkulova. Accretion disk luminosity around ro- tating naked singularities. Phys. Dark Univ. , 48:101917, 2025

    2025

  33. [41]

    Pseudo-Newtonian Simulation of a Thin Accretion Disk Around a Reissner–Nordstr¨ om Naked Singularity

    Miljenko ˇCemelji´ c, W lodek Klu´ zniak, Ruchi Mishra, and Maciek Wielgus. Pseudo-Newtonian Simulation of a Thin Accretion Disk Around a Reissner–Nordstr¨ om Naked Singularity. Astrophys. J., 981(1):69, 2025

    2025

  34. [42]

    Pantig, and Ali ¨Ovg¨ un

    Akhil Uniyal, Sayan Chakrabarti, Reggie C. Pantig, and Ali ¨Ovg¨ un. Nonlinearly charged black holes: Shadow and thin-accretion disk. New Astron., 111:102249, 2024

    2024

  35. [43]

    Anisotropic generalized poly- tropic spheres: Regular 3D black holes

    Seyed Naseh Sajadi, Mohsen Khodadi, Orlando Luongo, and Hernando Quevedo. Anisotropic generalized poly- tropic spheres: Regular 3D black holes. Phys. Dark Univ., 45:101525, 2024

    2024

  36. [44]

    Accre- tion disks properties around regular black hole solutions obtained from non-linear electrodynamics

    Yergali Kurmanov, Kuantay Boshkayev, Talgar Konys- bayev, Orlando Luongo, Nazym Saiyp, Ainur Uraza- lina, Gulfeiruz Ikhsan, and Gulnara Suliyeva. Accre- tion disks properties around regular black hole solutions obtained from non-linear electrodynamics. Phys. Dark Univ., 46:101...

    2024

  37. [45]

    The dark matter profiles in the milky way

    Hai-Nan Lin and Xin Li. The dark matter profiles in the milky way. Monthly Notices of the Royal Astronomical Society, 487(4):5679–5684, 06 2019

    2019

  38. [46]

    Ac- creting black holes in dark matter halos

    Sobhan Kazempour, Sichun Sun, and Chengye Yu. Ac- creting black holes in dark matter halos. Phys. Rev. D , 110:043034, Aug 2024

    2024

  39. [47]

    Elisa G. M. Ferreira. Ultra-light dark matter. The As- tronomy and Astrophysics Review , 29(1):7, Sep 2021

    2021

  40. [48]

    Rogers, Ren´ ee Hloˇ zek, Alex Lagu¨ e, Mikhail M

    Keir K. Rogers, Ren´ ee Hloˇ zek, Alex Lagu¨ e, Mikhail M. Ivanov, Oliver H.E. Philcox, Giovanni Cabass, Kazuyuki Akitsu, and David J.E. Marsh. Ultra-light axions and the s8 tension: joint constraints from the cosmic microwave background and galaxy clustering. Journal of Cosmo...

    2023

  41. [49]

    Ostriker, Scott Tremaine, and Ed- ward Witten

    Lam Hui, Jeremiah P. Ostriker, Scott Tremaine, and Ed- ward Witten. Ultralight scalars as cosmological dark matter. Phys. Rev. D , 95:043541, Feb 2017

    2017

  42. [50]

    Dark compact objects: An extensive overview

    Maksym Deliyergiyev, Antonino Del Popolo, Laura To- los, Morgan Le Delliou, Xiguo Lee, and Fiorella Burgio. Dark compact objects: An extensive overview. Phys. Rev. D, 99:063015, Mar 2019

    2019

  43. [51]

    Timothy D. Brandt. Constraints on macho dark matter from compact stellar systems in ultra-faint dwarf galax- ies. The Astrophysical Journal Letters , 824(2):L31, jun 2016. 10

    2016

  44. [52]

    Primordial black holes as a dark matter candidate

    Anne M Green and Bradley J Kavanagh. Primordial black holes as a dark matter candidate. Journal of Physics G: Nuclear and Particle Physics , 48(4):043001, feb 2021

    2021

  45. [53]

    Gravitational metamaterials from op- tical properties of spacetime media

    Orlando Luongo. Gravitational metamaterials from op- tical properties of spacetime media. 4 2025

    2025

  46. [54]

    Dark matter as gravitational solitons in the weak field limit

    Torsten Asselmeyer-Maluga and Jerzy Kr´ ol. Dark matter as gravitational solitons in the weak field limit. Universe, 6(12), 2020

    2020

  47. [55]

    Piat- tella

    Stefano Profumo, Leonardo Giani, and Oliver F. Piat- tella. An introduction to particle dark matter. Universe, 5(10), 2019

    2019

  48. [56]

    Jes´ us Zavala and Carlos S. Frenk. Dark matter haloes and subhaloes. Galaxies, 7(4):81, 2019

    2019

  49. [57]

    Quantum field theory of three flavor neutrino mix- ing and oscillations with CP violation

    Massimo Blasone, Antonio Capolupo, and Giuseppe Vi- tiello. Quantum field theory of three flavor neutrino mix- ing and oscillations with CP violation. Phys. Rev. D , 66:025033, Jul 2002

    2002

  50. [58]

    Dark matter and dark energy in- duced by condensates

    Antonio Capolupo. Dark matter and dark energy in- duced by condensates. Advances in High Energy Physics, 2016(1):8089142, 2016

    2016

  51. [59]

    Quantum flavor vacuum in the expanding universe: A possible candidate for cosmological dark matter? Phys

