{"id":"77f52210-60ed-4fb5-8ffd-6aabd590f91d","arxiv_id":"2411.09394","paper_version":2,"verdict":"CONDITIONAL","confidence":"HIGH","novelty_score":6.0,"correctness_risk":"medium","formal_verification":"none","parameter_count":7,"one_line_summary":"A proposed diagnostic correlates MeV pre-supernova neutrinos with TeV neutrinos from ejecta-circumstellar material interactions to test the origin of enhanced circumstellar gas around stripped-envelope supernovae.","lead":"Astrophysicists propose using two kinds of neutrino signals from the same supernova, low-energy pre-explosion neutrinos and high-energy neutrinos from later shock collisions, to test whether pre-explosion neutrino heating ejected the dense gas around the star. If the method works, it would give next-generation neutrino detectors a new way to study how massive stars lose mass before exploding.","discovery_kind":"new_method","skeptic_critique":{"model":"deepseek-v4-flash","headline":"The linear instantaneous mass-loss mapping in Eq. (1) is the load-bearing link between pre-SN and CSM neutrino light curves; if the stellar surface response is delayed, nonlinear, or saturated, the synchronized detection test would not diagnose the CSM origin.","rationale":"The paper proposes a genuinely interesting multi-energy neutrino diagnostic: if enhanced CSM is produced by pre-SN neutrino emission, then the MeV pre-SN neutrino light curve should be imprinted on the TeV CSM-neutrino light curve, and synchronized observations at JUNO and IceCube could test that. The central claim requires a physical bridge from Lpre-ν to the surface mass-loss rate that sets the CSM density. The only bridge provided is Eq. (1), Mdot_star(t) ≈ Mdot_wind + β·Lpre-ν(t)/c^2, with β varied as a constant. Everything downstream—ρ_csm, the t_csm mapping, t_onset, and LCSM-ν—follows from this assumed instantaneous linear proportionality. The reader's weakest_assumption identifies this same link, and I agree that it is the load-bearing assumption. Moriya (2014) motivates the mechanism, but does not calibrate the response function; stellar readjustment to a sudden loss of gravitational mass could be delayed, nonlinear, or limited by envelope binding energy. If so, the correlation Lpre-ν ∝ LCSM-ν would not hold even in the neutrino-driven-CSM scenario, and the proposed test would give a false negative (or, if other mass-loss mechanisms dominate, a false positive). The paper's Sec. 4 caveat that SN profile uncertainties only change the scale understates the issue, because shock trajectory determines the temporal mapping, not just the event-rate normalization. The paper does provide transparent equations, multiple β values, and explicit detector and background estimates, which is good support for a feasibility study. But because the central diagnostic rests on an unvalidated microphysical relation, a CONDITIONAL verdict remains appropriate. The proposed MESA-based test would directly check whether Eq. (1) is a valid mapping, and would settle whether the concern actually lands.","tokens_in":15257,"tokens_out":5414,"duration_ms":61839,"concrete_test":"Run a 1D stellar-structure/hydro simulation (e.g., MESA) of a stripped 5 Msun WR-like progenitor with a time-dependent central mass-loss term dM_c/dt = Lpre-ν(t)/c^2 imposed during the final ~10^6 s before collapse, using the Kato et al. (2017) light curve. Record the surface mass-loss rate Mdot_star(t) and check: (a) is Mdot_star(t) proportional to Lpre-ν(t) to within a factor of ~2 over the last week before core collapse? (b) is the response delay less than the JUNO time binning (≲1 day)? Repeat with Lpre-ν scaled by 0.1 and 10 to test linearity and saturation. If either check fails, Eq. (1) is not a valid mapping, and the synchronized detection diagnostic cannot be claimed as model-independent.","verdict_should_be":"UNCHANGED","load_bearing_attack":"The central chain is: Lpre-ν(t) -> Mcdot_c = Lpre-ν/c^2 (Eq. 1) -> Mdot_star(t) = Mdot_wind + β·Mdot_c(t) -> CSM density via the retarded-time relation (Eqs. 2–3) -> LCSM-ν(t) roughly proportional