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REVIEW 3 major objections 5 minor 298 references

Young protoplanetary discs are open, fast-replenished systems: the full gas reservoir is exchanged on ~10 kyr timescales, and massive streamers repeatedly truncate the discs.

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2026-08-04 11:30 UTC pith:7HDVUTOQ

load-bearing objection Worth reading and refereeing: a genuinely new cloud-fed zoom-in sample of nine discs with a streamer census and replenishment calculation, but the headline claim that the 10 kyr replenishment and surface-layer mode are common to all systems is only demonstrated for one quiet system, and the truncation numbers disagree with themselves. the 3 major comments →

arxiv 2608.02204 v1 pith:7HDVUTOQ submitted 2026-08-03 astro-ph.EP

Accretion across scales: streamers, surface-layer transport, and rapid replenishment in young protoplanetary discs

Christian Granzow Holm , Michiel Lambrechts , Michael Kuffmeier , Anders Johansen , Troels Haugb{\o}lle , {\AA}ke Nordlund This is my paper
classification astro-ph.EP
keywords protoplanetary discsstar formationideal magnetohydrodynamicsaccretionstreamersdisc replenishmentClass 0 protostarsplanet formation
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 tries to establish that the earliest protoplanetary discs—still embedded in their natal cloud—are open systems, not closed reservoirs. From zoom-in ideal-magnetohydrodynamic simulations of nine forming star–disc systems resolved to 0.8 au, it argues that after roughly 50 kyr accretion onto the star proceeds through the midplane and a high-density surface layer, tied to a toroidal magnetic field with reversals across the disc, and that the entire disc mass is replenished on ~10 kyr timescales. It further identifies massive, ~0.2 solar-mass streamers that deliver gas at rates comparable to the background accretion flow and, on impact, shrink discs by about 65% in radius and 40% in mass. If true, these results imply that the outer parts of very young discs are too rapidly refreshed and too turbulent to build planets, and that quiescent planet-forming conditions must wait until later evolution.

Core claim

On its own terms, the paper claims that Class 0 discs pass through two stages. During the first ~50 kyr, the disc forms and grows through filamentary infall while polar outflows carve cavities. In the later quiescent stage, a layered accretion mode sets in: the midplane is turbulent while the disc surface layers carry the bulk of the inwards mass flux at ~1e-5 solar masses per year, and the toroidal magnetic field develops sign reversals across the surfaces and a current sheet in the midplane. The defining quantitative result is a replenishment timescale tau_rep = M_disc / Mdot_disc of about 10 kyr in the outer disc and 0.1 kyr in the inner disc, meaning the full disc mass reservoir is excha

What carries the argument

The central mechanism is layered 'surface-layer accretion' driven by a wound-up toroidal magnetic field. The field, with reversals across both disc surfaces and a current sheet in the midplane, transports angular momentum vertically and funnels gas inwards along the disc surfaces, while the midplane remains turbulent. The paper quantifies this with a replenishment timescale tau_rep(r) = M_disc(r) / Mdot_disc(r), computed through cylindrical shells, and identifies 'destroyer-class' streamers—overdense infalling filaments that deposit mass comparable to the background accretion flow and truncate the disc. The numerical machinery is zoom-in adaptive-mesh ideal-MHD simulation of cloud-fed collap

Load-bearing premise

The load-bearing premise is that ideal MHD with a barotropic equation of state, at 0.8 au resolution, faithfully captures how gas accretes in the outer disc; if non-ideal magnetic effects or unresolved heating change the accretion layers, the 10 kyr replenishment picture could collapse.

What would settle it

Run the same nine cloud-fed cores with non-ideal MHD (ambipolar diffusion and Ohmic resistivity) and radiative transfer at comparable resolution: if the surface-layer accretion channel and toroidal-field reversal disappear, or if the outer-disc replenishment time rises above ~100 kyr, the central claim fails. Observationally, mapping ionisation tracers and infall kinematics in the outer regions of Class 0 discs could test whether the assumed well-ionised, strongly coupled regime actually holds.

