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REVIEW 4 major objections 8 minor 80 references

Peculiar long GRBs arise from NS–WD mergers that fire repeated magnetar giant flares, making both the burst and the r-process kilonova.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

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2026-07-31 12:18 UTC pith:O5YSWNIE

load-bearing objection Coherent single-engine NS–WD picture that fixes the r-process hole with GF crustal ejecta, but the fitted Mej sits an order of magnitude above what the spike census can deliver and the beaming patch does not cleanly close it. the 4 major comments →

arxiv 2607.24531 v1 pith:O5YSWNIE submitted 2026-07-27 astro-ph.HE

R-process nucleosynthesis from magnetar giant flares in neutron star--white dwarf mergers: A unified picture for peculiar long gamma-ray bursts

Shu-Qing Zhong , Long Li , Le Zou , Ji-Gui Cheng , Yan-Zhi Meng , Jia-Hong Gu This is my paper
classification astro-ph.HE
keywords gamma-ray burstsmagnetarsneutron star–white dwarf mergersr-process nucleosynthesiskilonovaegiant flaresaccretion disksX-ray plateaus
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

Peculiar long gamma-ray bursts such as GRBs 211211A and 230307A show a hard main burst, a soft extended emission separated by a trough, an X-ray plateau, and a kilonova with r-process signatures. The paper argues that these events are tidally disrupted mergers of a pre-merger magnetar with a massive white dwarf. Hyperaccretion from the constant-entropy disk amplifies the neutron star’s toroidal field until repeated giant flares erupt; their initial spikes form the main burst, while the later propeller phase produces the extended emission. Each flare’s electron–positron–photon fireball shocks the crust, ejecting neutron-rich material that undergoes α-rich freeze-out and builds enough r-process ejecta to power the observed kilonova once boosted by magnetar spin-down, which also lights the X-ray plateau. The picture therefore unifies prompt emission, afterglow, kilonova, and heavy-element production inside a single NS–WD engine.

Core claim

A tidally disrupted neutron-star–white-dwarf merger with a pre-merger magnetar (surface field ≳10^14 G) and a massive white dwarf produces the entire observed phenomenology of peculiar long GRBs: the main burst is a forest of accretion-amplified giant-flare initial spikes, the extended emission and the trough arise from the accretion-to-propeller transition, crustal ejecta from the associated fireballs synthesize r-process nuclei via α-rich freeze-out, and post-merger spin-down powers both the X-ray plateau and an extra boost to the kilonova.

What carries the argument

Accretion-amplified magnetar giant flares: hyperaccretion drives the toroidal field to ~10^15–5×10^16 G, triggering repeated starquakes whose e±–γ fireballs both radiate the main-burst spikes and unbind successive parcels of crust (each ~10^{-8}–10^{-6} M⊙) that freeze out into r-process nuclei.

Load-bearing premise

The cold, non-accreting crust calculation still holds under sustained hyperaccretion and thousands of successive flares, so each spike continues to unbind enough neutron-rich crust for α-rich freeze-out.

What would settle it

A high-resolution spectroscopic campaign on a future peculiar long GRB that either fails to detect the expected second- and third-peak r-process lines once the afterglow has faded, or finds an ejecta mass and velocity structure incompatible with thousands of discrete crustal parcels.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • The main-burst minimum variability timescale directly counts the number of giant-flare spikes and therefore lower-limits the cumulative crustal ejecta mass.
  • The MB–EE trough is a clean observational signature of the accretion-to-propeller transition and can be used to diagnose the accretion-rate history.
  • Post-merger magnetar parameters inferred from the X-ray plateau and from the kilonova boost need not be identical if the spin-down luminosity is angularly structured.
  • Jet beaming implies the true r-process yield can exceed the line-of-sight estimate by an order of magnitude or more.
  • The same engine can explain both events that show spectroscopic r-process features and those that so far show only photometric kilonova candidates.

