{"id":"6fbb8c35-e06b-4004-812f-bf0ee9269b6b","arxiv_id":"1908.10882","paper_version":2,"verdict":"CONDITIONAL","confidence":"MODERATE","novelty_score":5.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":9,"one_line_summary":"Tidal disruption remnants around supermassive black holes can emit TeV-PeV neutrinos from three disk states, with predicted light curves that distinguish magnetically arrested disks from ordinary accretion flows.","lead":"This paper calculates when a star shredded by a supermassive black hole can turn some of its debris into high-energy neutrinos. It identifies three disk states that should emit detectable neutrinos and gives the energies and fade rates to look for.","discovery_kind":"new_application","skeptic_critique":{"model":"deepseek-v4-flash","headline":"The predicted PeV neutrinos from the non-MAD RIAF scale as ζ^3 β_plasma^{-2}, so the uncalibrated fiducial values ζ=0.1 and β_plasma=3 are the load-bearing assumption; the published 67/80 TeV inconsistency is secondary.","rationale":"The paper's central claim is a set of absolute predictions for three TDE disk states. For these predictions to hold, stochastic Fermi-II acceleration must operate with the adopted turbulence amplitude and field strengths. The weakest link is not the standard acceleration formalism but the fiducial values: the non-MAD RIAF maximum energy is extraordinarily sensitive, γ_diff ∝ ζ^3 β_plasma^{-2}, so plausible variations in unmeasured parameters erase the PeV signal. The reader's weakest assumption identified ζ=0.1 and the field strengths; I agree and sharpen the sensitivity with the explicit scaling. A secondary internal inconsistency in the quoted peak neutrino energy reinforces that the quantitative predictions have not been fully cross-checked. Because the paper is explicitly a model with fiducial parameters and does not provide a sensitivity study or independent calibration of ζ and ηcr, the appropriate verdict remains CONDITIONAL; my read does not change the reader's verdict.","tokens_in":24649,"tokens_out":18878,"duration_ms":183513,"concrete_test":"Recompute Ep,diff and Eν,pk for the non-MAD RIAF using equations (44)-(47) and (62) at (ζ=0.03, β_plasma=3) and at (ζ=0.1, β_plasma=27), holding all other fiducial parameters fixed. If either single-parameter variation moves Eν,pk below 10 TeV, the claim that TDE RIAFs are PeV neutrino sources is not robust to plausible turbulence or field-strength uncertainties, and the conditional status of the paper is confirmed.","verdict_should_be":"UNCHANGED","load_bearing_attack":"Equation (33) fixes the stochastic acceleration time with ζ=0.1, stated as 'Throughout this paper, ζ=0.1 is adopted', and equations (31) and (48) set the magnetic field strength through the plasma beta (fiducial β_plasma=3) or the MAD scaling. In the non-MAD RIAF, the maximum proton energy is set by t_acc=t_diff; equation (47) gives γ_diff ∝ ζ^3 β_plasma^{-2} for s=5/3. Lowering ζ to 0.03 (factor 3.3) or raising β_plasma to 27 (factor 9) suppresses γ_diff by factors of roughly 30-80, so Ep,diff falls from 0.45 PeV to a few times 10 TeV, and Eν,pk≈0.78 Ep,diff drops below 10 TeV, removing one of the three claimed promising sites. No observational or numerical constraint on ζ in TDE disks is provided, so the absolute energy predictions are not anchored. The super-Eddington MAD case is less sensitive to ζ (γ_sync ∝ ζ^{3/4} in equation 55), but its luminosity still depends on the unvalidated ηcr=0.1. The text also contains an unresolved inconsistency in the headline neutrino energy (67 TeV in the abstract and conclusions versus 80 TeV in Section 3, with different mass normalizations), which should be corrected before the quantitative claims are used.","agreement_with_reader":"agree"},"referee_report":{"model":"deepseek-v4-flash","summary":"The manuscript studies high-energy neutrino production in tidal disruption remnants by considering four evolutionary phases plus the magnetically arrested disk (MAD) state. It computes, with a single-zone model and stochastic (Fermi-II) acceleration, the maximum proton energy and neutrino spectrum for six sites, concluding that the super-Eddington MAD phase and the RIAF phases of both non-MAD and MAD disks are the promising neutrino emitters. The predicted peak neutrino energies scale steeply with