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

If this is right

  • Outer regions of very young discs are not planet-forming sites: high turbulence, rapid gas refreshment, and streamer disruption hinder dust growth and planetesimal formation.
  • Discs can remain gravitationally stable (disc-to-star mass ratio below 10%) even while accreting at ~1e-5 solar masses per year; episodic bursts correlate with transient regions of marginal Toomre-Q instability.
  • Destroyer-class streamers naturally produce periods of disc truncation (size down ~65%, mass down ~40%) followed by regrowth on ~10 kyr timescales, offering an explanation for compact discs seen around outbursting young stars.
  • Rapid replenishment erases spatially separated chemical or isotopic reservoirs in the early disc, so any such reservoirs must be established later, when infall has declined.
  • Surface-layer accretion with toroidal-field reversal, previously seen in ideal-MHD disc models, operates in realistic embedded discs and connects stellar accretion to disc surface layers.

Where Pith is reading between the lines

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

  • If the 10 kyr replenishment is representative, the onset of planet formation is time-sequenced: the inner few au may quench first while the outer disc remains hostile; searches for planet formation tracers should be weighted toward older, less infall-dominated systems.
  • The streamer truncation and regrowth cycle predicts observable variability in disc outer radii and accretion rates at ~10 kyr intervals; high-cadence monitoring of Class 0 or outbursting young stellar objects could test this directly.
  • Because the simulations are ideal MHD, they likely represent a maximally magnetically coupled regime; a non-ideal MHD rerun could weaken the surface-layer channel and change the replenishment timescale, so the 10 kyr number is best read as contingent on that assumption.
  • With roughly five massive streamers among nine systems over 100 kyr, most young discs should experience at least one destroyer-class event, implying that snapshot measurements of Class 0 disc sizes may often catch discs in a post-truncation regrowth phase.

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

3 major / 5 minor

Summary. The paper presents three-dimensional ideal-MHD zoom-in simulations of nine young protoplanetary-disc systems formed in a (4 pc)^3 molecular-cloud simulation, resolving the inner discs to 0.8 au. The authors characterize disc formation, accretion modes, magnetic-field structure, streamer infall, and disc-size/mass evolution over ~10^5 yr. The central claims are that in the later quiescent phase (t ≳ 50 kyr) accretion proceeds predominantly through the disc surface layers, that the full disc mass reservoir is replenished on ~10 kyr timescales, and that massive streamers episodically truncate discs by ~65% in radius and ~40% in mass, making the outer regions of young discs inhospitable to planet formation.

Significance. If correct, the paper would substantially advance the picture of Class 0 disc evolution: rather than isolated, viscously spreading discs, these systems are open, continuously replenished reservoirs whose outer regions are too dynamic for early planet formation. The work benefits from a realistic cloud-scale environment, a sample of nine systems, and unusually detailed appendices, including a resolution study and a transparent description of the sink model and disc-fitting procedures. The qualitative scenario is internally consistent and the simulation campaign is a technical achievement. However, the most general claims — surface-layer accretion and 10 kyr replenishment — are demonstrated in detail for only one, deliberately quiet system, and the paper's own resolution study warns that quantitative accretion rates have not fully converged. The significance of the universal conclusion is therefore not yet established at the level claimed.

