{"id":"465a23c6-6765-4f8f-9cbb-b39c87d47825","arxiv_id":"2605.21062","paper_version":1,"verdict":"UNVERDICTED","confidence":"LOW","novelty_score":6.0,"correctness_risk":"unknown","formal_verification":"none","parameter_count":2,"one_line_summary":"Population synthesis from binary evolution models predicts periodic neutron star-companion interactions in more than half of surviving hydrogen-poor core-collapse supernovae, with periods peaking at 20-50 days and lasting 0.5-10 years.","lead":"This paper analyzes a grid of detailed binary stellar evolution models with population synthesis to predict how often the companion star interacts with the newly formed neutron star after a core-collapse supernova, producing periodic light-curve modulations. A smart generalist might read it to anticipate observable periodic signals in future or archival supernova data and to understand binary effects on supernova diversity.","discovery_kind":"new_application","skeptic_critique":{"model":"grok-4.3","headline":"Analytic prescriptions for companion expansion after SN ejecta impact determine the >50% CCI rate for H-poor systems","rationale":"The reader's weakest assumption correctly isolates the modeling step whose accuracy most directly controls the quantitative claim. Full-text access confirms the rate is derived from these prescriptions rather than from first-principles hydro or observational calibration, so the concern is load-bearing. No other internal inconsistency (e.g., kick distributions or explodability) appears more decisive once the expansion step is fixed.","tokens_in":1851,"tokens_out":402,"duration_ms":14746,"concrete_test":"Select the five binary models closest to the best-fit parameters for SN2022jli; recompute the post-impact companion radius and orbital evolution using the analytic formulae in the paper versus a short 3D hydro run (e.g., with FLASH or AREPO) initialized at the same pre-SN separation and ejecta profile; if the analytic inflation factor or interaction duration differs by >25% from the hydro result, re-run the population synthesis with the hydro-calibrated correction and report the revised H-poor CCI fraction.","verdict_should_be":"CONDITIONAL","load_bearing_attack":"The headline rate (>50% periodic CCI in non-disrupted H-poor CCSN binaries) is obtained by post-processing a binary evolution grid with analytic prescriptions that model the companion's radius and luminosity response to ejecta impact, followed by subsequent orbital evolution with the newborn NS. These prescriptions control both whether the inflated companion reaches the NS orbit and the duration of the interaction (0.5-10 yr). Because the paper does not report direct validation of the prescriptions against hydrodynamical simulations for the specific mass ratios and separations in the grid, an error in the assumed expansion factor or cooling timescale would directly rescale the fraction of systems classified as exhibiting periodic CCI. The distinction between H-poor and H-rich rates is also sensitive to the same step, since H-rich companions are typically wider.","agreement_with_reader":"agree"},"referee_report":{"model":"grok-4.3","summary":"The manuscript analyzes a comprehensive grid of detailed binary stellar evolution models with the newly developed SN-ORACLE population synthesis code. It implements analytic prescriptions for companion-star expansion after SN ejecta impact and derives occurrence rates, period distributions, and observables for periodic neutron-star–companion interactions (CCI) in core-collapse supernovae, using varied explodability and kick prescriptions. The central claim is that periodic CCI occurs in more than half of non-disrupted hydrogen-poor CCSN binaries (with periods peaking at 20–50 days and durations 0.5–10 yr) while remaining rare for hydrogen-rich events; specific models are identified that reproduce the light-curve periods of SN 2022jli, SN 2015ap, and SN 2022esa.","tokens_in":2059,"tokens_out":656,"duration_ms":47385,"significance":"If the analytic expansion prescriptions hold, the work supplies concrete, falsifiable predictions for periodic modulations in SN light curves and for the long-term brightness of companions, directly relevant to ongoing and archival searches. Credit is due for the use of state-of-the-art detailed binary grids, the introduction of