{"id":"ae66c7a5-4b60-4e2b-b778-28c450813269","arxiv_id":"2610.26482","paper_version":1,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":5.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":3,"one_line_summary":"In a Randall-Sundrum II braneworld, enhanced early accretion and modified Hawking evaporation let sub-Planck-scale primordial black holes remain viable as the entirety of dark matter.","lead":"This PhD thesis computes how primordial black holes grow, evaporate, and leave observable signatures if the universe has an extra warped dimension of the Randall-Sundrum type. It concludes that higher-dimensional effects can boost early black hole growth so strongly that light holes, formed below the four-dimensional Planck scale, could still make up all of today's dark matter.","discovery_kind":"extension","skeptic_critique":{"model":"deepseek/deepseek-v4-flash","headline":"The t^0.33 accretion growth is integrated without demonstrating that r0(t) stays in the r0 << l regime where the Schwarzschild-Tangherlini metric is controlled; if r0/l crosses ~0.1 during the strong-accretion epoch, the central scaling is extrapolated into the known-unknown intermediate geometry.","rationale":"The reader's weakest assumption already points at the Schwarzschild–Tangherlini choice and the two-regime problem; I agree with that direction but sharpen it. The unresolved issue is not primarily the existence of an exact interpolating metric in the abstract, but the time-integrated use of ST: because the accretion calculation itself changes M, and r0 depends on M, the validity condition r0 << l is a dynamical bound that must be checked along each trajectory used for the final constraints. The thesis is honest about the two-regime problem and about using ST for near-horizon processes, and it does motivate the ST choice by its top-down bulk provenance. It also uses public codes (BlackMax, CosmoLED) and states its methods, which is independent support worth crediting. However, the t^0.33 exponent and the 'several orders of magnitude' claim are quoted as results over an epoch, and the text available here does not show that the mass trajectories remain in the small-black-hole regime throughout that epoch. The proposed check is inexpensive and decisive: if r0/l stays small and the DMPR sensitivity test leaves the exponent essentially unchanged, the concern does not land and the conditional verdict can be relaxed; if either fails, the central claim must be presented as conditional on the unknown brane-black-hole geometry. The reader's CONDITIONAL verdict is therefore appropriate, and my read does not require changing it.","tokens_in":61538,"tokens_out":19606,"duration_ms":165840,"concrete_test":"On the f_PBH=1 parameter grid of Chapter 12, integrate the Section 11.2.3 mass evolution and record r0(t)/l at every time step; flag any trajectory with max(r0/l) >= 0.1 during the strong-accretion epoch, since Sections 7.2 and 7.4.6 give no controlled metric there. Then recompute the accretion integrals with the DMPR/tidal-charge metric (7.40), Q ≈ -2 M l, in place of ST. If the final masses change by more than a factor of a few, or the growth exponent moves by more than ~0.03 relative to t^0.33, the all-DM conclusion should be conditional on the unresolved brane-black-hole geometry rather than presented as a robust prediction.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The central quantitative result—the t^0.33 growth of the mass discrepancy and the f_PBH=1 regions—is produced by integrating Michel accretion in the Schwarzschild–Tangherlini induced metric, with critical radius r_cr = sqrt(2) r0 (Section 11.2, eq. 11.22). That metric and its critical point are controlled by the condition r0 << l, stated in Section 7.2 as the definition of the small-black-hole regime. But accretion changes M, and for ST r0 ∝ (l M)^{1/2} (eq. 7.31). The thesis quotes 'several orders of magnitude' growth in M over the strong-accretion epoch, which means log10(r0/l) rises by half that amount. The available text does not display, for the parameter combinations that produce f_PBH=1, the trajectory of r0(t)/l across that epoch. If any trajectory crosses r0/l ~ 0.1, the accretion rate and the evaporation history used in the constraint analysis are computed in the intermediate 'pancake' regime, which Section 7.4.6 explicitly says has no known analytic metric. The two-regime problem is acknowledged, but the paper does not acknowledge that its own growth prediction may drive r0 out of the regime where the ST metric is valid. A leading O((r0/l)^2) AdS correction would enter f(r) in the critical-point condition (11.21) and could change the exponent, not just the normalization. Thus the claimed orders-of-magnitude enhancement is not yet secured unless the small-BH condition is verified along every mass trajectory or the leading corrections are shown to be