to ρ_csm·v_sh^2. The proposed synchronized test therefore tests not just \"CSM was formed by pre-SN neutrinos\" but the much stronger assumption that surface mass loss responds instantaneously, linearly, and with a single constant efficiency β to the core neutrino luminosity. The paper treats β as a free systematic parameter, but it never derives it from a stellar-structure calculation, and it cites Moriya (2014) as the origin of the mechanism. If the neutrino energy-loss signal propagates to the surface on a hydrostatic/adjustment timescale comparable to the last days or weeks, Eq. (1) smears the light curve and the reconstructed CSM-neutrino light curve no longer reflects the pre-SN neutrino light curve. If the mass-loss response saturates (e.g., because the envelope cannot be unbound faster than its dynamical or thermal timescale), the late-time high-luminosity portion of Lpre-ν would not be imprinted in ρ_csm. If other mass-loss processes (waves, pulsations, binary interaction) dominate, a false enhancement could appear without pre-SN neutrino support. The Sec. 4 statement that explosion-energy and ejecta-mass uncertainties \"only change the scale\" is not sufficient because they also shift the shock trajectory and thereby the temporal mapping between t_csm and the observed TeV-neutrino arrival time. Without a physical validation of Eq. (1), the claimed \"flexibly applicable to any pre-SN model\" is not established.","agreement_with_reader":"agree"},"referee_report":{"model":"deepseek-v4-flash","summary":"The paper proposes a multi-energy neutrino diagnostic for the origin of enhanced circumstellar material (CSM) around stripped-envelope supernovae. The authors take a pre-SN neutrino light curve from Kato et al. (2017), convert the core neutrino luminosity into a stellar surface mass-loss rate through Eq. (1) with a free efficiency β, build a time-dependent CSM density profile using the retarded-time prescription of Piro & Lu (2020), and compute non-thermal TeV neutrino emission from the SN shock interacting with this CSM using standard pp-interaction and thin-shell shock models. They then estimate event rates at JUNO (pre-SN MeV ν̄e) and IceCube (TeV–PeV CSM ν) for distances of 300 pc and 1 kpc and for β = 1, 0.1, 0.01, and identify synchronized time windows in which a correlation between the two light curves could be tested. The main quantitative conclusions are that the synchronized test is feasible out to roughly 500 pc with current detectors, with future improvements extending the reach to about 1 kpc or a few kpc, and that the high-energy signal is far above the IceCube background in the adopted setup.","tokens_in":15639,"tokens_out":8235,"duration_ms":73373,"significance":"If the proposed correlation is observed, it would be a first demonstration of multi-energy neutrino astronomy and would support the scenario of neutrino-driven pre-SN mass loss. The forward model is built from standard, clearly referenced ingredients (thin-shell dynamics, Kelner et al. pp spectra, Kafexhiu et al. cross sections, IceCube effective areas), and the paper is explicit that the accessible distance is tied to the adopted pre-SN model and that the number of nearby Wolf-Rayet targets is small. The test is falsifiable: it predicts synchronized time structure in the JUNO and IceCube event rates for a given β and distance. However, the predicted correlation directly follows from the assumed linear response in Eq. (1), so a positive observation would validate that specific response model rather than independently confirming the CSM origin; the paper does not quantify the response timescale or saturation behavior.","major_comments":[{"comment":"The relation Ṁ⋆(t) = Ṁwind + β Lpre-ν(t)/c² is the load-bearing assumption that produces the predicted Lpre-ν ∝ LCSM-ν correlation. The paper treats β as a free systematic parameter, but it never derives or bounds β from a stellar-structure calculation; Moriya (2014) describes a response operating near the Eddington limit, where the envelope response could be delayed by an