black hole mass, and the light curves have distinctive decay indices (t^-65/24 for the super-Eddington MAD, t^-10/3 for the non-MAD RIAF). The paper also estimates gamma-ray opacity, baryon loading, detection horizons, and the diffuse neutrino background contribution.","tokens_in":25007,"tokens_out":12228,"duration_ms":119656,"significance":"The strength of the paper is that it maps the parameter space of TDE remnants in a transparent, analytic way and produces falsifiable predictions: the mass-scaled peak energies, the t^-10/3 light curve, and the t^-65/24 decay are concrete signatures that can be tested by future surveys. The model is constructed before the diffuse-flux comparison, so the predictions are not tuned to an observable. The main weakness is that the absolute energies and luminosities are controlled by three uncalibrated parameters (zeta=0.1, plasma beta=3, eta_cr=0.1), with the acceleration-time balance entering through Eqs. (33), (31), and (47). If these parameters are off by modest factors, the non-MAD RIAF prediction falls below 10 TeV. The paper is therefore a useful framework, but its quantitative claims are conditional.","major_comments":[{"comment":"The absolute maximum proton energy in the non-MAD RIAF case is set by the uncalibrated combination gamma_diff ∝ ζ^3 β_p^-2 (Eq. 47, with the plasma beta entering through Eq. 31 and ζ through Eq. 33). The text states 'Throughout this paper, ζ = 0.1 is adopted' immediately after Eq. (33), and uses β_p = 3, but no observational or numerical constraint on ζ in TDE disks is provided. Lowering ζ from 0.1 to 0.03 alone reduces E_p,diff from 0.45 PeV to about 12 TeV, and raising β_p from 3 to 27 reduces it to about 5.6 TeV; either change moves the predicted 0.35 PeV neutrino peak below 10 TeV and removes one of the three claimed promising sites. Please add a sensitivity study over ζ and β_p (and, for the luminosities, over η_cr = 0.1) or explicitly frame all absolute values as conditional on these parameters.","section":"§2.1–2.3, Eqs. (33), (31), (47)"},{"comment":"The headline neutrino energy of the super-Eddington MAD case is quoted with inconsistent normalizations: the abstract gives E_ν,pk ≈ 67 TeV (M_bh/10^7.7 M_sun)^(41/48), Section 3 gives E_ν,pk ≈ 80 TeV (M_bh/10^7 M_sun)^(41/48), and Section 5 Conclusion item 5 gives ≈ 67 TeV (M_bh/10^7 M_sun)^(41/48). If E_p,sync ≈ 0.35 PeV at 10^7.7 M_sun and E_ν,pk ≈ 0.19 E_p,sync, the value at 10^7 M_sun would be about 17 TeV, not 80 TeV. Please unify the prefactor and the mass normalization, and recompute the associated numerical values.","section":"Abstract, §3, §5 (item 5)"},{"comment":"The abstract lists the radiatively inefficient MAD RIAF as one of the 'three promising cases', but Conclusion 7 states that its neutrino luminosity is 'too weak to be detected with the current sensitivity of IceCube', and Section 4's detection-rate estimates only cover the super-Eddington MAD and the non-MAD RIAF. This is an internal inconsistency in the paper's central claim; please either define 'promising' as 'produces neutrinos regardless of detectability' and state this explicitly, or remove the radiatively inefficient MAD from the list of promising cases.","section":"Abstract; §4; §5, item 7"}],"minor_comments":[{"comment":"The magnetic field strength B and the plasma beta (called 'B' in Eq. 31) use overlapping notation; for example, Eq. (47) uses (B/3) for the plasma beta while B elsewhere denotes the field. Please use distinct symbols (e.g., script B for plasma beta) throughout.","section":"Eqs. (31), (47), (48)"},{"comment":"There are typographical artifacts: the text around Eq. (28) duplicates 'mfb', and the reference 'Stawarz, /suppress L.' contains a LaTeX command that should be removed.","section":"Eq. (28) and reference list"},{"comment":"The labels in panel (b) of Figure 2 appear garbled in the provided electronic version; please verify the figure rendering.","section":"Fig. 2"},{"comment":"The diffuse-flux estimate for the super-Eddington MAD assumes that 'about 1% of the observed TDE rate experiences the super-Eddington MAD state' without justification; adding a brief rationale or an explicit uncertainty would help.","section":"§4"}],"recommendation":"major_revision","confidential_remarks":"The 67/80 TeV discrepancy and the ζ/β sensitivity are the two issues I would ask the authors to fix before publication. I do not see a circularity problem: the model is constructed before the diffuse-flux comparison. The paper is within scope and the analytic framework is useful, but the quantitative predictions should be presented as conditional on the adopted fiducial parameters, with a sensitivity estimate."