the SN-ORACLE code, and the explicit matching of individual evolutionary sequences to three observed events. The quantitative rates, however, rest on unvalidated analytic steps whose accuracy controls the headline >50 % fraction.","major_comments":[{"comment":"The section describing the analytic prescriptions for companion expansion and cooling (post-ejecta impact): the >50 % periodic-CCI rate for non-disrupted H-poor systems is obtained by post-processing the binary grid with these prescriptions. No quantitative comparison to hydrodynamical simulations is reported for the mass ratios and orbital separations realized in the grid; an error in the assumed expansion factor or cooling timescale would directly rescale the reported fraction and the H-poor versus H-rich distinction.","section":"Methods / analytic prescriptions"},{"comment":"Results section on occurrence rates and period distributions: no error propagation or sensitivity study is presented for the derived fractions with respect to plausible variations in the explodability prescription, neutron-star kick distribution, or the free parameters of the analytic expansion model. This omission leaves the robustness of the central >50 % claim and the 0.5–10 yr duration range difficult to assess.","section":"Results / occurrence rates"}],"minor_comments":[{"comment":"Abstract: the statement that 'up to 27 % of H-poor SNe could show periodicity' is not immediately reconciled with the >50 % rate among non-disrupted binaries; a short parenthetical on the disrupted fraction would remove ambiguity.","section":"Abstract"},{"comment":"Figure showing period distributions: inclusion of the corresponding distribution for H-rich systems would allow immediate visual comparison and strengthen the claimed contrast.","section":"Figures"}],"recommendation":"major_revision","confidential_remarks":"The manuscript is a good fit for an astro-ph.SR journal. The reliance on external binary grids and a new synthesis code without hydro validation is a point that may warrant an additional referee with expertise in binary hydrodynamics."},"author_rebuttal":{"model":"grok-4.3","summary":"We thank the referee for the constructive and detailed review of our manuscript. We address each major comment below and describe the revisions we will implement to improve the robustness and clarity of our results.","responses":[{"response":"We acknowledge that the manuscript does not include a direct quantitative comparison of the analytic prescriptions to hydrodynamical simulations specifically for the mass ratios and orbital separations present in our binary grid. The prescriptions are based on analytic models calibrated against existing hydrodynamical studies in the literature. To address this point, we will add a dedicated paragraph in the methods section discussing the validity range of the prescriptions, citing the relevant hydrodynamical benchmarks, and include a sensitivity analysis varying the expansion factor and cooling timescale within plausible uncertainties. This will quantify the effect on the reported occurrence rates.","revision_made":"yes","referee_comment":"[Methods / analytic prescriptions] The section describing the analytic prescriptions for companion expansion and cooling (post-ejecta impact): the >50 % periodic-CCI rate for non-disrupted H-poor systems is obtained by post-processing the binary grid with these prescriptions. No quantitative comparison to hydrodynamical simulations is reported for the mass ratios and orbital separations realized in the grid; an error in the assumed expansion factor or cooling timescale would directly rescale the reported fraction and the H-poor versus H-rich distinction."},{"response":"The manuscript already explores results across multiple explodability prescriptions and neutron-star kick distributions, with the >50% fraction for non-disrupted H-poor systems remaining consistent. We agree, however, that a more systematic sensitivity study including variations in the free parameters of the analytic expansion model and basic error propagation would better demonstrate robustness. In the revised version we will add a new subsection or appendix presenting these sensitivity tests, including how the central fraction and duration range respond to changes in the analytic parameters.","revision_made":"partial","referee_comment":"[Results / occurrence rates] Results section on occurrence rates and period distributions: no error propagation or sensitivity study is presented for the derived fractions with respect to plausible variations in the explodability prescription, neutron-star kick distribution, or the free parameters of the analytic expansion model. This omission leaves the robustness of the central >50 % claim and the 0.5–10 yr duration range difficult to assess."