{"id":"eea2e3ef-2f86-45c9-8dc8-250eee385bcb","arxiv_id":"2009.03363","paper_version":3,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":5.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":0,"one_line_summary":"Extremal magnetic black holes would emit electromagnetic radiation during binary inspirals that can exceed the power of the brightest known gamma-ray bursts, with distinctive orbital and gravitational-wave signatures.","lead":"This paper surveys observable signatures of magnetically charged black holes, computing their magnetic fields, stable orbits, and the electromagnetic and gravitational waves emitted when they spiral into other black holes. It argues these objects would produce electromagnetic flares far brighter than known sources, giving astronomers a way to look for them.","discovery_kind":"unclear","skeptic_critique":{"model":"selfhosted/deepseek-v4.1-flash","headline":"The paper's own Sec. II concedes that near-extremal magnetic black holes may not form or survive, yet every quantitative signature in Secs. III–VI is evaluated at Q_B = M; the reader flagged this but treated it as a soft caveat rather than the load-bearing premise it is.","rationale":"The reader's weakest_assumption correctly names the near-extremality/survival premise, and I agree it is the load-bearing one. Where I differ is in weighting: the reader calls it a caveat that 'warrants a conditional verdict' but does not trace how far the quantitative claims move when the premise is relaxed. The paper's own Eq. 7 gives Q_B/M ≲ 10^-4 from monopole accretion, and Eq. 49 shows the horizon field scales as (Q_B/M)/(1+√(1-(Q_B/M)^2))^2, so at that charge the field is ~10^8 times smaller than the extremal value plotted in Fig. 2. The 'spectacular' EM fluxes of Sec. V and the GRB comparison in Fig. 5 inherit the same suppression. This is an internal consistency issue between Sec. II's agnosticism and Secs. III–VI's extremal evaluations, not a dispute with external consensus, so it belongs under correctness risk rather than soundness. The reader's secondary point about neglecting curvature in Sec. V is fair but less load-bearing: the paper explicitly restricts to early inspiral and cites [18] for PN corrections, so that approximation is bounded and acknowledged. The reader's note that the EM power normalization 'deserves a check' is also fair; Eqs. 70 and 73 differ by a factor of four, consistent with the stated superposition argument in Appendix B, and I did not find an arithmetic error there. On balance the paper's derivations (ISCO at 4|Q_B|, OSCO bound Eq. 48, Parker bound Eq. 61) are standard and checkable, and the de Sitter OSCO is a genuine addition. The verdict should remain CONDITIONAL, but the condition should be stated sharply: the abstract's strongest sentence (abstract:s6) should be qualified to the near-extremal regime, with the formation channel either cited or flagged as an open assumption. No change to ACCEPT or REJECT is warranted; the paper is honest about its approximations and its debt to [11,17,18], and the new results stand independently of the extremality question.","tokens_in":87902,"tokens_out":99423,"duration_ms":1872092,"concrete_test":"Recompute Fig. 2 and Eq. 70 at a representative non-extremal charge, e.g. Q_B/M = 10^-2 and 10^-4 (the accretion bound of Eq. 7), using the full factor (Q_B/M)/(1+√(1-(Q_B/M)^2))^2 in Eq. 49. If the horizon field at M = 10 M_⊙ drops below the Magnetar band (10^9 T) for Q_B/M ≲ 10^-2, then the abstract's 'many orders of magnitude larger than even Magnetars' claim is conditional on a formation channel the paper does not supply, and the abstract should say so explicitly.","verdict_should_be":"CONDITIONAL","load_bearing_attack":"The central quantitative claims (abstract:s6, Sec. V–VI) are all evaluated in the extremal limit Q_B = M. The paper is explicit that this limit is not derived: Sec. II states 'We will adopt an agnostic viewpoint about the exact details of their cosmological origin,' and its own charging argument (Eq. 7) gives Q_B/M ≲ 10^-4 for accretion of heavy monopoles, i.e. five orders of magnitude below extremality. The only route the paper offers to near-extremality is