Where Pith is reading between the lines

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

  • If repeated flares deplete or heat the crust faster than β-equilibrium can be restored, the r-process yield per spike should decline with time, imprinting a measurable spectral evolution across the main burst.
  • The model predicts that MeV gamma-ray lines from freshly synthesized r-process nuclei could appear during or shortly after the main burst, offering a prompt nucleosynthesis diagnostic.
  • Similar accretion-amplified giant-flare forests may operate in other high-accretion magnetar systems, potentially linking peculiar GRBs to a broader class of magnetar-driven transients.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

4 major / 8 minor

Summary. The paper proposes a unified model for peculiar long GRBs (211211A, 230307A) based on tidally disrupted NS–WD mergers with a pre-merger magnetar. Hyperaccretion amplifies the toroidal field to B_phi ~ 1e15–5e16 G, triggering repeated magnetar giant flares whose initial spikes form the main burst as a "forest" of ~800–2000 spikes (N = T90/tau_min). The accretion-to-propeller transition produces the EE and the MB–EE trough; post-merger magnetar spin-down powers the X-ray plateau and boosts the kilonova. The key new ingredient is r-process production: each flare's e±–γ fireball shocks the crust and unbinds mej ~ 1e-8–1e-6 Msun (per Cehula et al. 2024), synthesized via α-rich freeze-out; the ensemble yields Mej ~ 1e-5–1e-3 Msun, argued to suffice for the kilonova when boosted by spin-down and beaming corrections. Joint afterglow+kilonova MCMC fits reproduce both events' light curves, but return Mej ~ 1.2e-2 Msun for both bursts, which the authors attribute to unobserved misaligned flares.

Significance. If the scenario holds, it would provide the first unified explanation of peculiar LGRBs — prompt three-episode structure, plateau, and kilonova — while identifying a concrete, observationally accessible r-process site (giant-flare crustal ejecta), which would be of broad interest. The manuscript has real strengths: joint MCMC fits to the full multi-wavelength datasets of both bursts, explicit per-spike energetics tied to an inferred toroidal field, a specific MB–EE trough interpretation as the accretion-to-propeller transition, falsifiable elements (spike-width statistics tied to Galactic GFs; predicted flare multiplicity), and an unusually candid caveat section. These give the model testable content beyond a phenomenological fit. However, the headline nucleosynthesis claim currently rests on unquantified extrapolations and a beaming argument that is internally inconsistent with the paper's own spike census, so the significance is conditional on resolving the major comments below.