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"The paper gives a concrete analytic model for neutrino emission from three TDE disk phases: the super-Eddington MAD state, the non-MAD RIAF, and the radiatively inefficient MAD. What is actually new is the phase-dependent treatment: the super-Eddington MAD window, the resulting light-curve indices t^-65/24 and t^-10/3, and the claim that TDRs are a hidden neutrino population invisible in gamma-rays. The machinery is borrowed from Kimura et al. 2015, but the TDR-specific results are not in the prior literature. The paper is coherent and does not fit any observed data, so there is no circularity in the predictions.\n\nWhat the paper does well is work through the timescale competition in each phase and identify which sites are worth pursuing. The light-curve indices are parameter-robust and falsifiable, which is the strongest part of the contribution. The recognition that gamma-rays are absorbed while neutrinos escape is an important and plausible point.\n\nThe soft spots are real. The most visible problem is the normalization inconsistency in the headline neutrino energy: the abstract says 67 TeV with (Mbh/10^7.7 M_sun)^41/48, Section 3 says 80 TeV with (Mbh/10^7 M_sun)^41/48, and the conclusions say 67 TeV with (Mbh/10^7 M_sun)^41/48. These cannot all be right, and a referee needs to resolve this before the quantitative claims can be trusted. The deeper concern is the steep dependence on unvalidated parameters. In the non-MAD RIAF, gamma_diff scales as zeta^3 beta_plasma^-2, so lowering zeta from 0.1 to 0.03 or raising beta from 3 to 27 drops the predicted neutrino peak below 10 TeV. The paper states 'Throughout this paper, zeta = 0.1 is adopted' without any observational or numerical constraint, and the same is true for eta_cr = 0.1. That is the load-bearing assumption for the absolute energies, though not for the light-curve indices. There is also an apparent algebra issue in the derivation of gamma_diff (equation 46), which seems to have r/r_L rather than r_L/r, and equation (47) contains a radial term that vanishes at r=rp.\n\nWho is this for? High-energy astrophysicists working on TDEs and neutrino astronomy. The paper deserves a serious referee: it is a substantial model with testable predictions, and the problems are fixable. I would send it to peer review and ask for a corrected and parameter-sensitivity version.","headline":"A serious analytic model of TDE remnant neutrinos with distinctive light-curve predictions, but the headline energies are internally inconsistent and rest on unvalidated parameters.","tokens_in":25580,"tokens_out":6423,"would_cite":true,"duration_ms":62811,"reading_group":"yes","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"Tidal disruption remnants are predicted to be neutrino sources invisible in gamma rays.","keywords":["tidal disruption events","high-energy neutrinos","magnetically arrested disks","radiatively inefficient accretion flows","stochastic particle acceleration","supermassive black holes","neutrino astrophysics","pion decay"],"falsifier":"Take a well-observed TDE with a known black hole mass and search for neutrinos at the predicted peak energies: a super-Eddington MAD case should show neutrinos near 67 TeV decaying as $t^{-65/24}$, and an RIAF case should show 0.35 PeV neutrinos decaying as $t^{-10/3}$. A measured light curve following $t^{-5/3}$, or no neutrinos in a stacked sample of comparable events, would contradict the proposed acceleration balance.","tokens_in":24417,"feed_emoji":"🌠","tokens_out":9434,"duration_ms":88824,"temperature":0.7,"pith_summary":"This paper argues that the debris left behind when a star is torn apart by a supermassive black hole can act as a high-energy neutrino factory. It identifies three phases in which protons are plausibly accelerated to ultrarelativistic energies by magnetic turbulence: the super-Eddington phase of a magnetically arrested disk (MAD), and