the enhanced Hawking-radiation argument of [11], which is cited, not re-derived, and which itself requires the black hole to start already close to extremal or to be very light. So the chain is: (i) assume Q_B ≈ M; (ii) then B_horizon ∝ M^-1 with a fixed coefficient (Eq. 49); (iii) then the EM power in Eq. 70 and the 'spectacular' fluxes follow. Step (ii) is where the load-bearing weight sits, because the magnetic field at the horizon scales as (Q_B/M)/(1+√(1-(Q_B/M)^2))^2, which for Q_B/M = 10^-4 collapses by ~10^8 relative to the extremal value quoted in Fig. 2. The paper's headline comparison to Magnetars (B ≳ 10^9 T) survives only for M ≲ 10^-6 M_⊙ at extremality; at the accretion-limited charge it fails for essentially all astrophysical masses. This is not a disagreement with consensus — it is an internal gap between the stated agnosticism about formation (Sec. II) and the quantitative claims that silently assume the extremal limit throughout Secs. III–VI. The reader identified the same premise but graded it a 'soft caveat'; I think it is the single hinge on which the abstract's strongest sentence turns.","agreement_with_reader":"partial"},"referee_report":{"model":"selfhosted/deepseek-v4.1-flash","summary":"The manuscript surveys potential astrophysical signatures of magnetically charged Reissner-Nordstrom black holes, working almost entirely in the extremal limit Q_B = M. It reviews charge-to-mass bounds (Eqs. 2-7), derives horizon locations in asymptotically flat and de Sitter backgrounds (Eqs. 8-18), computes ISCO and OSCO radii for extremal MBHs (Eqs. 30-48), estimates near-horizon magnetic fields and compares them to Magnetars (Eq. 49, Figs. 2-3), derives a Parker-type bound on MBHs as a dark matter component (Eqs. 53-66), and computes electromagnetic and gravitational emission from MBH-BH and MBH-MBH inspirals (Eqs. 67-85, Figs. 4-7). The stated headline is that even where no electroweak corona forms, near-horizon fields and inspiral emissions can vastly exceed known astrophysical sources.","tokens_in":89276,"tokens_out":100006,"duration_ms":1985514,"significance":"If near-extremal magnetic black holes exist, the paper's central observational point is genuinely interesting: the near-horizon field of an extremal MBH scales as 1/M (Eq. 49), so even stellar-mass objects would carry fields far above Magnetar values, and the inspiral Poynting flux (Eqs. 70, 73) would be an unusually bright multi-messenger target. The ISCO/OSCO analysis (Eqs. 37, 46, 48) and the Parker bound (Eq. 64) are simple, checkable, and useful reference results. The paper is honest that it is a survey of potential signatures rather than a detection claim, and it explicitly flags the formation question as open. The value of the work therefore rests on the extremality assumption being at least plausibly realized, which the manuscript asserts rather than demonstrates.","major_comments":[{"comment":"The entire quantitative program of Secs. III-VI is evaluated at Q_B = M, but the paper's own charging argument in Eq. (7) gives Q_B/M < 10^-4 for accretion of heavy monopoles, and Sec. II then states 'We will adopt an agnostic viewpoint about the exact details of their cosmological origin.' The horizon field in Eq. (49) scales as (Q_B/M)/(1+sqrt(1-(Q_B/M)^2))^2, which at Q_B/M = 10^-4 is suppressed by roughly eight orders of magnitude relative to the extremal value plotted in Fig. 2. The abstract's claim [abstract:s6] that fields are 'many orders of magnitude larger than even Magnetars' therefore holds only in a corner of parameter space that the paper does not establish is populated. This is the load-bearing premise of the paper, and it needs either a quantitative formation/survival argument or an explicit statement of the near-extremality range over which each headline number survives. As written, the reader cannot tell which of the 'spectacular' claims are robust to, say, Q_B/M = 0.1 or 0.5.","section":"Sec. II, Eqs. (7) and (49); Secs. III-VI","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The electromagnetic and gravitational inspiral estimates neglect spacetime curvature and treat the emission as flat-space Larmor/dipole radiation, with the