major comments (3)
  1. [Sec. 4.5, Sec. 8, Abstract] The central universal claim is supported by only one system. The replenishment-time analysis (Eqs. 12–13) and Fig. 10 are computed exclusively for system 180, which was explicitly selected because it did not experience a major disruptive streamer event and has low magnetic field, low mass budget, and low rotational energy (Sec. 4). Section 8 nevertheless concludes that 'accretion flows predominantly along the disc surface' are 'common to all systems', and the abstract generalizes to 'young discs'. Section 5 shows large diversity — e.g., systems 82 and 122 do not approach a quasi-steady state (Sec. 5.5) — but no equivalent spherical-shell or cylindrical mass-flux decomposition is presented for the other eight systems. The manuscript should either provide the surface-layer/replenishment analysis for the full sample or explicitly restrict the claim to the quiescent, ideal-MHD regime exempli
  2. [Appendix A.4, Sec. 4.5] The quantitative accretion and replenishment rates are resolution-dependent. Figure A.1 shows that stellar accretion rates decrease with increasing resolution for systems 13 and 225, and the text estimates that at 0.8 au resolution the stellar mass is overestimated by up to 30%. The headline values Mdot ~ 10^-5 M_sun/yr and tau_rep ~ 10 kyr are derived from system 180 at the fiducial 0.8 au resolution, but no convergence test is shown for that system or for the cylindrical mass-flux measurement underlying Eq. (13). If the true accretion rate is lower, the replenishment time is correspondingly longer. The authors should quantify this uncertainty for the specific quantities used in the central claim, or explicitly state that tau_rep is a resolution-dependent upper/lower bound.
  3. [Sec. 6.1, Sec. 7] The applicability of the surface-layer accretion and replenishment picture to real discs rests on the ideal-MHD assumption, which the authors themselves call 'a crude approximation during the initial stages of disc growth on small scales ≲10 au'. The 10 kyr replenishment calculation includes radii r < 20 au (Fig. 10), and the surface-layer/toroidal-field-reversal pattern is an ideal-MHD result. Non-ideal effects such as ambipolar diffusion are known to reduce magnetic braking and alter the vertical current distribution, so they could change both the accretion geometry and the replenishment timescale. Since the planet-formation implications in Sec. 7 depend on high replenishment rates and strong turbulence, the manuscript should either provide a quantitative estimate of the expected non-ideal correction or clearly limit the conclusions to the well-ionised, ideal-MHD regime.
minor comments (5)
  1. [Abstract vs. Sec. 5.5 / Sec. 8] The abstract states streamers reduce disc size 'by half', while Sec. 5.5 and the conclusion state 'an average reduction by approximately 65 %'. These should be reconciled.
  2. [Sec. 5.4] The term 'destroyer-class streamer' is introduced informally. Since it is used as a classification criterion (M_str > M_disc), it would be clearer to state this condition explicitly at first use and give the threshold for the class.
  3. [Appendix A.4] The text says 'accretion rates decrease with increasing levels of refinement' but does not state the magnitude of the change for the two test systems. Adding the percentage decrease or a range in the caption of Fig. A.1 would help readers gauge the convergence uncertainty.
  4. [Sec. 4.4.2 / Fig. 8] The sentence 'The dashed grey line in panel b of Figure 8 shows the thermal scale height for a nearly isothermal disc' is followed by reference to a 'black dash-dotted line' without a clear colormap/line-style key in the text. Consider making the line styles easier to distinguish in the printed figure.
  5. [Sec. 6.1] The reference to 'recent observations hint that effective ionisation rates are high near young stellar objects' is supported by several citations, but the sentence does not specify which of the cited observations corresponds to B335 versus L1157; moving the parenthetical objects to the relevant citations would improve clarity.

Circularity Check

0 steps flagged

No significant circularity: the central results are measured simulation diagnostics, not derived from their own inputs.

full rationale

The paper's central claims — surface-layer accretion, streamer-driven truncation, and a ~10 kyr disc replenishment timescale — are obtained as direct measurements from the hydrodynamical simulations. The replenishment time is computed from the explicitly defined ratio τ_rep = M_disc / Ṁ_disc (Eqs. 12–13), with both quantities evaluated from the simulated density and velocity fields; this is a diagnostic definition, not a fitted parameter disguised as a prediction. The mass-flux angular structure of Eq. 5 is likewise a direct azimuthal average of simulated fluxes. No equation in the paper reduces the claimed result to an input parameter, and no fitting step is renamed as a prediction. The self-citations (Haugbølle et al. 2018 for the sink prescription and parent run; Kuffmeier et al. 2017 for the replenishment-time definition; Nordlund et al. 2018 for DISPATCH) are methodological and do not carry the physical conclusion. The surface-layer accretion mode is explicitly compared to independent external simulations (Suzuki & Inutsuka 2014; Zhu & Stone 2018), not asserted solely by self-citation. There is no imported uniqueness theorem and no ansatz smuggled in through a citation. The main caveat is that the detailed replenishment and surface-layer analysis is presented for system 180 only, while the conclusion generalizes it to all systems; this is an external-validity / overgeneralization concern, not a circularity. The paper also self-identifies ideal MHD as a crude approximation at small scales (Sec. 6.1) and resolution-dependent accretion rates (Appendix A.4), which are acknowledged limitations rather than circular steps. Overall, the derivation chain is non-circular.