adjustment timescale, nonlinear in Lpre-ν, or saturated at high luminosity. If any of these effects is relevant on the ~10⁵–10⁶ s timescales of the pre-SN light curve, the synchronized time-structure test would fail even when the CSM is genuinely neutrino-driven. Please estimate or bound the surface response timescale and discuss the linearity/saturation regime, or explicitly restrict the applicability claim to the linear-response model.","section":"Sec. 2.2, Eq. (1)"},{"comment":"The statement that uncertainties in explosion energy and ejecta mass 'only change the scale of the observed number of signals' is not supported by the model. ESN and MSN enter Eq. (A2) and therefore the ejecta density ρej in the thin-shell equations (4)–(5); changing them alters Rsh(t), vsh(t), the onset time tonset in Eq. (6), and the retarded-time mapping in Eqs. (2)–(3). The temporal correlation that the method relies on can therefore shift or broaden, not merely rescale. A quantitative check, e.g., varying ESN and MSN by a factor of two, is needed before claiming that the time structure is robust.","section":"Sec. 4, second paragraph"},{"comment":"The event-rate curves and the applicability region in Fig. 5 are shown without statistical or systematic error bands. The applicability conclusion depends on the significance of the pre-SN signal relative to the 18 day⁻¹ background and on model uncertainties in β, ϵp, ϵB, s, Aeff, and the atmospheric/astrophysical neutrino normalization. The text asserts that the experimental uncertainty is dominated by data statistics, but no propagation is shown. Please include at least Poisson uncertainties on the histograms and a representative systematic band, or give the conditions under which the quoted 500 pc reach would change.","section":"Sec. 3, Figs. 3 and 5"},{"comment":"The wording that the observation would 'capture the correlation in time structure that would not appear in other CSM origins' overstates the scope of the test. Because Eq. (1) builds the correlation into the forward model, a positive observation tests the specific linear-response neutrino-driving scenario; it does not by itself discriminate neutrino-driven CSM from other mass-loss mechanisms unless the response law is known. The conclusions should be phrased as testing the Moriya-type linear-response model, and the discussion should state what can and cannot be concluded about the CSM origin from a null or positive result.","section":"Sec. 1 and Sec. 4"}],"minor_comments":[{"comment":"The pre-SN neutrino light curve is taken from a 15 M⊙ progenitor, while the CSM calculation adopts M⋆ = 5 M⊙ and R⋆ = 3×10¹¹ cm; the text cites approximate universality of pre-SN luminosities, but the mismatch should be stated and justified explicitly.","section":"Sec. 2.1"},{"comment":"The axis label 'Number luminosity [erg s⁻¹ MeV⁻¹]' mixes number and energy units; it should be either a number rate per energy [s⁻¹ MeV⁻¹] or an energy luminosity per energy interval [erg s⁻¹ MeV⁻¹].","section":"Figure 2"},{"comment":"The quantity MCSM is used but never defined; please define it (presumably the shocked CSM mass) and state its relation to Msh in Eqs. (4)–(5).","section":"Eq. (10)"},{"comment":"The abstract says the method is 'reasonably applicable for the range up to ∼1 kpc', while Sec. 4 says the current setup is 'well available up to ∼500 pc' with effort needed beyond; please harmonize these statements.","section":"Abstract vs. Sec. 4"},{"comment":"'multi energy neutrino astronomytowards' is missing a space between 'astronomy' and 'towards'.","section":"Sec. 4"},{"comment":"The vertical axis is labeled 'log10 (Ejection efficiency)', while the text calls β the 'mass-loss efficiency'; please use one term consistently.","section":"Figure 5"}],"recommendation":"major_revision","confidential_remarks":"The manuscript is within the scope of ApJ and the multi-energy neutrino idea is timely and well-motivated. My main concern is the unquantified response law in Eq. (1), which is the central physical assumption behind the proposed synchronized test; if the authors can bound its timescale or clearly restrict the claim, the paper would be acceptable. I do not see concerns about citation practice or novelty disclosure."