stated justification that separations are large compared to horizon radii. But the most striking numbers in Fig. 5 are quoted for separations of a few horizon radii, precisely where the flat-space approximation and the Keplerian relations of Eqs. (76) and (81) are least reliable. The paper should state explicitly the range of a/r_H over which Eqs. (70) and (73) are claimed to be accurate, and should either restrict Fig. 5 to that range or attach an estimated curvature correction. Without this, the comparison to GRB 080916C in Fig. 5 is not a controlled statement.","section":"Sec. V, Eqs. (67)-(73); Sec. VI, Eqs. (77)-(84)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The orbital evolution equations add the electromagnetic energy loss to the quadrupole gravitational loss but keep the Newtonian Keplerian relations and the quadrupole formula unchanged. For extremal MBH-MBH pairs the Coulomb and gravitational forces are equal in magnitude (as the paper notes in Sec. II), so the orbital dynamics is not a small perturbation of the neutral case; the conservative two-body potential is modified at leading order, not just the radiation reaction. The claim that the chirp 'occurs much before' for MBH-MBH (Fig. 7) should be qualified accordingly, or supported by a leading-order effective-one-body or PN treatment of the modified potential. The paper cites [18] for PN corrections but does not incorporate them where they matter most.","section":"Sec. VI, Eqs. (77)-(84)","authors_acknowledge":null,"authors_acknowledge_p":null}],"minor_comments":[{"comment":"The abstract and introduction describe the work as adding 'new results' without identifying which results are new relative to [11], [17], and [18]. A short paragraph distinguishing the new material (e.g. the OSCO expression in Eq. (48), the Parker bound in Eq. (64), the inspiral power estimates) from the review material would help the reader.","section":"Abstract and Sec. I","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The bound Q_B/M < 10^-4 from monopole accretion is quoted without showing the intermediate steps analogous to Eqs. (2)-(6); a sentence spelling out the assumed monopole mass and flux would make the comparison to the electric case transparent.","section":"Sec. II, Eq. (7)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The statement that the orbit at r = |Q_B| is 'stable only in one direction' should be stated more carefully: it is not a stable circular orbit in the usual sense, since radial perturbations toward the horizon plunge. The text does say this, but the phrase 'ostensibly stable' in the sentence introducing Eq. (32) could mislead a casual reader.","section":"Sec. III, Eqs. (32)-(37)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The axis labels and units are difficult to read at the reproduced size, and the overlaid astrophysical scales in Fig. 1 are not identified in the caption. Please enlarge the labels and list each overlaid scale explicitly.","section":"Fig. 1 and Fig. 2","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The corona radius estimate r_corona ~ O(1) mm is quoted without the numerical inputs used; please show the values of m_W, m_H, and q_B inserted.","section":"Sec. IV, Eq. (51)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The symbol beta is defined as (omega a)/2c, but the physical orbital velocity of the MBH about the center of mass is omega a/2 only for equal masses; for unequal masses the boost factor should involve the reduced mass ratio. Please state the equal-mass assumption explicitly at this point rather than only later.","section":"Sec. V, Eq. (67)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"The waveform expressions are given without the standard 1/r and inclination-angle normalizations used elsewhere in the GW literature; a brief note on conventions would help comparison with [83].","section":"Sec. VI, Eq. (85)","authors_acknowledge":null,"authors_acknowledge_p":null},{"comment":"Reference [17] is described as focusing on MBHs with an electroweak corona below 10^-4 M_sun, but the text also says the Parker bound results are 'slightly different' from [17]. A sentence quantifying the difference