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arxiv: 2605.21062 · v1 · pith:ZFYM2VUOnew · submitted 2026-05-20 · 🌌 astro-ph.SR · astro-ph.HE

Neutron star-companion interaction in core collapse supernovae. Population synthesis based on detailed binary evolution models

Andrea Ercolino , Norbert Langer , Avishay Gal-Yam , Abel Schootemeijer , Caroline Mannes , Harim Jin , Ruggero Valli , Selma de Mink
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Luc Dessart
This is my paper

Pith reviewed 2026-05-21 02:09 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.HE
keywords core collapse supernovaebinary stellar evolutionneutron star companionspopulation synthesisperiodic light curveshydrogen-poor supernovaeSN2022jlicompanion inflation
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The pith

Periodic companion-neutron star interactions occur in more than half of surviving binary systems that produce hydrogen-poor core-collapse supernovae.

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

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.

Core claim

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,,

What carries the argument

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.

If this is right

  • 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.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • 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.

Load-bearing premise

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.

What would settle it

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.

Figures

Figures reproduced from arXiv: 2605.21062 by Abel Schootemeijer, Andrea Ercolino, Avishay Gal-Yam, Caroline Mannes, Harim Jin, Luc Dessart, Norbert Langer, Ruggero Valli, Selma de Mink.

Figure 1
Figure 1. Figure 1: Schematic evolution of SN2022jli-like transients in binaries, from the explosion (top), through ejecta-companion interaction (ECI) and compact-object-companion interaction (CCI), to the deflation of the companion (bottom). Characteristic timescales are shown on the left, with t = 0 marking core collapse. quently, SN2022jli provides a unique laboratory for probing and constraining theoretical models of bina… view at source ↗
Figure 2
Figure 2. Figure 2: Fraction of the companions of Type Ibc and Type Ibn super￾nova progenitors at the time of explosion in the reference population model (Sect. 3.1). We distinguish those with no companion (single stars, merger products, or disrupted binaries; white), a degenerate companion (gray), or a non-degenerate companion (blue outline). Non-degenerate companions are further divided into those that remain bound (teal) a… view at source ↗
Figure 3
Figure 3. Figure 3: Population-wide distributions of post-explosion orbital period Ppost−SN, eccentricity epost−SN, and the number of times the NS pene￾trates the envelope of the companion Ninter, for H-poor supernovae un￾dergoing periodic CCI in the reference model. All histograms and 2D plots are normalized to the total number of supernovae exhibiting peri￾odic CCI, except the histogram of Ninter (brown). The histogram of N… view at source ↗
Figure 4
Figure 4. Figure 4: Distribution of the maximum luminosity Lmax (top) of ECI￾inflated non-degenerate companions to all H-poor supernovae in the reference population model. The bottom panel shows the companion’s maximum luminosity relative to the its pre-ECI luminosity. Values are normalized to the total number of H-poor supernovae. Orange and teal filling show systems with unbound and bound companions after explo￾sion, respec… view at source ↗
Figure 5
Figure 5. Figure 5: As [PITH_FULL_IMAGE:figures/full_fig_p006_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Fraction of H-poor supernovae with periodic companion–compact-object interaction (CCI) for different popu￾lation models, versus the fraction of binaries in which the primary star explodes and forms a NS that is bound to the companion, fNS,bound, normalized to all systems where the primary undergoes core collapse. Colors indicate the kick prescription (k1–k3), markers the merger criterion (m1–m5), and shade… view at source ↗
Figure 7
Figure 7. Figure 7: Post-supernova orbital period (left) and eccentricity (right) distributions for binary models where periodic CCI is expected. Each line shows the results from a different population model, with those discussed in Sect. 3 shown with thicker lines (see legend) while those with other parameter combinations (see [PITH_FULL_IMAGE:figures/full_fig_p007_7.png] view at source ↗
Figure 8
Figure 8. Figure 8: As [PITH_FULL_IMAGE:figures/full_fig_p008_8.png] view at source ↗
read the original abstract

Most massive stars live in binary systems. When the first supernova (SN) in a binary occurs, the ejecta hit the companion, which may inflate as a consequence, and then interacts with the newly formed compact object. The recent Type Ic SN2022jli shows a periodic modulation in its emission, which is interpreted as evidence for such interaction. We derive predictions for the occurrence rate and observables of SNe exhibiting these companion - compact-object interactions (CCIs). We analyze a comprehensive, state-of-the-art grid of detailed binary stellar evolution models, and implement analytic prescriptions for the expansion of the companion star following its interaction with the SN ejecta. We employ the newly developed population synthesis code SN-ORACLE to derive the distribution functions of the properties of the SNe affected by CCI and their companions, where we use different explodability and neutron star birth kick distributions. We find that periodic CCI is expected to occur 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. We find broad period ranges, peaking around 20-50 days, with the interaction lasting for 0.5-10 years. We identify specific binary evolution models that reproduce the observed period of the light curve undulations of SN2022jli, SN2015ap, and SN2022esa. The inflation of the companion also increases its luminosity and brightness, increasing its detectability with current instruments. For SN2022jli, our best fitting models predict a J-band magnitude of 21-23 for up to 10 years. We find that up to 27% of H-poor SNe could show periodicity in their light curves, while only a few such events have been identified so far. Our results may help find periodic CCI features in future and archival SN observations.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

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.

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 (2)
  1. [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.
  2. [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.
minor comments (2)
  1. [Abstract] 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.
  2. [Figures] Figure showing period distributions: inclusion of the corresponding distribution for H-rich systems would allow immediate visual comparison and strengthen the claimed contrast.

Simulated Author's Rebuttal

2 responses · 0 unresolved

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.

read point-by-point responses

  1. Referee: [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.

    Authors: 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: yes

  2. Referee: [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.

    Authors: 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: partial

Circularity Check

0 steps flagged

No significant circularity in derivation chain

full rationale

The paper derives CCI occurrence rates (>50% for non-disrupted H-poor CCSN binaries) by post-processing an external grid of detailed binary evolution models with analytic prescriptions for companion expansion after ejecta impact, then feeding results into the new SN-ORACLE population synthesis code along with separate explodability and kick distributions. No step reduces by construction to its own inputs: the rates are forward predictions from the binary grid properties (separations, mass ratios) rather than any fitted parameter, self-definitional loop, or load-bearing self-citation. The H-poor vs. H-rich distinction follows directly from the grid's orbital statistics, which are independent of the CCI classification step. The derivation remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim depends on the accuracy of detailed binary evolution calculations, the validity of analytic post-interaction expansion rules, and the chosen distributions for explodability and neutron-star kicks; these are treated as inputs rather than derived quantities.

free parameters (2)
  • explodability and neutron star birth kick distributions
    Different distributions are employed to generate the final statistics; their specific functional forms and parameters are not derived within the work.
  • analytic prescriptions for companion expansion
    Implemented to model the response to SN ejecta; the functional form and any scaling constants are introduced rather than derived from first principles.
axioms (2)
  • domain assumption Most massive stars live in binary systems.
    Opening statement of the abstract; used to motivate the entire binary-evolution framework.
  • domain assumption The detailed binary stellar evolution models in the grid correctly capture mass transfer, common-envelope phases, and core evolution up to the supernova.
    The population synthesis is built directly on this pre-existing grid.

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