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A supernova accretion disk can keep launching jets even after the gas feeding it loses its spin, because viscosity ships angular momentum outward — and this can explain why some supernova remnants show just a few dominant jet pairs.

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2026-08-01 10:09 UTC pith:XR3GZAUM

load-bearing objection A self-consistent order-of-magnitude argument that zero-angular-momentum accretion can be survived for about one viscous time, but the central capture assumption is unmodeled and the headline timescale is largely the input timescale. the 4 major comments →

arxiv 2607.20314 v1 pith:XR3GZAUM submitted 2026-07-22 astro-ph.HE

Long-lived intermittent accretion disks in the jittering jets explosion mechanism (JJEM) of core-collapse supernovae

Noam Soker (Technion , Israel) This is my paper
classification astro-ph.HE
keywords core-collapse supernovaejittering jets explosion mechanismintermittent accretion disksangular momentum transportviscosity timescalejet feedbacksupernova remnant morphologyneutron star accretion
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.

The paper argues that intermittent accretion disks in the jittering-jets explosion mechanism (JJEM) can live much longer than the angular-momentum fluctuations that create them. Specifically, when a disk formed by high-angular-momentum material is subsequently fed gas with zero angular momentum, viscous outward angular-momentum transport lets the disk linger for roughly its own viscous timescale and swallow a few tenths of its own mass before dying. This viscous survival, combined with jet-driven clearing of polar infall and occasional positive-sum angular-momentum fluctuations, can produce the one to three very energetic jet pairs that some supernova remnants show. The result matters because it strengthens the case that jets, not neutrinos, power most core-collapse supernovae.

Core claim

The author shows with an order-of-magnitude analytic model that an α-disk around a newly born neutron star does not necessarily die when the accreting gas loses its angular momentum. Equations (13) and (14) give the disk's extra accreted mass as ΔM_D ≈ 0.3 M_D0 (Q−1)/0.3 and its survival time as Δt_D ≈ τ_vis (Q−1)/0.3 × R/(3H), so the disk accretes a substantial fraction of its own mass and survives about one viscous time. The mechanism is that viscosity transfers angular momentum outward, while the disk's stored angular momentum reservoir, quantified by the factor Q derived from its surface-density profile, provides the resources to keep accreting zero-angular-momentum gas. These two positi

What carries the argument

The central object is an intermittent accretion disk around the newly born neutron star, modeled as an α-disk with viscous time τ_vis ≈ 0.01–0.1 s. The key identity is the angular-momentum reservoir factor Q, obtained by integrating the assumed surface density Σ ∝ r^{−3/4} over the disk; Q ≈ 1.3–1.4 measures how much angular momentum the disk stores relative to its inner jet-launching radius. This Q enters the viscous-outward-transport bookkeeping that produces the extra-mass and survival-time estimates, while the jets themselves are assumed to carry away angular momentum from the inner region.

Load-bearing premise

The disk remains a coherent, roughly Keplerian α-disk with a smooth surface-density profile while being fed zero-angular-momentum gas, even though the author admits the disk is not fully relaxed and the standard thin-disk model cannot be applied.

What would settle it

A 3D hydrodynamical simulation of an α-viscosity disk around a neutron star that is suddenly fed gas with zero angular momentum at 0.1–0.3 M⊙/s would settle it: if the disk fragments, becomes strongly non-Keplerian, or accretes in less than one viscous time, then equation (14) overestimates the disk's survival time.

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

If this is right

  • An intermittent accretion disk can survive the end of the high-angular-momentum episode that formed it, extending jet-launching activity by roughly one viscous time.
  • Jet-launching episodes can last up to a few tenths of a second and carry a large fraction of the explosion energy, matching the energetic jet pairs inferred in some supernova remnants.
  • The combination of viscous prolongation, jet-blown bubbles channeling accretion to the equatorial plane, and random angular-momentum fluctuations can produce 1–3 dominant jet pairs rather than many weak ones.
  • The JJEM can account for supernova remnant morphologies with few, energetic jet axes without requiring rapid pre-collapse core rotation.
  • The number of dominant jet pairs scales with the viscous time, so variations in disk viscosity or scale height directly affect the observed morphology.