would be useful.","section":"References","authors_acknowledge":null,"authors_acknowledge_p":null}],"recommendation":"major_revision"},"author_rebuttal":null,"desk_editor":{"model":"selfhosted/deepseek-v4.1-flash","letter":"The useful parts first. The de Sitter outer stable circular orbit for the extremal magnetic Reissner-Nordstrom case (Eqs. 45-48) is a genuine, if small, extension of the known Schwarzschild-dS OSCO, and the coupled electromagnetic-gravitational orbital evolution equations (77-84) for MBH-BH and MBH-MBH are worth having written down in one place, including the factor-of-two shift in the Keplerian relation when Coulomb attraction exactly matches gravity. The EM power normalizations check out: Eq. (70) is the Larmor result for a charge orbiting at a/2, and Eq. (73) is correctly twice a single magnetic dipole with the cross terms averaging to zero. The Parker bound arithmetic is right to within rounding (I get 2.2e-3 rather than 1.7e-3, but that is a rounding-level difference). The paper is candid about its debts to [11,17,18]. Now the soft spots, in order of weight. First, extremality. The stress-test is right that every quantitative claim in Secs. III-VI is evaluated at Q_B = M, and the paper never shows a formation route to that limit for astrophysical masses. But the stress-test overstates one thing: Eq. (7)'s 10^-4 is a bound on one charging channel (accretion of heavy monopoles), not a bound on the charge itself, and the paper says so explicitly. The real gap is narrower and sharper: the only route offered to near-extremality is the Hawking-radiation argument of [11], which applies to M < 10^-4 M_sun. For stellar-mass and up, there is no route. At Q_B/M = 10^-4 the horizon field drops by four to five orders, so the abstract's 'many orders of magnitude above Magnetars' survives only marginally for stellar-mass and fails for M > 60 M_sun. That is the hinge under abstract:s6, and it deserves a sentence in the paper, not just the agnosticism disclaimer. Second, the gamma^4 'further enhancement' in Sec. V is double counting: Eq. (67) is already the full Lienard expression with beta, and integrating it gives the relativistic power. Minor, but should be fixed. Third, the OSCO is presented as a bound (Eq. 48), not a location; 'numerically the bound is relatively good' is doing more work than a bound should. Fourth, the GRB comparison in Fig. 5 is isotropic-equivalent versus beamed, not like-for-like. Who should read it: anyone doing magnetic black hole or exotic-compact-object phenomenology, or thinking about electromagnetic counterparts to gravitational-wave inspirals. It is a good map of the terrain. Recommendation: send it out. The calculations are checkable, the new results are real if modest, and the extremality gap is exactly the kind of thing a referee should force the authors to state plainly rather than bury in Sec. II.","headline":"A competent, honest survey of extremal magnetic black hole phenomenology; the new results are modest, and the whole edifice still rests on an unearned extremality assumption that the paper acknowledges but never closes.","tokens_in":30378,"tokens_out":4306,"duration_ms":81273},"pith_extraction":{"msc":[],"pacs":["04.70.Bw","04.30.-w","95.35.+d","14.80.Hv"],"model":"selfhosted/deepseek-v4.1-flash","headline":"Magnetically charged black holes would be the brightest compact objects in the sky","keywords":["magnetically charged black holes","magnetic monopoles","Reissner-Nordstrom black hole","extremal black holes","innermost stable circular orbit","Parker bound","gravitational waves","dark matter"],"falsifier":"A gravitational-wave inspiral whose frequency derivative matches the standard neutral-binary prediction to high precision, with no excess attributable to the $Q_B^2 M^{-1} u^3$ term, would rule out a magnetic charge large enough to matter for these signatures; conversely, a compact binary showing an anomalously fast chirp together with a periodic beamed electromagnetic counterpart would confirm the picture.","tokens_in":30722,"feed_emoji":"🧲","tokens_out":2904,"duration_ms":56283,"temperature":0.7,"pith_summary":"The paper asks what a black hole carrying magnetic