},"author_rebuttal":null,"desk_editor":{"model":"deepseek-v4-flash","letter":"Short version: the paper proposes a new way to test whether the enhanced CSM around stripped-envelope SNe comes from pre-SN neutrino-driven mass loss, by comparing the MeV pre-SN neutrino light curve with the TeV neutrino light curve from ejecta-CSM interactions. The synchronized two-energy diagnostic is new, as far as I know, and the forward model uses standard building blocks (Moriya's mass-loss scaling, Piro-Lu CSM profiles, Murase's pp neutrino emission, Kelner spectra). The mass-loss-efficiency scan and the (d, β) applicability map are genuinely useful, and the authors are honest about the small number of known WR stars within ~1 kpc.\n\nStrengths: the model is transparent, β is treated as a free systematic, and the event-rate estimates at JUNO and IceCube look plausible. The background treatment is approximate (zenith-averaged, no self-veto), but given the signal rates shown, that's a minor issue.\n\nWhere it's soft: Eq. (1) is the load-bearing assumption — that the surface mass-loss rate responds instantaneously and linearly to the core neutrino luminosity, with a single constant β. The authors scan β but never discuss a delayed, nonlinear, or saturating response. If the stellar surface doesn't track Lpre-ν that simply, the predicted Lpre-ν ∝ LCSM-ν correlation could break down even for a genuinely neutrino-driven CSM. That limits the diagnostic's interpretability, and the claim of flexible applicability to 'any pre-SN model' is overbroad. This is a limitation, not a fatal flaw, but it deserves an explicit caveat.\n\nThere's also an internal inconsistency: Sec. 3.3 gives the current reach as ~500 pc, while Sec. 4 opens with 'about 1 kpc,' and the abstract follows the latter without qualification. The explosion energy and ejecta mass are never stated numerically, and the statement that they 'only change the scale' is too strong — they also shift the shock trajectory and hence the time mapping. These are fixable.\n\nBottom line: a genuinely new method, built honestly, with addressable soft spots. Worth refereeing, and I'd ask the authors to clarify Eq. (1)'s domain of validity and reconcile the reach numbers.","headline":"A new synchronized MeV+TeV neutrino diagnostic for CSM origin; solid feasibility study, but the linear mass-loss mapping in Eq. (1) needs a clearer caveat.","tokens_in":16199,"tokens_out":4658,"would_cite":true,"duration_ms":40058,"reading_group":"maybe","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":null,"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"deepseek-v4-flash","headline":"This paper argues that if dense circumstellar material around stripped-envelope supernovae is created by pre-supernova neutrino emission, then the pre-supernova MeV neutrino light curve and the TeV neutrino light curve from the shocked…","keywords":["Circumstellar matter","Core-collapse supernovae","Massive stars","High energy astrophysics","Neutrino astronomy","Supernova neutrinos","Multi-energy neutrino astronomy","Pre-supernova neutrinos"],"falsifier":"A single nearby stripped-envelope supernova (within about 1 kpc) with an inferred dense CSM and a strong TeV neutrino signal at IceCube, but with no pre-SN neutrino excess at JUNO in the weeks before collapse, would falsify the proposed correlation. Conversely, a pre-SN neutrino light curve that matches the CSM-neutrino light curve poorly—quantified by a Kolmogorov–Smirnov test on the synchronized window—in an object with clearly enhanced CSM would also rule out the neutrino-driven origin for that event.","tokens_in":15044,"feed_emoji":"🔭","tokens_out":7874,"duration_ms":65060,"temperature":0.7,"pith_summary":"This paper proposes a way to settle a long-standing question in stellar evolution: why some stripped-envelope supernovae are surrounded by dense circumstellar material (CSM), far