    Antonio Capolupo, Sante Carloni, and Aniello Quaranta. Quantum flavor vacuum in the expanding universe: A possible candidate for cosmological dark matter? Phys. Rev. D, 105:105013, May 2022

    2022

  52. [60]

    Field mixing in curved spacetime and dark matter

    Antonio Capolupo, Aniello Quaranta, and Raoul Serao. Field mixing in curved spacetime and dark matter. Sym- metry, 15(4), 2023

    2023

  53. [61]

    Missing matter in galax- ies as a neutrino mixing effect

    Antonio Capolupo, Salvatore Capozziello, Gabriele Pisacane, and Aniello Quaranta. Missing matter in galax- ies as a neutrino mixing effect. Physics of the Dark Uni- verse, 48:101894, 2025

    2025

  54. [62]

    Capolupo, G

    A. Capolupo, G. Lambiase, and A. Quaranta. Neutrinos in curved spacetime: Particle mixing and flavor oscilla- tions. Phys. Rev. D , 101:095022, May 2020

    2020

  55. [63]

    Navas et al

    S. Navas et al. Review of particle physics. Phys. Rev. D , 110(3):030001, 2024

    2024

  56. [64]

    Generalized K- essence inflation in Jordan and Einstein frames

    Orlando Luongo and Tommaso Mengoni. Generalized K- essence inflation in Jordan and Einstein frames. Class. Quant. Grav., 41(10):105006, 2024

    2024

  57. [65]

    Healing the cosmological constant problem dur- ing inflation through a unified quasi-quintessence matter field

    Rocco D’Agostino, Orlando Luongo, and Marco Muc- cino. Healing the cosmological constant problem dur- ing inflation through a unified quasi-quintessence matter field. Class. Quant. Grav. , 39(19):195014, 2022

    2022

  58. [66]

    Particle production from non-minimal coupling in a sym- metry breaking potential transporting vacuum energy

    Alessio Belfiglio, Youri Carloni, and Orlando Luongo. Particle production from non-minimal coupling in a sym- metry breaking potential transporting vacuum energy. Phys. Dark Univ. , 44:101458, 2024

    2024

  59. [67]

    Speeding up the universe using dust with pressure

    Orlando Luongo and Marco Muccino. Speeding up the universe using dust with pressure. Phys. Rev. D , 98(10):103520, 2018

    2018

  60. [68]

    Alleviating the cosmological constant problem from par- ticle production

    Alessio Belfiglio, Roberto Giamb` o, and Orlando Luongo. Alleviating the cosmological constant problem from par- ticle production. Class. Quant. Grav. , 40(10):105004, 2023

    2023

  61. [69]

    Revising the cosmological constant problem through a fluid different from the quintessence

    Orlando Luongo. Revising the cosmological constant problem through a fluid different from the quintessence. Phys. Sci. Tech., 10(3-4):17–27, 2023

    2023

  62. [70]

    Ef- fects of non-vanishing dark matter pressure in the milky way galaxy

    K Boshkayev, T Konysbayev, E Kurmanov, O Luongo, D Malafarina, K Mutalipova, and G Zhumakhanova. Ef- fects of non-vanishing dark matter pressure in the milky way galaxy. Monthly Notices of the Royal Astronomical Society, 508(1):1543–1554, 09 2021

    2021

  63. [71]

    Graviton mass due to dark energy as a superconducting medium-theoretical and phenomeno- logical aspects

    Nader Inan, Ahmed Farag Ali, Kimet Jusufi, and Ab- delrahman Yasser. Graviton mass due to dark energy as a superconducting medium-theoretical and phenomeno- logical aspects. Journal of Cosmology and Astroparticle Physics, 2024(08):012, aug 2024

    2024

  64. [72]

    R. H. Sanders. Anti-gravity and galaxy rotation curves. aap, 136(2):L21–L23, July 1984

    1984

  65. [73]

    Constraining theories of gravity by fundamental plane of elliptical galaxies

    Salvatore Capozziello, Vesna Borka Jovanovi´ c, Duˇ sko Borka, and Predrag Jovanovi´ c. Constraining theories of gravity by fundamental plane of elliptical galaxies. Physics of the Dark Universe , 29:100573, 2020

    2020

  66. [74]

    Frigerio Martins and P

    C. Frigerio Martins and P. Salucci. Analysis of rota- tion curves in the framework of R n gravity. MNRAS, 381(3):1103–1108, November 2007

    2007

  67. [75]

    Testing gravity with the milky way: Yukawa potential

    Jakob Henrichs, Margherita Lembo, Fabio Iocco, and Luca Amendola. Testing gravity with the milky way: Yukawa potential. Phys. Rev. D , 104:043009, Aug 2021

    2021

  68. [76]

    Combining rotation curves and gravitational lensing: How to measure the equation of state of dark matter in the galactic halo.Mon

    Tristan Faber and Matt Visser. Combining rotation curves and gravitational lensing: How to measure the equation of state of dark matter in the galactic halo.Mon. Not. Roy. Astron. Soc. , 372:136–142, 2006

    2006

  69. [77]

    S., and Harko, T

    Kov´ acs, Z., Cheng, K. S., and Harko, T. Thin accretion discs around neutron and quark stars. A&A, 500(2):621– 631, 2009. Appendix A: Flavor condensate energy density in the Schwarzschild chart In this appendix we derive the energy density due to the flavor condensate in the ...

    2009

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