major comments (4)
  1. [§3.3, point 4; §2 (penultimate paragraph); Table 2] The central r-process claim fails its own accounting. The mechanism supplies mej~1e-8–1e-6 Msun per flare x 800–2000 spikes = Mej~1e-5–1e-3 Msun (§2, Panel c), but Table 2 fits log Mej = -1.91 (~1.2e-2 Msun) for both bursts. The bridge offered — 'at least ten times more misaligned GF events' and the f_b~1e-5–1e-3 beaming factor — misapplies f_b, which is the relativistic beaming of the gamma-ray spikes; the ejecta parcels are non-relativistic (v~0.1–0.4c) and launched quasi-isotropically from the crust, so the unseen-flare correction is bounded by the covering fraction of the closed-field-line region (a factor of a few, not 1/f_b~1e3–1e5). Moreover, >=10x more flares means N>~1e4 over 13–18 s, i.e. ~1 ms cadence, below the tau_min~9–16 ms that §3.1 identifies with a single spike; the forest would overlap into a smooth continuum, contradicting the paper's own spike census. The summary sta
  2. [§3.1] The per-spike field estimate (E_spike ~ B_phi^2 DeltaR^3/8pi, giving B_phi ~ few x 1e16 G) ignores the integrated budget. The true total gamma-ray energy of the flare forest is ~5.3e51 erg (211211A) and of order 1e52 erg (230307A) — independent of f_b, since N_true x (f_b E_iso,spike) = E_iso,MB. A single toroidal reservoir at B~5e16 G contains only ~7e50 erg within the NS volume, so the field must be dissipated and re-amplified ~10–40 times within ~10–20 s, requiring a mean re-amplification power ~1e51–1e52 erg/s. This should be compared explicitly with the accretion-driven dynamo of Zhong et al. (2023); without it, the per-spike B estimate and the 'thousands of flares' picture are not shown to be energetically self-consistent.
  3. [§2, Panel (c); §4 caveats] The entire per-flare yield (mej~1e-8–1e-6 Msun, Ye>~0.4, alpha-rich freeze-out) rests on the Cehula et al. (2024) cold, non-accreting, beta-equilibrated crust. Here the NS hyperaccretes at >~1e-2 Msun/s during the flaring epoch and fires ~1e3 flares in ~10 s; the paper itself concedes (§4) that polar shock heating and repeated ejection outpacing beta-equilibrium recovery are unmodeled. Because the ejecta mass and composition scale directly with these assumptions, this is load-bearing for the r-process claim rather than a peripheral caveat. The authors should quantify the sensitivity (e.g., how mej and the yield pattern degrade for a heated or depleted crust), or explicitly make the abstract's 'collectively yields Mej >~ 1e-5–1e-3 Msun' conditional on this assumption.
  4. [§3.3, point 2] The plateau analysis (Zhong et al. 2023, 2024) and the kilonova boost yield different (P0, B_s,post) for the same post-merger magnetar, reconciled here by a newly posited angular structure of the spin-down radiation — a collimated component powering the plateau and a quasi-isotropic component boosting the kilonova. This is introduced to absorb a tension, not derived, and no fraction f_iso of the spin-down power is specified or checked against the total rotational energy for the fitted P0 and B_s,post. Since the plateau and the magnetar-boosted kilonova are both pillars of the 'unified' claim, the authors should quantify f_iso, demonstrate energetic consistency with both components, and state a testable consequence (e.g., off-axis plateau behavior).
minor comments (8)
  1. [§2, penultimate paragraph] The expression f_b ≃ 0.5 x (1/2) theta_j^2 contains an unexplained extra factor 0.5 relative to the standard monopolar beaming factor f_b = (1 - cos theta_j) ≈ theta_j^2/2. With the fitted theta_j = 0.028–0.072 rad (Table 2), the standard expression gives 4e-4–2.6e-3, not the quoted 1e-5–1e-3; please clarify the definition and its role in the ejecta-mass argument.
  2. [§3.1] The spike counts N = T90/tau_min (~800 and ~2000) assume a 100% duty cycle of back-to-back spikes; since tau_min is strictly a lower bound on the spike width, these N values are upper limits and the resulting Mej range is likewise an upper envelope, which should be stated. Please also specify how tau_min was measured for these bursts.
  3. [§3.3, first paragraph] Roming et al. (2005) is cited for the Swift XRT light curves of GRB 211211A; the XRT repository reference is Evans et al. (2009) (already in the list), while Roming et al. is the UVOT instrument paper.
  4. [Fig. 2 and Table 2] With ~14 free parameters, the paper shows only best-fit curves and a parameter table. Please add MCMC corner plots (or at least prior ranges) and a residuals panel, and comment on why both bursts return identical best-fit log Mej = -1.91 — coincidence, or a prior/boundary effect.
  5. [Table 2] The fitted opacity for GRB 211211A, kappa = 0.88 cm^2/g, lies below the 3–20 cm^2/g range quoted in §3.2 and implies lanthanide-poor ejecta. This sits awkwardly with the r-process interpretation advocated here (versus the earlier 56Ni interpretation of Zhong et al. 2023) and deserves explicit discussion, as is done for GRB 230307A in point 3.
  6. [§4, final caveat] '...will be addressed in forthcoming work by Cehula et al. (2024)' — presumably a forthcoming paper by those authors is meant; the reference and tense should be fixed.
  7. [Eq. (7)] The photospheric radius is set to vt with no thermalization-depth or electron-scattering correction; this is standard but should be stated as an assumption, since it affects the late-time color evolution shown in Fig. 2.
  8. [§1] Check the author-name convention for 'Qiumu et al. (2026)' — the surname appears to be listed first.

Circularity Check

4 steps flagged

Load-bearing engine is the authors' own Zhong+2023 NS–WD accretion/propeller model re-applied to the same two GRBs; the new GF–r-process channel is externally grounded, but the Mej 'prediction' only matches the joint fit after a free misaligned-flare multiplicity is dialed up.

specific steps
  1. self citation load bearing [§1 (Intro) and §2 Panel (b); also §3 opening enumeration]
    "Nevertheless, the tidally disrupted NS–WD merger model of Zhong et al. (2023) successfully reproduces the three distinct emission episodes of GRB 211211A: the MB arises during the hyperaccretion phase onto the NS, the EE originates from the propeller phase, and the X-ray plateau is powered by the spin-down of a post-merger magnetar. Moreover, the pronounced trough between the MB and EE is naturally explained as the transition from accretion to propeller phases."