more than steady winds can explain. The hypothesis under test is that the intense neutrino emission from the star's core in the weeks before collapse removes enough mass to weaken gravity and drives an enhanced surface outflow that builds the CSM. The paper's key move is to chain two known relations: pre-supernova neutrinos drive the mass loss that creates the CSM, and the shock slamming into that CSM produces high-energy neutrinos, so the MeV and TeV neutrino light curves from the same object should mirror each other in time. The authors show the synchronized detection is feasible with JUNO and IceCube for supernovae out to roughly 500 pc (and about 1 kpc with planned upgrades), and that the comparison is model-independent in the sense that it tests time structure rather than absolute rates. If the correlation is absent in a nearby event, other CSM origins would be implicated.","feed_headline":"Twin neutrino bursts could reveal a supernova's secret mass loss","feed_subtitle":"If pre-explosion neutrinos drive the outflow, JUNO and IceCube should see synchronized bursts in two energy bands.","key_machinery":"The load-bearing relation is Eq.~(1): $\\dot{M}_\\star(t) \\approx \\dot{M}_{\\rm wind} + \\beta L_{\\rm pre-\\nu}(t)/c^2$, which converts the core neutrino luminosity into an enhanced surface mass-loss rate through a constant efficiency $\\beta$. This single linear map connects the MeV and TeV neutrino signals; all subsequent steps (CSM density from the time-dependent mass-loss profile, thin-shell shock dynamics, pp-neutrino production) are standard machinery that preserves the temporal correlation. The paper also introduces the synchronized-time-window test: only the time interval in which pre-SN neutrinos are detectable is used for the high-energy comparison.","core_discovery":"The central discovery is a model-independent diagnostic: the time structure of the pre-supernova thermal neutrino light curve is imprinted, through the mass-loss history, into the CSM density profile and hence into the light curve of non-thermal TeV neutrinos produced by the stellar shock as it sweeps up that CSM. Concretely, the paper constructs the chain $L_{\\rm pre-\\nu}(t) \\to \\dot{M}_\\star(t)$ (Eq.~1 with efficiency $\\beta$) $\\to \\rho_{\\rm csm}(r,t)$ (time-dependent mass-loss reconstruction assuming expansion at the escape velocity) $\\to$ shock evolution (thin-shell model) $\\to$ high-energy neutrino emission (pp interactions). The resulting high-energy neutrino light curve reproduces the shape of the pre-SN neutrino light curve, so a synchronized comparison at JUNO and IceCube—say, a Kolmogorov–Smirnov test on the event time distributions—can accept or reject the neutrino-driven mass-loss origin for any particular supernova.","pith_inferences":["If the pre-SN neutrino flux is detected by JUNO and the TeV flux by IceCube for a single nearby supernova, the method yields a direct measurement of $\\beta$, the currently unknown coupling between core mass loss and surface mass loss, rather than just a correlation check.","Since the time correlation is robust to overall normalization uncertainties such as explosion energy and ejecta mass, the method may also serve as a distance-independent consistency test for neutrino-driven mass-loss models.","The same two-band correlation could be applied to other transients with pre-explosion neutrino-driven activity, such as some electron-capture supernovae or massive stars with late-stage neutrino losses, provided the CSM shock produces TeV neutrinos.","A null result—dense CSM with no synchronized neutrino pair—would not entirely rule out neutrino-driven mass loss if the response is significantly time-delayed, so an upper limit on $\\beta$ would need to be interpreted with that caveat."],"forward_implications":["If the correlation holds for a nearby event, it identifies the neutrino-driven mass-loss channel as the physical cause of the enhanced CSM for that supernova.","The method is independent of the specific pre-SN neutrino model because it only compares time structures, so