}],"tokens_in":1651,"tokens_out":494,"duration_ms":35627,"standing_objections":[]},"desk_editor":{"model":"grok-4.3","letter":"The main takeaway is that periodic neutron star-companion interactions should appear in more than half of the non-disrupted systems that produce hydrogen-poor core-collapse supernovae, with much lower rates for hydrogen-rich cases. Periods peak around 20-50 days and last 0.5-10 years, and the inflated companions reach detectable magnitudes for up to a decade in some models. They also tie specific binary tracks to the observed periods in SN2022jli, SN2015ap, and SN2022esa, and estimate that up to 27% of H-poor events could show this signal.","headline":"The paper predicts periodic CCI in over half of surviving H-poor binary CCSNe using detailed evolution grids plus analytic post-explosion prescriptions, but those prescriptions control the headline rates without reported hydro checks.","tokens_in":2569,"tokens_out":205,"would_cite":false,"duration_ms":21465,"reading_group":"maybe","serious_thinker":"yes","would_accept_peer_review":true},"rs_alignment":{"model":"grok-4.3","evidence":[{"relation":"unclear","rs_module":"IndisputableMonolith/Cost/FunctionalEquation.lean","rs_theorem":"washburn_uniqueness_aczel","paper_passage":"We implement analytic prescriptions for the expansion of the companion star following its interaction with the SN ejecta... E_heat = p · E_kin,ej · Ω̃_eff with p=0.08... log R_max... τ_infl = α E_heat / L_max with α∼0.18"},{"relation":"unclear","rs_module":"IndisputableMonolith/Foundation/DimensionForcing.lean","rs_theorem":"reality_from_one_distinction","paper_passage":"post-supernova orbital periods P_post-SN = 9.8–226 d, peaking at 20–70 d... N_inter ≥2 for periodic CCI"}],"headline":"Standard binary population synthesis with analytic ECI/CCI prescriptions; no J-cost, φ-ladder or 8-tick structure","alignment":"orthogonal","rationale":"Paper derives SN rates and CCI fractions from MESA grids + fitted analytic expansions (E_heat, R_max, τ_infl with free efficiencies p=0.08, α≈0.18) and kick/explodability parameters. Central machinery is conventional stellar evolution + population synthesis; no ratio-symmetric cost J(x), golden-ratio identities, cosh-cost forcing, or 8-tick periodicity appears. Domain (applied binary astrophysics) lies outside RS foundational forcing chain.","tokens_in":62510,"confidence":"high","tokens_out":357,"duration_ms":13094,"cache_read_input_tokens":38528,"cache_creation_input_tokens":0},"lean_confirmation":null,"pith_extraction":{"msc":[],"pacs":[],"model":"grok-4.3","headline":"Periodic companion-neutron star interactions occur in more than half of surviving binary systems that produce hydrogen-poor core-collapse supernovae.","keywords":["core collapse supernovae","binary stellar evolution","neutron star companions","population synthesis","periodic light curves","hydrogen-poor supernovae","SN2022jli","companion inflation"],"falsifier":"A large observational sample of hydrogen-poor core-collapse supernovae showing a rate of periodic light-curve modulations with 20-50 day periods well below 50 percent among surviving binaries would falsify the predicted occurrence fraction.","tokens_in":2771,"feed_emoji":"","tokens_out":800,"duration_ms":33952,"temperature":0.7,"pith_summary":"When the first star in a massive binary explodes, its ejecta strike the companion, which can expand and then orbitally interact with the new neutron star, producing periodic emission. The authors run population synthesis on a large grid of detailed binary evolution calculations to forecast how often this companion-compact object interaction happens and what its observable signatures are. They conclude the periodic version is common in hydrogen-poor supernova progenitors that remain bound but rare in hydrogen-rich ones. This framework reproduces the periods seen in events like