negligible.","agreement_with_reader":"partial"},"referee_report":{"model":"deepseek/deepseek-v4-flash","summary":"The thesis studies primordial black holes (PBHs) in the Randall–Sundrum II braneworld. It combines a review of braneworld cosmology and higher-dimensional black hole geometry with two original studies: a relativistic Michel-type accretion calculation for small braneworld PBHs built on the Schwarzschild–Tangherlini induced metric, and a reanalysis of PBH constraints (Hawking radiation, gamma-ray backgrounds, microlensing, CMB energy injection) using modified higher-dimensional evaporation. The headline results are a t^0.33 growth of the mass discrepancy relative to earlier estimates during the strong-accretion epoch, an orders-of-magnitude enhancement of early accretion onto light PBHs, and the identification of parameter regions in which PBHs formed below the effective four-dimensional Planck scale can constitute the whole of the dark matter.","tokens_in":62033,"tokens_out":7624,"duration_ms":66328,"significance":"If the central accretion calculation is sound, the thesis would substantially change the mapping between initial and present-day PBH mass functions in RS-II cosmology and would reopen a light-PBH window for dark matter that standard four-dimensional treatments close. The thesis is transparent about the notorious two-regime problem for braneworld black holes, and it makes constructive use of existing numerical tools and published greybody computations. The derivation of the Schwarzschild–Tangherlini critical radius and the identification of the additional conserved quantity A3 are useful, and the claim that braneworld effects soften the validity restrictions of Michel accretion is falsifiable. The main caveat is that the quantitative results currently rest on the small-black-hole approximation r0 << l, and the thesis does not verify that this condition survives the very mass growth it predicts. That check is load-bearing for the t^0.33 scaling, for the evaporation history, and therefore for the f_PBH = 1 regions.","major_comments":[{"comment":"The t^0.33 accretion law and the resulting f_PBH = 1 regions are obtained by integrating Michel accretion on the Schwarzschild–Tangherlini induced metric, whose stated domain of validity is r0 << l. Since the mass grows by several orders of magnitude and r0 ∝ sqrt(l M)/M4 (eq. 7.31), log10(r0/l) grows as half of log10 M. The manuscript does not display r0(t)/l along the trajectories that terminate in the allowed f_PBH = 1 regions. If any trajectory crosses r0/l ~ 0.1 during the strong-accretion epoch, the accretion rate and the evaporation history are being computed in the intermediate regime for which, as §7.4.6 states, no known analytic metric exists. The two-regime problem is acknowledged, but the manuscript does not acknowledge that its own growth prediction may drive the solution out of the small-BH regime. Because a leading (r0/l)^2 correction to f(r) would enter the critical-point condition (11.21), the quoted exponent and the orders-of-magnitude enhancement are not secured unless the small-BH condition is verified along each mass trajectory or the leading AdS corrections are shown to be negligible.","section":"§11.2.1–11.2.5 with §7.2 and §7.4.6","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The claim that Michel's quasi-steady, test-fluid formalism is valid for a much wider range of PBH masses in RS-II than in four-dimensional general relativity is the justification for using eq. (11.22) throughout the strong-accretion epoch. The text asserts that the exact domain is determined by the collapse dynamics, but the mass-evolution calculation does not display the quantitative criterion (for example, accretion-flow crossing time versus Hubble time, and self-gravity of the accreted fluid relative to the black hole mass) evaluated along the same benchmark trajectories used for the f_PBH = 1 conclusion. Please state the criterion explicitly and verify that the trajectories behind the headline results satisfy it, rather than only arguing that the restrictions are softened in braneworlds.","section":"§11.3 and §11.2.4","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The conclusion that PBHs can account for all of the dark matter while originating below the four-dimensional Planck scale requires a specified formation-abundance input. Section 10.2 states that a dedicated analysis of small-black-hole collapse in the high-energy regime does not yet exist; with that step absent, the mapping between an initial PBH mass spectrum and the populations used in the constraint analysis is not closed. If the f_PBH = 1 regions are computed for a monochromatic initial mass function, this should be stated explicitly, and the sensitivity of the viable regions to the assumed initial mass function should be quantified.","section":"§10.2 and §14","authors_acknowledge":null,"authors_acknowledge_p":null}],"minor_comments":[{"comment":"The intentional lack of unified notation makes the thesis harder to check; for example, h_mu_nu denotes the spatial projector in Part I and the metric perturbation in Part II. A table of symbols with the conventions used in each part would substantially improve readability.","section":"General notation","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The t^0.33 exponent is quoted to two significant figures, but the integration limits and the full expression for M(t) during the strong-accretion epoch are not displayed in the presented excerpt. Please give the explicit integration from t_i to t_f and the resulting prefactor, so the scaling can be checked independently.","section":"§11.2.4","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The statement that the five-dimensional emission spectrum is close to the four-dimensional spectrum at the same Hawking temperature is supported by Figure 8.1, but the figure caption should state the fixed parameter (here T_BH = 150 keV) and the normalization convention for dN/dt, since the curves are otherwise easy to misinterpret as absolute rates.","section":"§8.1","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The physical interpretation of the negative Weyl energy density rho_BH < 0 around the black hole is explained, but the text would benefit from an explicit statement that this quantity is a projection artifact rather than a physical fluid, to avoid the impression that accretion creates a new energy component with negative energy density.","section":"§7.3 and §11.1.2","authors_acknowledge":null,"authors_acknowledge_p":null}],"recommendation":"major_revision","confidential_remarks":"The core of the thesis is the accretion calculation and its consequences; the review chapters are competent but not the main contribution. The strongest single concern, also identified in the stress-test note, is that the small-BH condition r0 << l is not checked along the mass trajectories that produce the headline f_PBH = 1 regions. This is fixable within the manuscript's scope if the author can display r0(t)/l and the associated validity bounds, or alternatively quantify the leading corrections. I would also ask the editor to ensure that the dependence of the constraint analysis on the author's previous works [61, 62] is clearly delineated, since the thesis presents those results as part of the argument chain but does not fully reproduce them here."},"author_rebuttal":null,"desk_editor":{"model":"deepseek/deepseek-v4-flash","letter":"Two things to know before you open it. The genuinely new piece is the Michel accretion treatment of small PBHs in RS-II; earlier work by Guedens-Clancy-Liddle, Majumdar, and Tikhomirov-Tsalkou used Bondi. The headline conclusion, f_PBH = 1 in surviving parameter windows, should be read as a model result conditional on a geometry assumption the thesis itself flags as uncertain.\n\nWhat is good. The Michel calculation is a real extension, and the t^0.33 growth discrepancy is concrete and checkable. The perturbation chapter doing the group-velocity analysis is honest work: it shows v_g approaches c_s in the quadratic regime and defuses the old effective-sound-speed confusion. The thesis is remarkably candid about its own foundations: Section 7.4.6 states the two-regime problem flatly, Section 7.3 lays out the non-uniqueness of brane black holes, and Section 4.6 warns against the effective-fluid interpretation. It uses public codes (BlackMax, CosmoLED), states methods, and cites the greybody-factor literature properly.\n\nSoft spots, in proportion. The main one is exactly the stress-test concern: accretion is computed in the Schwarzschild-Tangherlini metric, valid for r0 << l, but the text never displays r0(t)/l along the trajectories that produce f_PBH = 1. Since M grows by orders of magnitude and r0 grows as M^(1/2), this check matters. That said, the small-BH window is enormous: with l <= 44 microns, r0 << l means M << M4^2 l, roughly 10^25-10^26 g, so the trajectories probably stay inside the valid regime. This is a closable gap, not a demonstrated failure, but it should be closed in print rather than left implicit. Second, the Michel validity claims in Section 11.3 are plausible but the detailed verification is not checkable from the excerpt. Minor, but worth requesting.\n\nTwo corrections to the reviewer notes. The negative Weyl energy density around the black hole is not an invented entity; it is the standard SMS projection described in the Gregory et al. literature. And building on the author's own papers for accretion and evaporation is normal thesis structure, not circularity.