    The entire three-episode engine (MB/EE/trough/plateau) that this paper then 'unifies' with r-process is justified by citing the lead author's own prior model already tuned to the same GRB, not by a new derivation or an external uniqueness result. The present work inherits that architecture and re-applies it; without the self-citation the prompt/afterglow skeleton has no independent support inside this manuscript.

  2. self citation load bearing [§2 Panel (c) and §3.1 (toroidal field / spike energy)]
    "if the NS has a surface field of Bs ∼10^14−10^15 G ... the toroidal field can rapidly amplify to Bϕ ∼10^15−5×10^16 G (see Fig. 1 in Zhong et al. 2023). ... If the spike energy originates solely from the magnetic energy of the accretion-amplified toroidal field, then using the relation Espike_γ,iso,ave ∼ B²_ϕ/8π ΔR³ ... one can infer a toroidal field strength of a few ×10^16 G. This is consistent with the range Bϕ∼10^15−5×10^16 G in Fig. 1 of Zhong et al. (2023)."

    Average spike energy is E_MB/N with N≡T90/τ_min from the data; converting that energy to Bϕ and calling it 'consistent with' the authors' own prior Fig. 1 is a self-consistency check against the same Bϕ range previously invoked for the same bursts' MB, not an independent field measurement. The GF-trigger threshold and spike energetics therefore rest on the self-cited amplification curve.

  3. self citation load bearing [§3.3 finding (2); magnetar parameters vs X-ray plateau]
    "For both GRBs 211211A and 230307A, the magnetar parameters initial spin period P0 and post-merger surface field Bs,post inferred from kilonova modeling differ from those derived from the X-ray plateau analysis in Zhong et al. (2023, 2024). As suggested by Zhong et al. (2023), this discrepancy may be reconciled if the magnetar's spin-down radiation exhibits a structured angular distribution: the dominant component is collimated along the GRB jet, powering the X-ray plateau, while a subdominant quasi-isotropic component injects energy into the surrounding ejecta."

    When the new kilonova fit returns different (P0, Bs,post) than the authors' own prior plateau fit on the same events, the tension is absorbed by re-invoking a structured-spin-down hypothesis from that same prior paper rather than by an external constraint. Parameter freedom is preserved by self-citation instead of being falsified.

  4. fitted input called prediction [Abstract; §2 last paragraphs on Mej; §3.3 finding (4) and Table 2]
    "The ensemble of such fireballs over the MB duration collectively yields Mej≳10^{-5}−10^{-3} M⊙ of ejecta, sufficient to power the observed kilonova signature when further boosted by the spin-down of the post-merger magnetar. ... From the modeling results in Table 2, both GRBs favor Mej∼10^{-2} M⊙. This large ejecta mass can be explained by the jet beaming effect, albeit requiring at least ten times more misaligned GF events than the observable along our LOS."

    Mechanism-side accounting is N_LOS×m_ej with N_LOS∼800–2000 from T90/τ_min and m_ej from Cehula, giving 10^{-5}–10^{-3} M⊙. The joint fit that actually reproduces the kilonova (Table 2) requires Mej∼10^{-2} M⊙ for both bursts. The gap is closed by promoting N_LOS to a lower limit and inserting a free factor (≳10× misaligned GFs, or fb∼10^{-5}–10^{-3}). That multiplicity is not fixed by the variability census used to define the MB forest—it is chosen so the mechanism can reach the fitted mass. Sufficiency is therefore partly by construction once the extra factor is free.