Where Pith is reading between the lines

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

  • If viscous survival operates similarly in black-hole accretion disks fed by stochastic fallback, it could help explain long-duration gamma-ray bursts that lack a persistent, ordered angular momentum source.
  • The Q-factor bookkeeping assumes instantaneous mixing of zero-angular-momentum gas; incomplete mixing could create counter-rotating layers that either shorten or lengthen the disk's life, a regime not modeled here.
  • A testable prediction is that a supernova remnant should rarely show more than three comparably energetic jet pairs; a four-pair case with similar energies would stress the model.
  • Applying the argument to disks around lower-mass proto-neutron stars (where the inner launching radius and viscous time shift) may predict a mass dependence in the appearance of energetic jet pairs.

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 / 4 minor

Summary. The paper, in the framework of the jittering-jets explosion mechanism (JJEM), proposes a mechanism for forming long-lived intermittent accretion disks around newly born neutron stars. The author considers two consecutive accretion episodes: the first with positive specific angular momentum forms a Keplerian-like disk, and the second has zero angular momentum. The central claim is that viscous outward angular momentum transport (Eq. 8) allows the disk to continue accreting zero-angular-momentum gas, with the disk surviving for a time Δt_D ≈ τvis (Eq. 14) and accreting an extra mass ΔM_D ≈ 0.3 M_D0 (Eq. 13). Two additional processes—jet-induced blocking of polar accretion and random angular momentum fluctuations—are argued to further prolong disk lifetime. The paper applies this to explain CCSNRs with two or three energetic jet pairs, such as S147, W44, RCW 89, and G0.9+0.1, thereby strengthening the JJEM as the primary CCSN explosion mechanism.

Significance. If the proposed mechanism is physically valid, it would offer a natural explanation for CCSNRs whose morphology requires two or three jet pairs carrying most of the explosion energy—a feature that is difficult to accommodate within the standard JJEM picture of many short-lived, low-energy jet episodes. The paper is transparent about its assumptions and provides order-of-magnitude estimates that could be tested by future three-dimensional simulations. It also explicitly identifies its speculative nature. However, the quantitative results hinge on a strong and as-yet-unjustified assumption about how zero-angular-momentum gas is captured by the disk, and the headline timescale is essentially the assumed viscous time. Therefore, the significance of the paper is conditional; it is an interesting proposal that currently lacks a firm physical basis for its key bookkeeping step.

major comments (4)
  1. [§3.2, Eq. (9)] The derivation assumes that zero-angular-momentum gas from the second episode is captured by the disk and adds to its mass. This is not self-evident: a parcel with j=0 at R≈50 km has a dynamical infall time τ_K≈0.005 s (Eq. 3), an order of magnitude shorter than τvis≈0.05 s used in Eq. (14). Without centrifugal support, such gas will plunge through the disk on a dynamical time unless pressure gradients or shocks transfer angular momentum to it. The paper does not derive a mechanism or a timescale for this capture, and in §3.1 it admits that the disk is not fully relaxed and the standard thin-disk model cannot be used. Equations (13) and (14) are therefore contingent on an unexamined physical process, and the claimed prolongation may substantially overestimate ΔM_D and Δt_D.
  2. [§3.2, Eq. (11)] The angular momentum reservoir J_D,0 is computed assuming a Keplerian disk with surface density Σ∝r^{-3/4}, a profile characteristic of a steady, optically thick, blackbody-emitting disk. The paper states in §3.1 that such a model cannot be used for these intermittent disks, and indeed acknowledges 'although this is not the case here' before Eq. (11). The factor Q, and hence the numbers in Eqs. (13)–(14), depend on this choice. The author should either provide a physical justification for adopting this profile for a non-relaxed disk or demonstrate that the results are insensitive to the profile.
  3. [§3.2, Eq. (14)] The headline result Δt_D ≈ τvis (Q−1)/0.3 × R/(3H) is dimensionally and substantively a restatement of the assumed viscous timescale τvis. Since τvis is an input parameter (Eq. 1) calibrated to earlier JJEM work, the paper does not predict a new lifetime scale but rather shows that the disk can survive for its own viscous time under certain conditions. The paper should acknowledge this limitation more explicitly; as written, the conclusion that 'the disk can survive for a typical time of the order of its viscous time' is partially circular.
  4. [§3.2, Eq. (13)] Equation (13) equates the angular momentum lost at the inner boundary with (M_D0+ΔM_D)j_d,j. However, the zero-angular-momentum gas in the second episode carries no angular momentum; it cannot lose j_d,j when it reaches the inner disk unless it has been spun up by the disk. The bookkeeping therefore implicitly assumes that all accreted gas, including the zero-j component, acquires the local specific angular momentum before accretion. This is the same capture problem as in the first major comment, but it deserves separate emphasis because it is an internal inconsistency in the angular momentum conservation statement: the newly added mass should not be debited the disk's angular momentum unless it has been entrained.
minor comments (4)
  1. [§3.2, text] 'accretion is continues' should read 'accretion is continuous'.
  2. [Appendix] 'in he study' is a typo for 'in the study'.
  3. [Figure 1] The caption refers to 'red double-lined arrows' and 'dashed-pale-blue arrows', but the figure as rendered appears to have no color or the color coding is unclear. The text should be adjusted to match the actual figure formatting.
  4. [Abstract/Introduction] The abbreviations CCSNR and CCSNe are used without full definitions at first occurrence. Considering the broad readership of the journal, the author should define both terms explicitly.