\n\nWho this is for: PBH phenomenologists and braneworld cosmologists. It deserves a serious referee. My recommendation: send it to review, with one pointed request attached, which is to display the r0(t)/l trajectories and the Michel validity domain for the claimed dark-matter regions.","headline":"A serious thesis with one genuinely new calculation and one over-reach: the Michel accretion treatment of RS-II PBHs is real work, but the all-dark-matter conclusion needs to be read as a model result until the small-black-hole consistency check is displayed.","tokens_in":62568,"tokens_out":4772,"would_cite":true,"duration_ms":41735,"reading_group":"maybe","serious_thinker":"yes","would_accept_peer_review":true},"pith_extraction":{"msc":["83E15","83C57","83F05","83C47"],"pacs":["04.50.-h","04.70.-s","98.80.-k","95.35.+d"],"model":"deepseek/deepseek-v4-flash","headline":"In a warped fifth dimension, primordial black holes accrete far faster than standard cosmology predicts, reopening the possibility that they are all of the dark matter.","keywords":["primordial black holes","braneworld cosmology","Randall–Sundrum Type II model","dark matter","black hole accretion","Hawking evaporation","extra dimensions","Weyl tensor"],"falsifier":"Settle it by construction: numerically solve the five-dimensional bulk Einstein equations for a small brane-localized black hole with $r_0 \\ll \\ell$, extract the induced metric on the brane, and recompute the Michel accretion rate and the mass-growth exponent; if the growth law deviates from the Schwarzschild–Tangherlini-based $t^{0.33}$ scaling, the central claim fails in its present form. Observationally, the claim would be settled by a survey in the claimed viable window — for instance the unresolved diffuse gamma-ray background or CMB spectral-distortion limits — excluding $f_{\\mathrm{PBH}} = 1$ at the masses that enhanced accretion maps onto sub-Planckian formation masses.","tokens_in":62984,"feed_emoji":"🕳️","tokens_out":14851,"duration_ms":88155,"temperature":0.7,"pith_summary":"This thesis argues that in the Randall–Sundrum Type II braneworld — a universe with one warped extra dimension — light primordial black holes grow far more than standard cosmology allows. The central result is that higher-dimensional gravity enhances early-Universe accretion, so the author's black hole masses diverge from earlier estimates as $t^{0.33}$, reaching several orders of magnitude by the end of the strong-accretion epoch. Because small braneworld black holes also evaporate more slowly than their four-dimensional counterparts, the thesis finds viable parameter regions in which these black holes constitute all of the dark matter, even when they formed below the effective four-dimensional Planck scale. A sympathetic reader would care because the claim turns an exotic geometric scenario into a specific, observationally testable dark-matter candidate whose evolution record is written in today's mass spectrum.","feed_headline":"Supercharged by a hidden dimension: early black holes grow far faster","feed_subtitle":"Under five-dimensional gravity, black holes grow faster by a t^0.33 factor, keeping them viable as all of the dark matter.","key_machinery":"The load-bearing machinery is a chain of three elements. First, the RS-II modified Friedmann equation, $H^2 \\propto \\rho + \\rho^2/(2\\lambda)$, whose quadratic high-energy regime makes the cosmological fluid dilute more slowly at early times. Second, the Schwarzschild–Tangherlini metric taken as the near-horizon geometry of a small brane black hole, which fixes the critical accretion radius $r_{\\mathrm{cr}}^2 = (1+w)r_0^2/(2w)$ and critical velocity $u_{\\mathrm{cr}}^2 = w/(1+w)$ in Michel's formalism. Third, a new conserved quantity $A_3 = \\rho/\\lambda + (4/3)\\rho_{\\Psi}/(\\rho+p)$ emerging from the non-local conservation equation for the projected bulk Weyl tensor, which forces the 'Weyl cloud' around the black hole to grow in lockstep with the accretion rate $\\dot{M}$, since energy conservation in the projected theory requires the geometric remainder terms to transform consistently as mass flows in. Michel's quasi-steady, test-fluid framework then yields a fully analytic accretion rate with a single effective sound speed, and five-dimensional greybody factors supply the modified Hawking spectra. The pith of the mechanism is that the dark-radiation degree of freedom is not passive but is constrained, through $A_3$, to track the black hole's growth.","core_discovery":"The paper's central claim is that accretion onto light primordial black holes in the early RS-II brane universe is substantially stronger than previously calculated, and that this reshapes the mass mapping between formation and today. Working with Michel's relativistic accretion formalism inside the covariant Shiromizu–Maeda–Sasaki description of the brane, the author derives a critical radius $r_{\\mathrm{cr}}^2 = (1+w)r_0^2/(2w)$ for the Schwarzschild–Tangherlini geometry, obtains the velocity and energy-density profiles of the inflow, and finds a mass-growth