charge, rather than electric charge, would look like to astronomers, and argues that the answer is dramatic enough to be searched for now. The reason to care is that electric charge on a black hole is stripped away almost instantly by infalling ionised gas, whereas magnetic charge has no light carriers to discharge it, so a magnetically charged black hole could survive from the early universe to today. Working in the extremal limit where the magnetic charge equals the mass, the authors compute the near-horizon fields, the innermost stable orbit, bounds on how much dark matter such objects could make up, and the electromagnetic and gravitational radiation from binary inspirals involving them. Their central claim is that even where the fields are too weak to restore electroweak symmetry, they still dwarf those of magnetars, and that an inspiralling pair would radiate electromagnetic power rivalling the most energetic gamma-ray bursts while its gravitational-wave frequency chirps earlier than a neutral pair's. The paper is a survey of signatures and order-of-magnitude estimates rather than a detection or a derivation of how such objects would form.","feed_headline":"Magnetic black holes would outshine magnetars and GRBs","feed_subtitle":"If near-extremal magnetic charges survive, their binary inspirals would radiate more power than a gamma-ray burst.","key_machinery":"The load-bearing device is the extremal condition $M = |Q_B|$, which makes the Reissner-Nordstrom metric depend on a single scale and turns every formula into a clean power of the mass. It gives a horizon at $r_H = |Q_B|$, a vanishing Hawking temperature, an ISCO at $4|Q_B|$, and an exact cancellation between gravitational attraction and magnetic repulsion for like charges (or a doubling for opposite charges). In de Sitter space the same condition makes the outer event horizon and the cosmological horizon share a temperature, which the authors read as thermodynamical stability, and produces an outer stable circular orbit whose position they bound with the Lagrange-Zassenhaus root bound rather than solving the quartic exactly. For the radiation estimates the machinery is electromagnetic duality, which maps the standard electric Lienard formula and the fields of two oscillating dipoles onto their magnetic analogues, plus the Parker bound, which converts the energy a charged object extracts from a galactic field over its regeneration time into a limit on the object's abundance.","core_discovery":"The paper's central claim is that an extremal magnetic black hole, one whose magnetic charge equals its mass in gravitational units, is a distinctly bright and distinctly audible astrophysical object. At the horizon the magnetic field is $B = 2.34^{15}$ Tesla times $M_*/M$, so across a wide mass range it exceeds a magnetar's field by many orders of magnitude even where no electroweak corona forms. The innermost stable circular orbit sits at $r = 4|Q_B|$, close to the horizon, so accreting matter and inspiralling companions live in an extreme field. For binary inspirals the authors compute, using a Lienard-type formula mapped to magnetic charges, that a magnetic-plus-neutral pair radiates electromagnetic power $P = 2.34^{15}$-scaled as $a^{-4}$, or $a^{-4}$ in separation, and that a magnetic-plus-magnetic pair radiates four times more; at fixed separation in units of the horizon radius the extremal prediction is mass-independent. The radiated power can exceed that of Type Ia supernovae and approach GRB 080916C. Because the same energy loss drives the orbit, the gravitational-wave frequency evolves with an extra term scaling as $Q_B^2 M^{-1} u^3$ on top of the standard $u^{11/3}$ inspiral, so the chirp begins earlier than for neutral black holes. Finally, requiring that magnetic black holes not drain the galactic magnetic field over its regeneration time bounds their dark matter fraction at $f_{DM} < 1.7^{-3}$ for the extremal case.","pith_inferences":["The beamed emission during inspiral is a natural candidate for periodic radio transients: an object whose beam sweeps past Earth once per orbit would produce a repeating, slowly rising-frequency signal, which is a different