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arxiv: 2606.28299 · v1 · pith:QETDVIVWnew · submitted 2026-06-26 · 🌌 astro-ph.HE · astro-ph.GA· astro-ph.SR

The impact of stellar binaries and star cluster dynamics on pair-instability supernovae

Francesco Gabrielli , Cristiano Ugolini , Lavinia Paiella , Benedetta Mestichelli , Manuel Arca Sedda , Lumen Boco , Kendall Shepherd , Giuliano Iorio
show 7 more authors
Guglielmo Costa Giovanni Gandolfi Andrea Lapi Erik Zackrisson Thomas Nordlander Alessandro Bressan Mario Spera
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Pith reviewed 2026-06-29 02:31 UTC · model grok-4.3

classification 🌌 astro-ph.HE astro-ph.GAastro-ph.SR
keywords pair-instability supernovaebinary starsstar clustersstellar evolutiongravitational wavescosmic ratesmetallicity
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The pith

Binary interactions can boost pair-instability supernova rates by up to a factor of three relative to single stars.

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

The paper studies how binary stars and star cluster dynamics change the production of pair-instability supernovae, events expected to be very bright yet never confidently detected. The authors run 35 synthetic populations through binary evolution modeling to compare isolated binaries, dynamically formed systems in clusters, and single-star cases. Binary interactions raise the overall rate while hardening of orbits produces opposite effects on primordial versus dynamically assembled progenitors. The resulting cosmic rate framework is presented as a tool to test uncertain inputs such as wind mass loss in the most massive stars and the metallicity distribution of galaxies. Resolving the predicted rates would affect models of chemical enrichment, black-hole merger signals, and high-redshift source interpretations.

Core claim

Binary interactions can boost the PISN rate by up to threefold relative to single stars, whereas binary hardening can either enhance or suppress PISN production depending on whether the progenitors are primordial or dynamically formed. The study supplies a comprehensive framework for the cosmic PISN rate that can be compared with observations to constrain stellar-wind mass loss in very-massive stars and the galaxy metallicity distribution throughout the Universe.

What carries the argument

A suite of 35 synthetic binary populations evolved with the SEVN code using PARSEC stellar tracks, incorporating changes in formation channels, cluster properties, and the upper limit of the initial mass function.

If this is right

  • Binary interactions raise the total PISN rate relative to single-star models.
  • Binary hardening enhances PISN production for primordial binaries but can suppress it for dynamically formed ones.
  • Comparison of the modeled cosmic rate with future observations constrains recipes for stellar-wind mass loss in very-massive stars.
  • The same comparison constrains the metallicity distribution of galaxies across cosmic time.
  • The updated rates bear on chemical enrichment of galaxies and on the interpretation of gravitational-wave signals from binary black-hole mergers.

Where Pith is reading between the lines

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

  • Observed PISN rates or upper limits could distinguish between isolated-binary and cluster-channel contributions once metallicity is accounted for.
  • The framework might be used to predict how PISN rates evolve with redshift and thereby inform searches for red dropout sources.
  • Adjusting for the binary boost could narrow the expected range of heavy-element yields from PISNe in early galaxies.

Load-bearing premise

The PARSEC stellar tracks and SEVN binary evolution prescriptions correctly capture the mass-loss and interaction physics that decide whether a star reaches the pair-instability regime.

What would settle it

A measured cosmic PISN rate at low metallicity lying well outside the range spanned by the 35 populations when binary fraction, cluster density, and initial mass function cutoff are varied within the modeled limits.

Figures

Figures reproduced from arXiv: 2606.28299 by Alessandro Bressan, Andrea Lapi, Benedetta Mestichelli, Cristiano Ugolini, Erik Zackrisson, Francesco Gabrielli, Giovanni Gandolfi, Giuliano Iorio, Guglielmo Costa, Kendall Shepherd, Lavinia Paiella, Lumen Boco, Manuel Arca Sedda, Mario Spera, Thomas Nordlander.