it can be applied to any progenitor or neutrino emission model.","The applicable volume extends to about 500 pc with current detectors and to roughly 1 kpc (and farther with future ones), covering the closest known Wolf-Rayet stars, including $\\gamma^2$ Velorum at about 340 pc.","Even when synchronized detection is not possible, the reconstructed high-energy neutrino light curve alone constrains the mass-loss efficiency $\\beta$ of the progenitor.","The same strategy can be carried over to other pairings of detectors (SK-Gd, Hyper-Kamiokande, KM3NeT), widening the reach in distance and in mass-loss efficiency."],"supporting_citations":[{"why":"Supplies the hypothesis that neutrino emission before collapse reduces gravity and drives enhanced mass loss, which is the physical basis of Eq. (1).","marker":"Moriya 2014"},{"why":"Provides the pre-supernova neutrino light curve model used for the demonstration of the method.","marker":"Kato et al. 2017"},{"why":"Gives the time-dependent CSM density reconstruction from the mass-loss history, used to build the shock environment.","marker":"Piro & Lu 2020"},{"why":"Supplies the thin-shell model for the evolution of the shock through the CSM.","marker":"Koo & McKee 1992"},{"why":"Provides the model for high-energy neutrino production from ejecta-CSM interaction via pp collisions.","marker":"Murase 2018, 2024"},{"why":"Provides the JUNO background rates and inverse beta decay detection efficiency used for the pre-SN neutrino event rates.","marker":"An et al. 2016"},{"why":"Supplies the IceCube effective area used for computing the CSM neutrino event rates.","marker":"Abbasi et al. 2021"},{"why":"Provides the atmospheric neutrino background flux used in the high-energy event rate estimate.","marker":"Honda et al. 2015"}],"fun_headline_variants":["Neutrino echoes reveal supernova's hidden mass loss","Two energy bands, one supernova secret: neutrino sync","JUNO and IceCube team up to spot supernova mass loss","MeV and TeV neutrinos sync to diagnose supernova CSM"],"cache_read_input_tokens":3200,"weakest_assumption_plain":"The predicted correlation stands or falls with the assumption that the star's surface mass-loss rate responds to the core's neutrino luminosity instantly and with a constant, linear efficiency $\\beta$ (Eq. 1); if the response is delayed, nonlinear, saturates, or is swamped by other mass-loss processes, the correlation can disappear even when the CSM is genuinely neutrino-triggered.","fun_headline_variants_meta":{"raw":{"variants":["Neutrino echoes reveal supernova's hidden mass loss","Two energy bands, one supernova secret: neutrino sync","JUNO and IceCube team up to spot supernova mass loss","MeV and TeV neutrinos sync to diagnose supernova CSM"]},"model":"deepseek-v4-flash","effort":"low","cost_usd":0.000212,"raw_usage":{"total_tokens":1456,"prompt_tokens":1019,"completion_tokens":437,"prompt_tokens_details":{"cached_tokens":384},"prompt_cache_hit_tokens":384,"prompt_cache_miss_tokens":635,"completion_tokens_details":{"reasoning_tokens":364}},"tokens_in":635,"tokens_out":437,"duration_ms":4723,"temperature":1.0,"reasoning_tokens":364,"cache_read_input_tokens":384,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-08-12T20:41:00.580517+00:00","model_set":{"reader":"deepseek-v4-flash"},"falsifier":"A single nearby stripped-envelope supernova (within about 1 kpc) with an inferred dense CSM and a strong TeV neutrino signal at IceCube, but with no pre-SN neutrino excess at JUNO in the weeks before collapse, would falsify the proposed correlation. Conversely, a pre-SN neutrino light curve that matches the CSM-neutrino light curve poorly—quantified by a Kolmogorov–Smirnov test on the synchronized window—in an object with clearly enhanced CSM would also rule out the neutrino-driven origin for that event.","supporting_citations":[{"cited_title":"S., Kajita , T., Kasahara , K., & Midorikawa , S","cited_arxiv_id":null,"evidence_quote":"Provides the atmospheric neutrino background flux used in the high-energy event rate estimate."}],"review_version":1}