observational target than a one-off burst.","The mass-independence of the extremal inspiral power at fixed separation in horizon units means an observed luminosity alone cannot fix the mass; a coincident gravitational-wave measurement of the chirp would be needed to break the degeneracy.","If near-extremal magnetic black holes are as long-lived as the paper assumes, they would also accrete from the interstellar medium, and the resulting steady synchrotron emission may be a more accessible, if less spectacular, target than inspiral flares.","The same duality machinery could be applied to a magnetic black hole orbiting a neutron star, where the companion's own magnetosphere would interact with the hole's field and possibly produce a distinct precursor signal."],"forward_implications":["If extremal magnetic black holes exist at stellar or intermediate masses, their binary inspirals would be electromagnetic sources whose luminosity rivals gamma-ray bursts, with a beamed, headlight-like emission pattern that sweeps the sky once per orbit as the orbit tightens.","Gravitational-wave searches would see a chirp that runs ahead of the neutral-black-hole prediction, so a measured excess in $d\\nu_{GW}/dt$ beyond the standard inspiral term would be a signature of magnetic charge rather than of mass alone.","The Parker bound on magnetic-field depletion limits magnetic black holes to a small fraction of dark matter, so any dark matter interpretation of a compact-object population must contend with that ceiling.","The existence of an outer stable circular orbit in the de Sitter case sets a maximum radius for bound orbits around such objects, a boundary absent in flat or anti-de Sitter backgrounds.","Because the near-horizon fields exceed magnetar fields over a wide mass range, accretion onto such objects, not just inspiral, would be an extreme-field laboratory for quantum field theory in curved space."],"supporting_citations":[{"why":"Supplies the framework the whole paper builds on: magnetic black holes, near-horizon field strengths, and electroweak symmetry restoration in the corona.","marker":"[11]"},{"why":"Prior phenomenology of low-mass magnetic black holes with electroweak coronas, including the use of M31 magnetic field data to strengthen the Parker bound.","marker":"[17]"},{"why":"Original Parker bound on magnetic monopoles from survival of the galactic magnetic field, which the paper adapts to magnetic black holes.","marker":"[65]"},{"why":"Provides the form of the Parker bound and the coherence-length and regeneration-time parameters the paper's dark matter fraction limit follows.","marker":"[66]"},{"why":"Establishes the outer stable circular orbit in Schwarzschild-de Sitter spacetime, the feature the paper extends to the magnetic case.","marker":"[55]"},{"why":"Gives the approximate location of the outer stable orbit and its astrophysical interpretation, which the paper's de Sitter analysis parallels.","marker":"[56]"},{"why":"Peters-Mathews gravitational-wave power formula for eccentric binaries, the baseline against which the modified chirp evolution is computed.","marker":"[90]"},{"why":"Source for the circularisation of orbits by radiation reaction and for the relation between orbital and gravitational-wave frequency.","marker":"[83]"},{"why":"Supplies the enhanced Hawking radiation argument via massless 1+1 dimensional chiral fermions in a magnetic field, which underpins the claim that magnetic black holes can be long-lived.","marker":"[63]"},{"why":"The magnetar field benchmark against which the paper's near-horizon magnetic fields are compared.","marker":"[4]"}],"fun_headline_variants":["Magnetic black holes could outshine supernovae during binary inspiral","Magnetic black hole pairs radiate near gamma-ray burst power","Magnetic black hole chirps start earlier than neutral black holes","Galactic magnetic fields cap magnetic black hole dark matter","These are astrophysical hints, not detections, for magnetic black holes"],"cache_read_input_tokens":0,"weakest_assumption_plain":"The whole edifice rests on magnetic black holes actually forming with charge close to the extremal value and then surviving to the present day, a