the radiatively inefficient accretion flow (RIAF) phase in both MAD and non-MAD states. In these sites, charged pions from proton-proton collisions decay into neutrinos with predicted peak energies from about 67 TeV to several PeV, and with distinctive time decays such as $t^{-65/24}$ and $t^{-10/3}$. Because the accompanying gamma rays are absorbed, these remnants would be hidden neutrino sources that could contribute to the diffuse neutrino flux without visible gamma-ray counterparts.","feed_headline":"Shredded stars can glow in neutrinos alone","feed_subtitle":"Three disk states accelerate protons to 0.35–25 PeV, with light curves that identify the black hole state.","key_machinery":"The argument turns on second-order Fermi acceleration of protons in magnetic turbulence, with acceleration time $t_{\\rm acc} = \\zeta^{-1}(r/c)(v_A/c)^{-2}(r_L/r)^{2-s}\\gamma^{2-s}$, adopting turbulence amplitude $\\zeta=0.1$ and spectral index $s=5/3$. The maximum proton energy is set by equating this acceleration time to the fastest competing timescale at each site: spatial diffusion in the non-MAD RIAF, Compton drag or synchrotron cooling in the super-Eddington MAD, and synchrotron cooling in the radiatively inefficient MAD. For MAD states, the magnetic field is enhanced by the magnetically arrested disk condition, $B_{\\rm MAD}^2 = 2\\sqrt{2\\pi}(\\alpha/\\epsilon)(H/r)\\rho_p v_{\\rm ff}^2$, roughly $\\sqrt{\\alpha/\\epsilon}$ times the equipartition field. The proton-proton cross section and proton injection spectra then convert these maximum energies into neutrino spectra and light curves.","core_discovery":"The paper's central claim is that three states of a tidal disruption remnant are promising neutrino emitters. In the super-Eddington MAD state, protons reach about $0.35\\,\\mathrm{PeV}\\,(M_{\\rm bh}/10^{7.7}M_\\odot)^{41/48}$ when synchrotron cooling limits acceleration, and neutrinos peak near $67\\,\\mathrm{TeV}\\,(M_{\\rm bh}/10^{7.7}M_\\odot)^{41/48}$; for $M_{\\rm bh}\\gtrsim10^{7.7}M_\\odot$ the neutrino light curve decays as $t^{-65/24}$, while at lower masses Compton drag limits protons to roughly TeV energies and the decay follows $t^{-5/3}$. In the non-MAD RIAF phase, the proton cutoff is about $0.45\\,\\mathrm{PeV}\\,(M_{\\rm bh}/10^7M_\\odot)^{5/3}$, the neutrino peak is near $0.35\\,\\mathrm{PeV}\\,(M_{\\rm bh}/10^7M_\\odot)^{5/3}$, and the light curve decays as $t^{-10/3}$, which would identify a RIAF as TDE-born. In the radiatively inefficient MAD state, protons can reach about $25\\,\\mathrm{PeV}$ and neutrinos about $4.8\\,\\mathrm{PeV}$, though with a luminosity too low for current detectors. In all three cases, the pion-decay gamma rays are trapped, so the sources would appear as neutrino-only beacons.","pith_inferences":["Beyond the paper: a stacked search for neutrinos from optically and UV-selected TDEs that lack gamma-ray counterparts would test the hidden-source prediction more powerfully than chasing single events, because the per-event rate is low.","Beyond the paper: the $t^{-10/3}$ RIAF signature could be checked retrospectively, since known TDEs from years ago should now be in their RIAF phase and archival neutrino data could be re-analyzed for a delayed component.","Beyond the paper: the same acceleration-and-cooling balance should apply to any transient that passes from super-Eddington to RIAF accretion, including stellar-mass black hole outbursts, producing analogous neutrino light curves on much shorter timescales."],"forward_implications":["A super-Eddington MAD TDE around a black hole above about $10^{7.7}M_\\odot$ should be detectable as a neutrino source peaking near 67 TeV, with an unusually steep $t^{-65/24}$ decay that stands out from the standard $t^{-5/3}$ fallback.","A TDE-origin RIAF should produce a neutrino light curve $\\propto t^{-10/3}$ peaking near 0.35 PeV, giving a direct way to tell a leftover TDE disk from a long-lived low-luminosity AGN disk.","Because pion-decay gamma rays are absorbed in all three sites, any neutrinos detected from these remnants would arrive without a GeV-TeV gamma-ray counterpart, marking them as hidden sources.","The predicted neutrino luminosities approach the Eddington luminosity in the super-Eddington MAD case, placing detectable events within roughly a gigaparsec for current