SN2022jli and predicts that the inflated companions remain bright enough for years to be detected by current telescopes. If the rates hold, many more such periodic features should appear in both new and archival supernova data.","feed_headline":"Over half of surviving hydrogen-poor SN binaries show periodic CCI","feed_subtitle":"Population synthesis on detailed binary models predicts 20-50 day periods lasting months to years, plus brighter companions detectable for a","key_machinery":"Population synthesis of a grid of detailed binary evolution models, combined with analytic prescriptions for the expansion of the companion star after supernova ejecta interaction and its subsequent orbital dynamics with the compact object.","core_discovery":"Analyzing a comprehensive grid of detailed binary stellar evolution models with the SN-ORACLE population synthesis code and analytic prescriptions for companion expansion after supernova ejecta impact, the authors find that periodic CCI occurs in more than half of the binary systems that produce a hydrogen-poor core collapse SN and are not disrupted, while the occurrence rate in systems producing hydrogen-rich SNe is small. The resulting period distribution is broad and peaks around 20-50 days, with interactions lasting 0.5-10 years. Specific models in the grid reproduce the observed periods of SN2022jli, SN2015ap, and SN2022esa, and the inflated companions reach J-band magnitudes of 21-23,,","pith_inferences":["A systematic search for periodic modulations in existing and future hydrogen-poor supernova light curves could directly measure the surviving binary fraction.","The models identify specific binary configurations that match known events, offering targets for multi-wavelength follow-up years after explosion.","Different choices for neutron-star birth kicks would change the exact bound fraction but are unlikely to erase the large difference between hydrogen-poor and hydrogen-rich channels."],"forward_implications":["The interactions produce broad period ranges peaking at 20-50 days and lasting 0.5-10 years.","Up to 27 percent of hydrogen-poor supernovae could display periodicity in their light curves.","The expanded companions increase in luminosity and reach J-band magnitudes of 21-23 for up to 10 years after events like SN2022jli.","The effect is far more common for hydrogen-poor than for hydrogen-rich core-collapse supernovae."],"fun_headline_variants":["Binary models show periodic CCI in over half of surviving H-poor SNe","More than half surviving hydrogen-poor binaries exhibit periodic CCI","Binary synthesis shows periodic CCI for over half of H-poor SN survivors","Population synthesis finds periodic interactions in majority of H-poor SN binaries"],"cache_read_input_tokens":2112,"weakest_assumption_plain":"The analytic prescriptions implemented for the expansion of the companion star following its interaction with the SN ejecta accurately capture the physical response and subsequent orbital interaction with the compact object.","fun_headline_variants_meta":{"raw":{"variants":["Binary models show periodic CCI in over half of surviving H-poor SNe","More than half surviving hydrogen-poor binaries exhibit periodic CCI","Binary synthesis shows periodic CCI for over half of H-poor SN survivors","Population synthesis finds periodic interactions in majority of H-poor SN binaries"]},"model":"grok-4.3","cost_usd":0.011753,"raw_usage":{"total_tokens":5167,"prompt_tokens":878,"num_sources_used":0,"completion_tokens":63,"cost_in_usd_ticks":117528000,"prompt_tokens_details":{"text_tokens":878,"audio_tokens":0,"image_tokens":0,"cached_tokens":64},"completion_tokens_details":{"audio_tokens":0,"reasoning_tokens":4226,"accepted_prediction_tokens":0,"rejected_prediction_tokens":0}},"tokens_in":878,"tokens_out":63,"duration_ms":64286,"temperature":1.0,"reasoning_tokens":4226,"cache_read_input_tokens":64,"cache_creation_input_tokens":0},"cache_creation_input_tokens":0},"created_at":"2026-05-21T02:09:12.099470+00:00","model_set":{"reader":"grok-4.3"},"falsifier":"A large observational sample of hydrogen-poor core-collapse supernovae showing a rate of periodic light-curve modulations with 20-50 day periods well below 50 percent among surviving binaries would falsify the predicted occurrence fraction.","supporting_citations":[],"review_version":1}