{"arxiv_id":"astro-ph/9906391","incoming":{"papers":272,"sentences":548,"groups":[{"kind":"contests","label":"Contests it","papers":1,"sentences":1,"quotes":[{"arxiv_id":"2605.20117","title":"The potential of diffuse Galactic Ridge neutrino measurements to constrain dark matter","url":"/paper/2605.20117","section":"Galactic DM density profile","sentence":"From a DM annihilation standpoint, the original Adiabatic Spike [ref] has also been ruled out by comparing the expected DM flux with the observed HESS data in the GC [ref] , which further motivates using this approach.","intent_p":0.71,"contests_p":0.73}]},{"kind":"extends","label":"Builds on it","papers":3,"sentences":4,"quotes":[{"arxiv_id":"0802.0234","title":"Multi-wavelength signals of dark matter annihilations at the Galactic center","url":"/paper/0802.0234","section":"A few benchmark scenarios","sentence":"The picture sketched in [ref] and [ref] has been further refined in [ref] , where a time-evolution analysis of the cusp formation is performed, including the effects of self annihilations, scattering of dark matter particles by stars, and capture in the black hole.","intent_p":0.85,"contests_p":null},{"arxiv_id":"2404.11513","title":"Dark matter, black holes, and gravitational waves","url":"/paper/2404.11513","section":"Matter around Black Holes","sentence":"Gondolo and Silk [ref] applied the results obtained by Quinlan, Hernquist, and Sigurdsson [ref] to the dark matter cusps that several groups of authors had put forward in the 1990s [ref] .","intent_p":0.81,"contests_p":null},{"arxiv_id":"1707.06302","title":"Dark matter spikes in the vicinity of Kerr black holes","url":"/paper/1707.06302","section":"Discussion","sentence":"The expression in rhofit is a generalization of Eq. 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[ref] for a DM spike growing from an initial profile $∝ρ_0 ( r/r_0 )^-γ$: [equation] where the saturation density determined by DM annihilations reads [equation] with $m_DM$ and $⟨σv ⟩$ respectively the mass and annihilation cross-section of the DM particle, and $t_BH$ the age of the BH.","intent_p":0.81,"contests_p":null},{"arxiv_id":"2605.07616","title":"Probing the Inert Doublet Dark Matter with Stellar-Mass Black Hole Mini-Spikes","url":"/paper/2605.07616","section":"Indirect Detection","sentence":"In this work, we adopt the framework developed in Ref. [ref] , in which the dark matter distribution around stellar-mass black holes is modeled under the assumption of adiabatic growth [ref] .","intent_p":0.96,"contests_p":null},{"arxiv_id":"2511.12570","title":"Black hole spacetimes with dark matter spikes: Energy-momentum tensor and backreaction effects","url":"/paper/2511.12570","section":"DM spike around a BH","sentence":"We adopt the standard approach from [ref] , assuming the geodesics of DM particles are governed solely by the Schwarzschild metric of the central BH.","intent_p":0.98,"contests_p":null},{"arxiv_id":"2306.11787","title":"Gravitational Radiation from hyperbolic encounters in the presence of dark matter","url":"/paper/2306.11787","section":"Model for the dynamical friction due to DM spike","sentence":"We consider a DM mini spike model given in [ref] .","intent_p":0.83,"contests_p":null},{"arxiv_id":"2307.06823","title":"Multi-TeV dark matter density in the inner Milky Way halo: spectral and dynamical constraints","url":"/paper/2307.06823","section":"S2 star dynamical constraints","sentence":"In the left panel, we show the constraints integrating the McMillan17 profile with the BH adiabatic spike prescription given by [ref] and computing the maximum $R_sp$ allowed by the observations.","intent_p":0.95,"contests_p":null}]},{"kind":"data_used","label":"Uses its data or values","papers":5,"sentences":6,"quotes":[{"arxiv_id":"2501.11569","title":"Blazar Boosted ALP and vector portal Dark matter confronting light mediator searches","url":"/paper/2501.11569","section":"DM density profile","sentence":"Generally the spike radius is taken to be $R_sp=10^5 R_s$ [ref] , where $R_s=2 GM_BH/c^2 (c=1$ in natural unit) is the Schwarzschild radius [ref] .","intent_p":0.91,"contests_p":null},{"arxiv_id":"2506.12642","title":"Dark matter spikes with strongly self-interacting particles","url":"/paper/2506.12642","section":"DM density profile","sentence":"[equation] where the constant $α_γ$ must be evaluated numerically, and is $α_γ≈0.1$ for $γ=0.7-1.4$ [ref] .","intent_p":0.98,"contests_p":null},{"arxiv_id":"2401.09182","title":"Probing black holes in a dark matter spike of M87 using quasinormal modes","url":"/paper/2401.09182","section":"Density profile of a dark matter spike near the black hole","sentence":"Here, we adopt the power-law index $γ$ from Refs. [ref] and mainly focus on the case of $γ∈[1/2,3/2]$ and then $γ_sp ∈[16/7,12/5]$.","intent_p":0.97,"contests_p":null},{"arxiv_id":"2411.14047","title":"Dynamical friction can flip the hierarchical three-body system","url":"/paper/2411.14047","section":"DM sipke parameters $ρ_sp$ and $R_sp$","sentence":"Finally, the empirical radius $R_sp$ can be obtained with [equation] where $a_γ≃0.1$ [ref] .","intent_p":0.94,"contests_p":null},{"arxiv_id":"2605.15330","title":"A metric solution for rotating black holes embedded in dark matter halos with central spikes","url":"/paper/2605.15330","section":"Numerical results and discussions","sentence":"For the Milky Way, the mass is $M_B ≃4×10^6 M_⊙$, while the mass within the central parsec can reach $∼10^7$-$10^8 M_⊙$, depending on the assumed density profile [ref] .","intent_p":0.83,"contests_p":null}]},{"kind":"comparison","label":"Compares with it","papers":7,"sentences":7,"quotes":[{"arxiv_id":"2404.08731","title":"Dark Matter Mounds: towards a realistic description of dark matter overdensities around black holes","url":"/paper/2404.08731","section":"Introduction","sentence":"We see that the density after SMS formation is significantly lower than the spike profile of Refs. [ref] , in the region where the gravitational wave signal is expected to peak.","intent_p":0.86,"contests_p":null},{"arxiv_id":"0802.0234","title":"Multi-wavelength signals of dark matter annihilations at the Galactic center","url":"/paper/0802.0234","section":"A few benchmark scenarios","sentence":"Our benchmark DM profiles are shown in Fig. [ref], together, for comparison, with the NFW profile and the \"spiky\" profile obtained implementing the original procedure outlined in [ref] .","intent_p":0.96,"contests_p":null},{"arxiv_id":"2605.01023","title":"Formation and Redshift Evolution of Dark Matter Spikes","url":"/paper/2605.01023","section":"Cosmic Evolution of DM overdensities in a star cluster: The steady-state solutions","sentence":"In the previous section we saw that for several plausible scenarios for the initial black hole mass seed and DM and stellar initial density profiles, steep overdensities can be formed, in some scenarios even resembling the Gondolo and Silk expectation from Ref. [ref] , see Appendix [ref].","intent_p":0.86,"contests_p":null},{"arxiv_id":"2506.06554","title":"Black-hole hair from vector dark matter accretion","url":"/paper/2506.06554","section":"Density profile","sentence":"This is the same behavior as has been found for analogous scalar-field solutions [ref] , and it matches the well-understood behavior of cold dust accreting onto a central [ref] .","intent_p":1.0,"contests_p":null},{"arxiv_id":"2608.00307","title":"Kerr black holes with vector dark matter hair","url":"/paper/2608.00307","section":"Density profile","sentence":"In the particle regime ($μM≳1$), the spike had a profile $ρ∼r^-3/2$, which matches both the analogous scalar-field profile [ref] and the density profiles of generic non-relativistic particle dark matter spikes studied in the literature [ref] .","intent_p":0.98,"contests_p":null}]},{"kind":"supports_this_paper","label":"Cites it as support","papers":3,"sentences":3,"quotes":[{"arxiv_id":"2409.10846","title":"Probing dark-matter effects with gravitational waves using the parameterized post-Einsteinian framework","url":"/paper/2409.10846","section":"Introduction","sentence":"In fact, prior work has confirmed this: if dark matter is present around an IMBH in sufficiently large amounts, the density of a spherically symmetric DM overdensity (referred to as a DM “spike” [ref] ) could be inferred from a GW measurement with LISA [ref] .","intent_p":0.97,"contests_p":null},{"arxiv_id":"1904.13060","title":"On the change of old neutron star masses with galactocentric distance","url":"/paper/1904.13060","section":"Mass Change of Neutron Stars","sentence":"Such conjecture is reinforced, as several papers are agreeing on the fact that the density close to the galactic center is of the order of, or even much larger ($10^4$ times larger) than, that indicated by DC14 [ref] .","intent_p":0.98,"contests_p":null},{"arxiv_id":"0808.2641","title":"Fitting the Gamma-Ray Spectrum from Dark Matter with DMFIT: GLAST and the Galactic Center Region","url":"/paper/0808.2641","section":"Dark Matter Models","sentence":"Our choice is physically well motivated by the scenario of adiabatic contraction of dark matter around the central super-massive black hole Sgr A$^*$ [ref] .","intent_p":1.0,"contests_p":null}]},{"kind":"background","label":"Cites it as background","papers":80,"sentences":95,"quotes":[{"arxiv_id":"2305.05155","title":"Constraining $p$-wave Dark Matter Annihilation with Gamma-ray Observations of M87","url":"/paper/2305.05155","section":"Introduction","sentence":"If the center of a galaxy hosts a supermassive black hole (SMBH), then the region just outside the black hole may exhibit a large density of dark matter, known as a dark matter spike [ref] .","intent_p":0.97,"contests_p":null},{"arxiv_id":"1701.00067","title":"Black Holes, Dark Matter Spikes, and Constraints on Simplified Models with $t$-Channel Mediators","url":"/paper/1701.00067","section":"Dark Matter Spike Near the Supermassive Black Hole","sentence":"The formation of a DM spike is contingent on several conditions, detailed for example in [ref] and [ref] .","intent_p":0.91,"contests_p":null},{"arxiv_id":"2605.01023","title":"Formation and Redshift Evolution of Dark Matter Spikes","url":"/paper/2605.01023","section":"Canonical spike formation","sentence":"The traditional framework for the formation of dark-matter (DM) overdensities around a supermassive black hole (SMBH) is the adiabatic growth model from [ref] .","intent_p":0.9,"contests_p":null},{"arxiv_id":"2502.15468","title":"Multi-messenger detection of black hole binaries in dark matter spikes","url":"/paper/2502.15468","section":"Introduction","sentence":"The binary is embedded within a DM spike, formed in a DM halo as a consequence of the adiabatic growth of a central black hole [ref] .","intent_p":0.81,"contests_p":null},{"arxiv_id":"2301.08756","title":"NGC 1068 constraints on neutrino-dark matter scattering","url":"/paper/2301.08756","section":"Dark matter spike profile","sentence":"The accretion of DM onto the SMBH has been widely studied in the literature, e.g., Refs. 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