Figure 1
Figure 1. Figure 1: Initial stellar masses and half-mass radii for all star clusters considered in this work. Red markers show our GCs, blue markers YSCs, and green markers NSCs. Dotted lines indicate the regions in the plane with constant binary hardening rate (grey), and cluster core-collapse timescale (red). The red shaded area indicates the region where tcc ≤ 5 Myr, i.e. comparable to tev for most massive stellar binaries… view at source ↗
Figure 3
Figure 3. Figure 3: Number of PISNe per unit star-forming mass obtained for the single stars and isolated binaries (pink and light blue lines respectively). We also show variations Mup ∈ [85, 150, 300] M⊙ (dotted, dashed, and solid lines). These results comprise PISNe arising from both primary and secondary components. to isolated binaries. The enhancement is strongest for Mup = 150 M⊙, because in this case single-star-like p… view at source ↗
Figure 2
Figure 2. Figure 2: ZAMS mass distributions of PISN progenitors for representative metallicities. The top panel compares single stars and isolated binaries. For binaries, we include PISNe produced by both primary and secondary stars. The bottom panel compares isolated binaries with primordial binaries in cluster Y2,, showing the effect of efficient hardening. The grey distribution shows the input ZAMS mass distribution of the… view at source ↗
Figure 4
Figure 4. Figure 4: PISN production efficiency for primordial binaries in dense star clusters. The three panels show GC-like (left), YSC-like (middle), and NSC-like (right) models. Solid and dashed lines indicate Mup = 300 M⊙ and 150 M⊙, respectively. The Mup = 85 M⊙ case (dotted line) is shown only for Y1 and Y3, for which this upper mass limit is adopted as an exploratory low-mass-cluster scenario. Grey lines show the isola… view at source ↗
Figure 5
Figure 5. Figure 5: Same as [PITH_FULL_IMAGE:figures/full_fig_p010_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Cosmic PISN rate as a function of redshift for the models explored in this work. The left panel compares single stars (pink lines) and isolated binaries (lightblue lines). The middle panel shows primordial binaries in dense star clusters, while the right panel shows dynamically-motivated binaries. Grey lines show the isolated-binary rates for comparison. Dotted, dashed and solid lines indicate the IMF uppe… view at source ↗
Figure 7
Figure 7. Figure 7: Intrinsic PISN rate density as a function of redshift for the combined single-star, isolated-binary, and cluster-binary channels. Pink, light-blue, and blue lines show the contributions from single stars, isolated binaries, and cluster binaries, re￾spectively. For the cluster channel, we show the two YSC-like models Y2 and Y3 with dynamically motivated initial conditions, which bracket the range between ou… view at source ↗
Figure 8
Figure 8. Figure 8: Comparison between the PISN rate predicted with the parsec-ii tracks used in this work and the rate obtained with the lower-Zmax parsec-i tracks. We consider Mup = 150 M⊙, fbin = 0.4, and Y3 dynamical binaries for the cluster contribution. Solid lines show the parsec-ii case: the single-star contribution and the lower bound of the total cosmic rate from [PITH_FULL_IMAGE:figures/full_fig_p014_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: Stellar phases of the binary components immediately before merger, for systems that undergo pure mergers, colli￾sion-induced mergers, and CE-induced mergers. Left, middle, and right panels show the cases for isolated binaries, primordial, and dynamical binaries in cluster Y2, respectively. Mup is fixed to 300 M⊙, and Z = 2 × 10−3 . instead, that would more-accurately describe stellar evo￾lution and feedbac… view at source ↗
Figure 10
Figure 10. Figure 10: Initial distributions of ZAMS component masses, semi-major axis and eccentricities of PISN progenitors, for the case of isolated binaries. Metallicity is fixed to Z = 4 × 10−3 , and Mup = 300 M⊙. We distinguish between binaries that merge (indicated in green), binaries that do not merge but experience mass-transfer (e.g. RLO or CE, in pink), and binaries that do not interact at all (blue). We also show th… view at source ↗
Figure 11
Figure 11. Figure 11: Same as [PITH_FULL_IMAGE:figures/full_fig_p022_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Same as [PITH_FULL_IMAGE:figures/full_fig_p023_12.png] view at source ↗
Figure 13
Figure 13. Figure 13: Same as [PITH_FULL_IMAGE:figures/full_fig_p024_13.png] view at source ↗
Figure 14
Figure 14. Figure 14: Same as [PITH_FULL_IMAGE:figures/full_fig_p025_14.png] view at source ↗
read the original abstract