premise the authors explicitly decline to derive when they write that they will adopt an agnostic viewpoint about the exact details of their cosmological origin.","fun_headline_variants_meta":{"raw":{"variants":["Magnetic black holes could outshine supernovae during binary inspiral","Magnetic black hole pairs radiate near gamma-ray burst power","Magnetic black hole chirps start earlier than neutral black holes","Galactic magnetic fields cap magnetic black hole dark matter","These are astrophysical hints, not detections, for magnetic black holes"]},"model":"selfhosted/deepseek-v4.1-flash","effort":"low","attempts":1,"cost_usd":0.0,"raw_usage":{"total_tokens":2133,"prompt_tokens":1115,"completion_tokens":1018,"prompt_tokens_details":null,"completion_tokens_details":{"reasoning_tokens":943}},"tokens_in":1115,"tokens_out":1018,"duration_ms":17514,"image_pages":[],"temperature":1.0,"reasoning_budget":50,"reasoning_tokens":943,"transport_provider":"selfhosted","cache_read_input_tokens":0,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-11-12T03:51:40.989299+00:00","model_set":{"reader":"selfhosted/deepseek-v4.1-flash"},"pipeline_version":"pith-pipeline@v1.5.0-archive-selfhost","input_kind":null,"input_chars":null,"input_total_chars":null,"passes_missing":null,"published_standing":null,"published_confidence":null,"objection_audit":null,"run_record":null,"basis":{"kind":"not_recorded","source":null,"chars_given":null,"chars_total":null},"receipt":null,"falsifier":"A gravitational-wave inspiral whose frequency derivative matches the standard neutral-binary prediction to high precision, with no excess attributable to the $Q_B^2 M^{-1} u^3$ term, would rule out a magnetic charge large enough to matter for these signatures; conversely, a compact binary showing an anomalously fast chirp together with a periodic beamed electromagnetic counterpart would confirm the picture.","supporting_citations":[{"cited_title":"Comments on magnetic black holes","cited_arxiv_id":"2004.06084","evidence_quote":"Supplies the framework the whole paper builds on: magnetic black holes, near-horizon field strengths, and electroweak symmetry restoration in the corona."},{"cited_title":"Phenomenology of Magnetic Black Holes with Electroweak-Symmetric Coronas","cited_arxiv_id":"2007.03703","evidence_quote":"Prior phenomenology of low-mass magnetic black holes with electroweak coronas, including the use of M31 magnetic field data to strengthen the Parker bound."},{"cited_title":"Primordial Black Holes as Dark Matter: Recent Developments","cited_arxiv_id":"2006.02838","evidence_quote":"Original Parker bound on magnetic monopoles from survival of the galactic magnetic field, which the paper adapts to magnetic black holes."},{"cited_title":"Astrophys. J. 160, 383","cited_arxiv_id":null,"evidence_quote":"Provides the form of the Parker bound and the coherence-length and regeneration-time parameters the paper's dark matter fraction limit follows."},{"cited_title":"Innermost and outermost stable circular orbits in the presence of a positive cosmological constant","cited_arxiv_id":null,"evidence_quote":"Gives the approximate location of the outer stable orbit and its astrophysical interpretation, which the paper's de Sitter analysis parallels."},{"cited_title":"GW170817/GRB 170817A/AT2017gfo association: some implications for physics and astrophysics","cited_arxiv_id":"1710.05805","evidence_quote":"Peters-Mathews gravitational-wave power formula for eccentric binaries, the baseline against which the modified chirp evolution is computed."},{"cited_title":"Nucl. Phys. B 236, 90","cited_arxiv_id":null,"evidence_quote":"Source for the circularisation of orbits by radiation reaction and for the relation between orbital and gravitational-wave frequency."},{"cited_title":"The strongest cosmic magnets: Soft Gamma-ray Repeaters and Anomalous X-ray Pulsars","cited_arxiv_id":"0804.0250","evidence_quote":"The magnetar field benchmark against which the paper's near-horizon magnetic fields are compared."}],"lane_accuracy":{"status":"not yet measured","lane":{"model":"selfhosted/deepseek-v4.1-flash","input_kind":null},"url":"https://pith.science/accuracy"},"review_version":1}