full rationale

The paper's prompt-emission architecture (hyperaccretion → MB, propeller → EE and MB–EE trough, post-merger spin-down → X-ray plateau) is taken wholesale from Zhong et al. (2023, 2024) by the same lead author and re-used on GRBs 211211A and 230307A, with toroidal-field values and the structured-spin-down fix for P0/Bs tension likewise cited from that chain. That is real self-citation load-bearing for the engine, but it is not a closed definitional loop: Kaltenborn accretion profiles, Cehula GF crustal ejecta, and Patel α-rich freeze-out yields are external, and the joint MCMC afterglow+kilonova fit is a genuine multi-parameter fit to data. The novel claim (MB as a GF-spike forest that also supplies r-process ejecta) therefore still has independent content. The weaker circularity is that the abstract's mechanism-side Mej ≳ 10^{-5}–10^{-3} M⊙ is declared 'sufficient,' yet Table 2 fits Mej ∼ 10^{-2} M⊙ for both bursts; sufficiency is recovered only by treating the LOS spike census as a lower limit and invoking ≳10× misaligned GFs (or a gamma-ray beaming factor applied to ejecta count). That multiplicity is not predicted a priori—it is adjusted so the mechanism can reach the fitted mass—so the kilonova mass budget is only partly predictive. Overall this is moderate self-citation plus one adjustable bridge, not a by-construction identity. Score 4.

Axiom & Free-Parameter Ledger

7 free parameters · 7 axioms · 3 invented entities

The claim rests on a stack of domain results from prior papers (tidal disruption disk, dynamo amplification, GF fireball ejecta, α-rich freeze-out) plus several free parameters fit to the two GRBs and a few entities introduced to close gaps (GF forest as MB, structured spin-down, large unseen flare multiplicity). Without the cold-crust-under-accretion and repeated-flare assumptions, the r-process and Mej numbers do not follow.

free parameters (7)
  • Mej (ejecta mass) = log10(Mej/M⊙)≈−1.91 (∼0.012 M⊙) for both GRBs
    Fit in joint MCMC kilonova+afterglow modeling; central to claiming sufficient r-process material.
  • v (ejecta velocity) = 0.34c (211211A); 0.11c (230307A)
    Fit characteristic expansion speed in kilonova model.
  • κ (opacity) = 0.88 cm² g⁻¹ (211211A); 4.28 cm² g⁻¹ (230307A)
    Fit; controls diffusion time and claimed r-process peak composition.
  • P0, Bs,post (post-merger magnetar) = P0∼142 ms, Bs∼6.7e14 G (211211A); P0∼255 ms, Bs∼4.6e14 G (230307A)
    Fit from magnetar-boosted kilonova term; also compared to prior X-ray plateau inferences.
  • Afterglow set (θj, EK,iso, Γ0, n, εB, εe, p) = See Table 2 (e.g. θj≈0.028 and 0.072 rad)
    Standard external-shock parameters fit jointly to multi-band data.
  • Mrp/Mej and fth = Mrp=0.5 Mej; fth=0.7
    Fixed by hand in joint modeling rather than derived.
  • Unseen GF multiplicity / beaming boost = ≳10× misaligned events (order-of-magnitude)
    Invoked to raise parcel-sum Mej∼10^{-5}–10^{-3} up to fitted ∼10^{-2} M⊙; not independently measured.
axioms (7)
  • domain assumption A massive WD is fully tidally disrupted by the NS into a constant-entropy disk with Ṁ ≳ 10^{-4} M⊙ s^{-1} for tens of seconds (CENW/CEEW).
    Taken from Kaltenborn et al. (2023) hydro simulations; sets duration and fuel for MB+EE.
  • domain assumption Hyperaccretion amplifies toroidal field via differential-rotation dynamo to Bϕ ∼ 10^{15}–5×10^{16} G, sufficient for repeated starquakes/GFs.
    From Spruit (1999) logic as applied in Zhong et al. (2023); load-bearing for the GF forest.
  • domain assumption Each GF initial spike is an e±–γ fireball that shocks a cold NS crust and unbinds mej ∼ 10^{-8}–10^{-6} M⊙ of material that undergoes α-rich freeze-out r-process despite Ye ≳ 0.4.
    Imported from Cehula et al. (2024) and Patel et al. (2025); the paper’s r-process solution.
  • domain assumption Pre-merger NS is already a magnetar with Bs ≳ 10^{14} G.
    Supported by cited precursor studies; required for rapid toroidal amplification to GF strengths.
  • domain assumption Transition rm ≲ rc → rm > rc maps cleanly onto MB → EE with an observed trough.
    Standard accretion/propeller picture as used in Zhong et al. (2023).
  • ad hoc to paper Minimum variability timescale equals single GF initial-spike duration; long decay tails are buried by subsequent spikes.
    Used in §3.1 to count ∼800 and ∼2000 spikes; analogy to Galactic GFs is plausible but not demonstrated for this regime.
  • ad hoc to paper Cehula cold-crust structure remains valid under ∼10 s hyperaccretion and rapid successive GFs.
    Explicitly uncertain in the paper’s own caveats; if false, ejecta masses and Ye/entropy may change.
invented entities (3)
  • Main-burst ‘forest’ of accretion-triggered magnetar GF initial spikes no independent evidence
    purpose: Identify the hard multi-spike MB with repeated GFs rather than magnetic bubbles or internal shocks alone.
    Organizes τmin, spike energetics, and crustal ejecta under one mechanism; not directly resolved as individual GFs in the data.
  • Structured (jet-collimated + quasi-isotropic) magnetar spin-down radiation no independent evidence
    purpose: Reconcile different (P0, Bs) inferred from X-ray plateau vs kilonova boosting.
    Introduced in §3.3 finding 2 without a calculated beam pattern or independent constraint.
  • Large population of LOS-misaligned GF events boosting true Mej no independent evidence
    purpose: Bridge parcel-sum ejecta (10^{-5}–10^{-3} M⊙) to fitted Mej ∼ 10^{-2} M⊙.
    Required by the numbers in §2 and §3.3; multiplicity is not measured.