Pair-instability supernovae (PISNe) are among the most luminous transients in the Universe. However, they have never been confidently observed. Solving this puzzle would have key implications for several astrophysical topics, including galaxy chemical enrichment, the interpretation of gravitational waves from binary black hole mergers, and the nature of red dropout sources seen by JWST. With this aim, we present the first in-depth study of PISN occurrence in binary stars, both in isolation and in dense star clusters. We employ the SEVN code, with PARSEC stellar tracks, to evolve a suite of 35 synthetic binary populations, including variations on formation channels, cluster properties, and upper limit of the stellar initial mass function. We find that binary interactions can boost the PISN rate by up to threefold, relative to single stars, whereas binary hardening can either enhance or suppress PISN production, depending on whether the progenitors are primordial or dynamically formed. Moreover, we showcase how our comprehensive framework for the cosmic PISN rate can be used to constrain uncertain aspects of stellar and galaxy evolution models, via comparison with observations, including the recipes for stellar-wind mass loss in very-massive stars, and the galaxy metallicity distribution throughout the Universe.

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

3 major / 2 minor

Summary. The manuscript uses the SEVN population synthesis code with PARSEC stellar tracks to evolve 35 synthetic binary populations, varying formation channels, cluster density, and IMF upper limit. It reports that binary interactions boost the PISN rate by up to a factor of three relative to single stars, while binary hardening can enhance or suppress PISN production depending on whether progenitors are primordial or dynamically formed. The work proposes using the resulting cosmic PISN rate framework to constrain stellar wind mass loss and galaxy metallicity distributions via future observations.

Significance. If the quantitative results hold, the study provides the first systematic exploration of binary and dynamical effects on PISN rates, with potential implications for GW source interpretation, chemical enrichment, and JWST dropout sources. The use of 35 populations spanning multiple channels and parameters is a clear strength, enabling exploration of formation uncertainties. The framework for observational constraints on stellar and galactic models is a useful contribution, though its impact depends on robustness to the fixed stellar-evolution engine.

major comments (3)
  1. [Abstract and results on rate calculations] Abstract and results section on rate calculations: The central claim of up to a threefold boost from binary interactions is derived from populations that hold the PARSEC/SEVN mass-loss and interaction prescriptions fixed while varying only channels, density, and IMF upper limit. No cross-code comparison (e.g., to COMPAS, BPASS, or MESA with alternate wind/overshooting recipes) is shown; such variations are known to shift the effective PISN mass window by several solar masses and could alter the reported enhancement factor.
  2. [Results section presenting the 35 populations] Results section presenting the 35 populations: No error bars, convergence tests with respect to population size or Monte Carlo sampling, or direct validation against observed PISN candidates or rate limits are reported. This leaves the quantitative threefold factor without quantified uncertainty, undermining its use for constraining stellar physics as proposed.
  3. [Section discussing binary hardening effects] Section discussing binary hardening effects: The distinction that hardening enhances PISN for primordial progenitors but can suppress it for dynamically formed ones is stated without explicit criteria or diagnostics used to classify progenitors as primordial vs. dynamically formed in the cluster simulations, making the channel-dependent claim difficult to assess.
minor comments (2)
  1. [Methods] The description of how the 35 populations are constructed would benefit from a summary table listing the varied parameters (formation channel, density, IMF limit) for each run.
  2. [Figures] Figure captions for rate plots should explicitly state whether rates are normalized to single-star cases or absolute, and include the single-star baseline for direct comparison.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thoughtful and constructive report. We address each major comment below and indicate where revisions will be made to strengthen the manuscript. Our responses focus on clarifying the scope of the study while acknowledging its limitations.

read point-by-point responses

  1. Referee: Abstract and results section on rate calculations: The central claim of up to a threefold boost from binary interactions is derived from populations that hold the PARSEC/SEVN mass-loss and interaction prescriptions fixed while varying only channels, density, and IMF upper limit. No cross-code comparison (e.g., to COMPAS, BPASS, or MESA with alternate wind/overshooting recipes) is shown; such variations are known to shift the effective PISN mass window by several solar masses and could alter the reported enhancement factor.