Circularity Check

0 steps flagged

No significant circularity: the disk-lifetime result is angular-momentum bookkeeping, not a fitted prediction.

full rationale

The derivation chain in §3.2 is an angular-momentum bookkeeping calculation, not a fitted prediction. Equation (11) integrates an assumed Σ ∝ r^{-3/4} disk to define Q; equation (13) follows algebraically from the angular-momentum equality (M_D0 + ΔM_D) j_d,j = J_D0; equation (14) then substitutes the definitional relation Mdot_acc = M_D0/τvis and k = H/R, giving Δt_D ≈ τvis. This makes the final timescale algebraically tied to the input viscous time, but the paper does not fit τvis to the result, nor rename a fitted parameter as a prediction. It explicitly labels the calculation an idealized order-of-magnitude estimate and calls for simulations ('Presently, my suggestion is in a somewhat speculative phase. Future hydrodynamical simulations will have to examine all three processes.'). The many self-citations contextualize the JJEM and the CCSNR morphological interpretations, but the new disk-lifetime mechanism does not depend on an unverified self-citation or an imported uniqueness theorem. The admitted inconsistency between 'I cannot use the standard model' and the later adoption of the standard Σ ∝ r^{-3/4} surface density is a physical/correctness concern (as is whether zero-j gas is actually captured rather than plunging), not a circularity. I therefore find no significant circularity in the paper's central derivation.

Axiom & Free-Parameter Ledger

5 free parameters · 7 axioms · 0 invented entities

The paper introduces no new particles, forces, or conserved quantities. It relies on standard accretion disk physics plus the JJEM framework and a qualitative morphological interpretation of supernova remnants. The free parameters are all order-of-magnitude assumptions; none is fitted to data, but the central quantitative output Δt_D ≈ τvis is largely determined by the assumed input τvis.