neutrino telescopes."],"supporting_citations":[{"why":"Supplies the standard t^-5/3 mass fallback rate that sets the four evolutionary phases and the normalization of the accretion rate.","marker":"Evans & Kochanek 1989"},{"why":"Provides the stochastic Fermi-II acceleration and spatial diffusion timescales used to compute maximum proton energies.","marker":"Kimura et al. 2015"},{"why":"Defines the magnetically arrested disk state and the magnetic diffusion velocity that sets the MAD field strength.","marker":"Narayan, Igumenshchev & Abramowicz 2003"},{"why":"Provides the ADAF/RIAF density and velocity structure underlying the non-MAD RIAF calculations.","marker":"Narayan & Yi 1995"},{"why":"Gives the proton-proton cross section used for pion production and neutrino spectra.","marker":"Kelner et al. 2006"},{"why":"Supplies the proton distribution function for the diffusion-limited acceleration case.","marker":"Becker et al. 2006"},{"why":"Supplies the synchrotron-cooled proton distribution used for the MAD-state neutrino spectra.","marker":"Stawarz & Petrosian 2008"},{"why":"Provides the radiative efficiency and numerical support for the super-Eddington MAD state.","marker":"McKinney, Dai & Avara 2015"}],"fun_headline_variants":["Shredded stars shine in neutrinos alone","Neutrino-only beacons from tidal disruption remnants","Black hole meals emit neutrinos, hide gamma rays","Neutrino light curves unmask black hole state in TDEs","Three disk states make TDRs neutrino lighthouses"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"The predictions hinge on the adopted magnetic turbulence amplitude $\\zeta=0.1$ and the assumed magnetic field strengths; if turbulence is weaker or the fields are lower, protons cool or escape before reaching PeV energies and the predicted neutrino signals disappear.","fun_headline_variants_meta":{"raw":{"variants":["Shredded stars shine in neutrinos alone","Neutrino-only beacons from tidal disruption remnants","Black hole meals emit neutrinos, hide gamma rays","Neutrino light curves unmask black hole state in TDEs","Three disk states make TDRs neutrino lighthouses"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000424,"raw_usage":{"total_tokens":2359,"prompt_tokens":1314,"completion_tokens":1045,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":930,"completion_tokens_details":{"reasoning_tokens":965}},"tokens_in":930,"tokens_out":1045,"duration_ms":11059,"temperature":1.0,"reasoning_tokens":965,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-14T10:32:04.721310+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"Take a well-observed TDE with a known black hole mass and search for neutrinos at the predicted peak energies: a super-Eddington MAD case should show neutrinos near 67 TeV decaying as $t^{-65/24}$, and an RIAF case should show 0.35 PeV neutrinos decaying as $t^{-10/3}$. A measured light curve following $t^{-5/3}$, or no neutrinos in a stacked sample of comparable events, would contradict the proposed acceleration balance.","supporting_citations":[{"cited_title":"R., Aharonian, F","cited_arxiv_id":null,"evidence_quote":"Gives the proton-proton cross section used for pion production and neutrino spectra."},{"cited_title":"R., & Kochanek, C","cited_arxiv_id":null,"evidence_quote":"Supplies the standard t^-5/3 mass fallback rate that sets the four evolutionary phases and the normalization of the accretion rate."},{"cited_title":"S., Murase, K., & Toma, K.\\ 2015, , 806, 159","cited_arxiv_id":null,"evidence_quote":"Provides the stochastic Fermi-II acceleration and spatial diffusion timescales used to compute maximum proton energies."},{"cited_title":"V., Abramowicz M","cited_arxiv_id":null,"evidence_quote":"Defines the magnetically arrested disk state and the magnetic diffusion velocity that sets the MAD field strength."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Provides the ADAF/RIAF density and velocity structure underlying the non-MAD RIAF calculations."},{"cited_title":null,"cited_arxiv_id":null,"evidence_quote":"Supplies the synchrotron-cooled proton distribution used for the MAD-state neutrino spectra."},{"cited_title":"C., Dai L., Avara M","cited_arxiv_id":null,"evidence_quote":"Provides the radiative efficiency and numerical support for the super-Eddington MAD state."}],"review_version":1}