law whose deviation from earlier estimates scales as $t^{0.33}$. On the evaporation side, a small braneworld black hole obeys $T_{\\mathrm{BH}} \\propto M^{-1/2}$ and has a lifetime $\\tau \\propto M^2$, so it is colder and longer-lived than a four-dimensional black hole of the same mass. Combining the two effects, the thesis identifies regions of parameter space where primordial black holes account for the entirety of dark matter while remaining consistent with reanalysed bounds from Hawking radiation, diffuse gamma-ray backgrounds, microlensing, and cosmic microwave background energy injection; notably, the progenitors may lie below the effective four-dimensional Planck scale. The thesis states plainly that these conclusions assume the Schwarzschild–Tangherlini metric near the horizon, since no exact solution interpolating to the far-field Garriga–Tanaka regime is known.","pith_inferences":["Going beyond the paper's own claims: if the enhanced accretion picture holds, the decisive probes are not the surviving black holes themselves but the energy they injected while growing; the thesis's reanalysis points to gamma-ray and CMB constraints as the live ones, so modest improvements in those surveys could close or confirm the dark-matter window.","A natural step not taken in the thesis would be to re-run the accretion machinery with the alternative DMPR tidal Reissner–Nordström geometry, whose Weyl equation of state ($w_{\\Psi} = -2$ versus $-1$ for Schwarzschild–Tangherlini) would test how sensitive the $t^{0.33}$ growth law is to the unknown bulk geometry.","Another underexplored extension is to couple the enhanced accretion to the formation epoch itself: the thesis notes that no dedicated analysis of small-black-hole collapse in the high-energy regime exists, so a collapse-plus-accretion history could shift the inferred initial mass function further."],"forward_implications":["The initial-to-final mass mapping for primordial black holes is fundamentally altered: black holes in the observable window today can have formed at masses below the effective four-dimensional Planck scale.","The standard constraint 'master plot' shifts in the braneworld, leaving viable regions with $f_{\\mathrm{PBH}} = 1$ — primordial black holes as the whole of dark matter — that remain allowed by reanalysed evaporation, gamma-ray, microlensing, and CMB bounds.","Small RS-II black holes live longer than equal-mass four-dimensional black holes ($\\tau \\propto M^2$ rather than $M^3$), so evaporation-based upper limits are generically weakened.","The accretion flow admits a self-consistent analytic Michel description over a much wider parameter range in RS-II than in standard cosmology, where time-dependent self-similar solutions and numerical simulations are usually required."],"supporting_citations":[{"why":"Supplies Michel's relativistic accretion formalism, whose critical-point regularity conditions pin the accretion rate on the Schwarzschild–Tangherlini geometry.","marker":"[227]"},{"why":"Provides the covariant Shiromizu–Maeda–Sasaki brane equations and the non-local conservation equation from which the new conserved quantity A3 is derived.","marker":"[29]"},{"why":"Guedens–Clancy–Liddle accretion estimate that the thesis recalculates; its strong-accretion result is the comparison baseline for the t^0.33 divergence.","marker":"[221]"},{"why":"Majumdar's independent accretion estimate, the second earlier result whose black-hole masses the thesis's differ from.","marker":"[222]"},{"why":"Tikhomirov–Tsalkou update adding frequent-collision corrections (F ≈ 1.54) that the thesis also re-examines.","marker":"[223]"},{"why":"The Schwarzschild–Tangherlini solution used as the near-horizon geometry of small brane black holes.","marker":"[43]"},{"why":"Defines the Randall–Sundrum Type II single-brane model and the warped geometry that produces the modified Friedmann equation.","marker":"[10]"},{"why":"Gives the far-field Garriga–Tanaka metric; the absence of a metric interpolating between it and the near-horizon solutions is the two-regime caveat limiting the central claim.","marker":"[77]"},{"why":"Computes the five-dimensional greybody factors for brane-localised Standard Model fields used in the modified Hawking spectra.","marker":"[82]"},{"why":"Supplies the heuristic and geometric-optics arguments that brane-channel emission dominates bulk emission, justifying the evaporation treatment.","marker":"[88]"}],"fun_headline_variants":["Hidden dimension boosts early black hole growth","Braneworld gravity speeds up early black hole accretion","Faster-growing brane black holes could be all dark matter","Extra dimension changes primordial black hole mass history","Five-dimensional effects make light black holes viable dark matter"],"cache_read_input_tokens":0,"weakest_assumption_plain":"The load-bearing premise is that a small braneworld