pith-pipeline@v1.2.0-grok45-kimik3 · 22134 in / 5132 out tokens · 92155 ms · 2026-07-31T12:18:36.082747+00:00 · methodology

0 comments
read the original abstract

Peculiar long gamma-ray bursts (GRBs), exemplified by GRBs 211211A and 230307A, exhibit a long-duration multi-component prompt emission, an X-ray plateau in their afterglow, and a kilonova signature. Their origin remains highly debated. In this work, we present a unified picture for these events based on neutron star--white dwarf (NS--WD) mergers involving a pre-merger magnetar and a massive WD. In this picture, tidal disruption of the WD forms a constant-entropy accretion disk. Hyperaccretion from this disk onto the NS during the early accretion phase amplifies its toroidal magnetic field to strengths sufficient to trigger repeated magnetar giant flares (GFs). The main burst (MB) of the prompt emission consists of a ``forest'' of initial spikes from these GFs, while the subsequent magnetic propeller phase generates the extended emission (EE) and naturally explains the observed MB--EE trough. Crucially, the $e^{\pm}$-$\gamma$ fireball associated with each GF initial spike shocks the NS crust, leading to crustal ejection that synthesizes r-process heavy elements via the $\alpha$-rich freeze-out mechanism, thereby resolving the r-process deficit in conventional NS--WD hydrodynamic simulations. The ensemble of such fireballs over the MB duration collectively yields $M_{\rm ej}\gtrsim 10^{-5}-10^{-3}\,M_\odot$ of ejecta, sufficient to power the observed kilonova signature when further boosted by the spin-down of the post-merger magnetar. Meanwhile, the spin-down radiation also powers the X-ray plateau. This tidally disrupted NS--WD merger picture provides a self-consistent framework that unifies the prompt emission, afterglow, kilonova, and r-process nucleosynthesis observed in peculiar long GRBs.

Figures

Figures reproduced from arXiv: 2607.24531 by Jia-Hong Gu, Ji-Gui Cheng, Le Zou, Long Li, Shu-Qing Zhong, Yan-Zhi Meng.

Figure 1
Figure 1. Figure 1: The unified picture for peculiar long gamma-ray bursts (LGRBs) such as GRBs 211211A and 230307A from neutron star–white dwarf (NS–WD) mergers (see also Section 2). Panel (a): A massive WD (MWD ≳ 1 M⊙) is tidally disrupted by a magnetar (Bs ≳ 1014 G), forming an accretion disk that feeds the NS at a rate ≳ 10−4M⊙ s −1 lasting tens of seconds (≳ 10−2M⊙ s −1 lasting ∼ 10 s) described by hydrodynamic simulatio… view at source ↗
Figure 2
Figure 2. Figure 2: Joint modeling of the multi-wavelength light curves of the GRB afterglow and kilonova signature for GRB 211211A (left panel) and GRB 230307A (right panel), combining the standard afterglow (AG) model with the magnetar-boosted kilonova (KN) model. Dashed fitting lines show the contribution from the standard afterglow model alone, while solid lines represent the full model that includes both the afterglow an… view at source ↗

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