free parameters (5)
  • α (viscosity parameter) = ≈0.15 (assumed)
    Sets the viscous timescale via Eqs. (1)–(4); taken as a representative value for intermittent disks around a newborn NS, not measured.
  • H/R (disk aspect ratio) = ≈1/3 (assumed, via R = 3H)
    Controls the fraction k = H/R of infalling gas that reaches the disk (Eq. 9) and directly scales the prolonged lifetime in Eq. (14).
  • τvis (disk viscous timescale) = 0.01–0.1 s (input)
    Taken from Soker 2025b and Müller et al. 2017; the main result Δt_D ≈ τvis is essentially this input timescale restated.
  • Mdot_acc (mass accretion rate) = 0.3 M⊙/s (scaled)
    Used to estimate disk density and set M_D0/τvis; based on Müller et al. 2017, acknowledged to vary with time.
  • R_d,j and R_D (inner and outer disk radii) = ≈20 km and ≈50–60 km
    Set the specific angular momentum j_d,j and the factor Q = 1.3–1.4 in Eq. (11); chosen to represent the jet-launching region and the outer intermittent disk.
axioms (7)
  • domain assumption CCSNe are exploded by jittering jets from intermittent accretion disks around the newborn NS (JJEM)
    The paper is framed entirely within JJEM; not derived here, based on a long list of self-authored prior papers (§1).
  • domain assumption Stochastic angular momentum fluctuations in pre-collapse convective zones seed the intermittent disks
    Quoted from Gilkis & Soker 2015 and Müller et al. 2017; underlies the zero-j / fluctuating-j feeding in §3.2.
  • domain assumption The disk is Keplerian and uses the α-viscosity prescription ν = α C_s H
    Used throughout Eqs. (1)–(8); the paper recognizes the disk is not a standard thin optically-thick disk but uses α anyway (§3.1).
  • ad hoc to paper Surface density profile Σ ∝ r^{−3/4} (blackbody disk) despite the disk not being that type
    Invoked to compute the total disk angular momentum factor Q in Eq. (11); the paper says 'although this is not the case here'.
  • ad hoc to paper The disk survives as long as its specific angular momentum exceeds j_d,j; at death all remaining disk angular momentum is lost at the inner edge
    Central to the bookkeeping behind Eqs. (13)–(14); a chosen survival criterion, not a derived result.
  • domain assumption Jets block polar accretion, forcing subsequent accretion to arrive preferentially from the equatorial plane
    Feedback process (1), cited from Soker 2025c; used to justify k = H/R in Eq. (9) and in §3.3.
  • domain assumption Observational identification of 1–3 energetic jet pairs in CCSNRs via point-symmetric morphology is reliable
    Motivates the entire study (§2, Appendix); the method is qualitative and new to CCSNRs, as the Appendix admits.

pith-pipeline@v1.3.0-alltime-deepseek · 12871 in / 17874 out tokens · 154999 ms · 2026-08-01T10:09:59.644614+00:00 · methodology

0 comments
read the original abstract

Motivated by observations of core-collapse supernova (CCSN) remnants that suggest cases where one to three energetic pairs of jets dominate the CCSN remnant morphology and, hence, the CCSN explosion energy, I examine the formation of long-lived intermittent accretion disks that launch such pairs of energetic jets in the framework of the jittering-jets explosion mechanism (JJEM). In the JJEM, pairs of jets explode all CCSNe. In most CCSNe, stochastic angular momentum fluctuations in the convective zones of the pre-collapse core seed instabilities above the newly born neutron star that lead to the formation of intermittent accretion disks. These disks launch several to about twenty pairs of jets that explode the star. CCSNRs with signatures of 1-3 very energetic pairs of jets require long-lived, intermittent accretion disks. I show that viscosity-driven angular momentum transport in the disk can prolong its lifetime even when material with zero angular momentum continues to feed the disk. In addition, the jets prevent matter from accreting from the polar direction, thereby extending the disk's lifetime. These two positive feedback processes, and the fluctuations that, in some cases, add up to a positive angular momentum, can substantially prolong the lifetime of 1-3 intermittent accretion disks (or none), which then launch the energetic pairs of jets. This study adds to the wide variety of morphologies that the JJEM can explain, hence strengthening the JJEM as the primary explosion mechanism of CCSNE.

Figures

Figures reproduced from arXiv: 2607.20314 by Israel), Noam Soker (Technion.

Figure 1
Figure 1. Figure 1: A schematic drawing of the flow structure when a new accretion episode with an average zero angular mo￾mentum occurs immediately after an accretion episode that formed a developed and more or less relaxed accretion disk that launches jets (depicted by the red double-lined arrows). The NS is at the center, and the disk’s angular momentum is vertical in the figure. The equatorial plane is horizontal along th… view at source ↗

discussion (0)

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