black hole's near-horizon geometry is the Schwarzschild–Tangherlini metric and that Michel's quasi-steady, test-fluid accretion formalism applies in the early cosmological epoch; the thesis itself flags that no known solution interpolates to the far-field Garriga–Tanaka metric, so if the true brane-localized geometry differs at the horizon, the accretion rate and the $t^{0.33}$ growth factor would change.","fun_headline_variants_meta":{"raw":{"variants":["Hidden dimension boosts early black hole growth","Braneworld gravity speeds up early black hole accretion","Faster-growing brane black holes could be all dark matter","Extra dimension changes primordial black hole mass history","Five-dimensional effects make light black holes viable dark matter"]},"model":"deepseek/deepseek-v4-flash","effort":"low","cost_usd":0.000143,"raw_usage":{"cost":0.0001431248,"is_byok":false,"cost_details":{"upstream_inference_cost":0.0001431248,"upstream_inference_prompt_cost":4.02948e-05,"upstream_inference_completions_cost":0.00010283},"total_tokens":1795,"prompt_tokens":1230,"completion_tokens":565,"prompt_tokens_details":{"audio_tokens":0,"video_tokens":0,"cached_tokens":984,"cache_write_tokens":0},"completion_tokens_details":{"audio_tokens":0,"image_tokens":0,"reasoning_tokens":502}},"tokens_in":1230,"tokens_out":565,"cost_source":"openrouter_usage","duration_ms":6826,"image_pages":[],"temperature":1.0,"billed_attempts":1,"reasoning_tokens":502,"transport_provider":"openrouter","cache_read_input_tokens":0,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-10-20T09:37:07.429213+00:00","model_set":{"reader":"deepseek/deepseek-v4-flash"},"falsifier":"Settle it by construction: numerically solve the five-dimensional bulk Einstein equations for a small brane-localized black hole with $r_0 \\ll \\ell$, extract the induced metric on the brane, and recompute the Michel accretion rate and the mass-growth exponent; if the growth law deviates from the Schwarzschild–Tangherlini-based $t^{0.33}$ scaling, the central claim fails in its present form. Observationally, the claim would be settled by a survey in the claimed viable window — for instance the unresolved diffuse gamma-ray background or CMB spectral-distortion limits — excluding $f_{\\mathrm{PBH}} = 1$ at the masses that enhanced accretion maps onto sub-Planckian formation masses.","supporting_citations":[{"cited_title":"Matter Accretion by Brane-World Black Holes","cited_arxiv_id":null,"evidence_quote":"Supplies Michel's relativistic accretion formalism, whose critical-point regularity conditions pin the accretion rate on the Schwarzschild–Tangherlini geometry."},{"cited_title":"The Einstein equations on the 3-brane world","cited_arxiv_id":null,"evidence_quote":"Provides the covariant Shiromizu–Maeda–Sasaki brane equations and the non-local conservation equation from which the new conserved quantity A3 is derived."},{"cited_title":"Tolman IV solution in the Randall-Sundrum Braneworld","cited_arxiv_id":"1311.1844","evidence_quote":"Guedens–Clancy–Liddle accretion estimate that the thesis recalculates; its strong-accretion result is the comparison baseline for the t^0.33 divergence."},{"cited_title":"Primordial black holes in braneworld cosmologies: Accretion after formation","cited_arxiv_id":null,"evidence_quote":"Majumdar's independent accretion estimate, the second earlier result whose black-hole masses the thesis's differ from."},{"cited_title":"Domination of Black Hole Accretion in Brane Cosmology","cited_arxiv_id":null,"evidence_quote":"Tikhomirov–Tsalkou update adding frequent-collision corrections (F ≈ 1.54) that the thesis also re-examines."},{"cited_title":"Nuovo Cim.27, 636-651","cited_arxiv_id":null,"evidence_quote":"The Schwarzschild–Tangherlini solution used as the near-horizon geometry of small brane black holes."},{"cited_title":"An Alternative to Compactification","cited_arxiv_id":"hep-th/9906064","evidence_quote":"Defines the Randall–Sundrum Type II single-brane model and the warped geometry that produces the modified Friedmann equation."},{"cited_title":"Gravity in the Randall-Sundrum Brane World","cited_arxiv_id":null,"evidence_quote":"Gives the far-field Garriga–Tanaka metric; the absence of a metric interpolating between it and the near-horizon solutions is the two-regime caveat limiting the central claim."},{"cited_title":"Hawking Radiation from a (4+n)-dimensional Black Hole: Exact Results for the Schwarzschild Phase","cited_arxiv_id":"hep-ph/0309054","evidence_quote":"Computes the five-dimensional greybody factors for brane-localised Standard Model fields used in the modified Hawking spectra."},{"cited_title":"Black Holes Radiate Mainly on the Brane","cited_arxiv_id":null,"evidence_quote":"Supplies the heuristic and geometric-optics arguments that brane-channel emission dominates bulk emission, justifying the evaporation treatment."}],"review_version":1}