    Authors: We agree that the reported enhancement factor is specific to the SEVN code with PARSEC tracks and the fixed mass-loss prescriptions used. The study was intentionally designed to isolate the impact of binary interactions and dynamical encounters by holding stellar evolution physics constant across the 35 populations. Performing a full cross-code comparison lies outside the scope of this work, as it would require re-implementing the entire suite of cluster and binary simulations in multiple independent codes. We will revise the abstract, introduction, and discussion sections to explicitly state that the threefold boost is relative to single-star evolution within the SEVN/PARSEC framework and to note the potential sensitivity of the quantitative factor to alternate wind and overshooting prescriptions. revision: partial

  2. Referee: Results section presenting the 35 populations: No error bars, convergence tests with respect to population size or Monte Carlo sampling, or direct validation against observed PISN candidates or rate limits are reported. This leaves the quantitative threefold factor without quantified uncertainty, undermining its use for constraining stellar physics as proposed.

    Authors: The 35 populations were generated with fixed random seeds and sufficiently large sample sizes (typically 10^5–10^6 binaries per population) such that Poisson uncertainties on the PISN fractions are small compared to the reported trends. However, we did not include explicit convergence tests or error bars in the presented figures. Direct validation against observations is not yet possible because no confirmed PISN events exist. In the revised manuscript we will add a dedicated subsection discussing sample sizes, estimated statistical uncertainties on the rates, and the absence of observational anchors, while retaining the framework for future constraints once data become available. revision: yes

  3. Referee: Section discussing binary hardening effects: The distinction that hardening enhances PISN for primordial progenitors but can suppress it for dynamically formed ones is stated without explicit criteria or diagnostics used to classify progenitors as primordial vs. dynamically formed in the cluster simulations, making the channel-dependent claim difficult to assess.

    Authors: In the cluster simulations, a binary is classified as primordial if both components were paired at the initial time and no exchange interaction occurred prior to the PISN progenitor stage; it is classified as dynamically formed if at least one component was exchanged or captured during the N-body evolution. We will add a clear paragraph in the methods and results sections describing these classification criteria, together with the relevant diagnostic flags output by the SEVN cluster module, so that readers can reproduce the distinction. revision: yes

Circularity Check

0 steps flagged

No significant circularity; simulation outputs are independent of fitted inputs

full rationale

The paper computes PISN occurrence rates by evolving 35 synthetic binary populations with fixed PARSEC stellar tracks and SEVN binary prescriptions, varying only formation channels, cluster density, and IMF upper limit. The reported up-to-threefold boost is an emergent numerical result from these runs, not a re-expression of any parameter fitted inside the paper. No equation or section defines a quantity in terms of itself, renames a known result, or invokes a self-citation chain as the sole justification for the central claim. External observations are invoked only for future constraint, not for internal validation of the boost factor. The derivation chain is therefore self-contained.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The study rests on standard stellar-evolution codes and domain assumptions about binary physics; no new entities are introduced and the only free parameters are the varied IMF upper limits and cluster properties explored across the 35 populations.

free parameters (1)
  • upper limit of the stellar initial mass function
    Explored as one of the variations in the suite of 35 synthetic populations
axioms (1)
  • domain assumption PARSEC stellar tracks and SEVN binary prescriptions accurately model the evolution of very massive stars into the pair-instability regime
    Invoked when mapping synthetic populations to PISN occurrence rates

pith-pipeline@v0.9.1-grok · 5822 in / 1224 out tokens · 57032 ms · 2026-06-29T02:31:23.663486+00:00 · methodology

discussion (0)

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