Axiom & Free-Parameter Ledger

5 free parameters · 5 axioms · 0 invented entities

No new physical entity is introduced; 'destroyer-class streamer' is a classification. The listed free parameters are numerical/sub-grid choices and the adopted EOS. The quantitative claims depend on these choices, especially the sink model, and on the ideal-MHD approximation.

free parameters (5)
  • Sink disc-accretion efficiency chi_disc = 10^-3
    Controls the rate at which material in the accretion sphere spirals onto the sink (Eq. A.8). Directly sets stellar accretion rates and the inner-disc surface density plateau visible in Fig. 8b.
  • Sink free-fall efficiency chi_ff = 1
    Sets free-fall accretion onto the sink when no rotationally supported disc is present (Eq. A.9). Affects early accretion rates and sink growth.
  • Sink max accretion fraction epsilon_max = 80%
    Limits how much gas a cell can lose per timestep (Appendix A.3). Influences outflow/accretion balance and the quoted accretion-rate values.
  • Barotropic EOS break densities and exponents = rho1=2.50e-16, rho2=3.84e-13, rho3=3.84e-8, rho4=3.84e-3 g cm^-3; exponents 1.1, 7/5, 1.1, 5/3
    Adopted from Masunaga & Inutsuka (2000); replaces the energy equation. Sets thermal support, scale height, and thus all disc-structure and Toomre-Q statements.
  • AMR refinement parameters = LJ,min=8 cells per Jeans length; omega_max=5; geometric distance 144 cells; hysteresis 0.4/1.0/1.4
    Determine where resolution is added (Eqs. 1–3). Convergence test (Fig. A.1) shows accretion rates change with maximum refinement level, so these choices affect quantitative results.
axioms (5)
  • domain assumption Ideal MHD equations with a barotropic EOS adequately capture outer-disc accretion physics.
    Used throughout. The authors call ideal MHD 'a crude approximation during the initial stages of disc growth on small scales ≲10 au' (Sec 6.1) and do not model ambipolar diffusion, Ohmic dissipation, or radiative transfer.
  • ad hoc to paper Sink particle sub-grid model represents the protostar and inner boundary.
    Accretion uses tuned chi_disc=1e-3, chi_ff=1, epsilon_max=80%, and does not accrete magnetic field (Appendix A.3). This affects the stellar accretion rates and inner-disc structure.
  • domain assumption The selected nine isolated cores are representative of young Class 0 discs.
    Sinks are the most isolated candidates with final stellar mass 0.5–1 M_sun (Sec 2.3). Clustered formation and strong interactions are excluded, yet conclusions are phrased generically about young discs.
  • domain assumption Cosmic-ray ionisation reaches the outer disc midplane at r>10 au.
    Used to justify applying ideal MHD in the outer disc (Sec 6.1). Ionisation is not modelled; recent observations of elevated ionisation rates are cited, but stellar-wind shielding could reduce them.
  • domain assumption Disc radius can be identified by v_phi>0.8 v_kep plus Rayleigh stability after filtering.
    All disc size, mass, and replenishment numbers depend on this definition (Sec 4.4.1, Appendix A.5). The authors note the procedure 'requires a certain amount of tuning to be robust'.

pith-pipeline@v1.3.0-daily-deepseek · 33071 in / 16821 out tokens · 128680 ms · 2026-08-04T11:30:01.640431+00:00 · methodology

0 comments
read the original abstract

Protoplanetary discs evolve around newly-formed stars through an interplay of infall from surrounding turbulent cloud material, accretion towards the young star, and outflow driven mass-loss. It has been challenging to determine if discs are fed predominantly through infall along the disc midplane, or along the poles, and if accretion occurs in a steady or burst-like fashion. Here, we present a suite of 3D ideal magnetohydrodynamical simulations of protoplanetary disc formation and evolution in a dynamic, large-scale molecular cloud environment using the adaptive mesh refinement framework DISPATCH. We focus on nine stellar systems, where we resolve discs down to a scale of 0.8 au. Across the sample, stellar accretion proceeds at rates of $\sim$10$^{-5}$ M$_\odot$ yr$^{-1}$ over 10$^{5}$ yr, with significant variability. Discs grow to 100 au scales and remain gravitationally stable in time, with disc-to-star mass ratios below 10 %. Transient high-density streamers, with 10 kyr infall times, can drive anisotropic mass delivery at rates comparable to the background accretion flow. Their interaction with discs typically results in a temporary reduction of the disc size by half, and disc mass by 40 %. During later quiescent disc evolution stages ($t\gtrsim$50 kyr), accretion predominantly occurs through the midplane and disc surface layers. This is associated with the development of a toroidal magnetic field morphology, which includes field reversals across both disc surfaces. In this way, the full disc mass reservoir is replenished on 10 kyr-timescales. These findings support that the outer parts of very young discs, when well-ionised and close to the ideal MHD regime, are not yet conducive to planet formation, due to high replenishment rates, strong turbulence, and disruptive streamer infall events.

Figures

Figures reproduced from arXiv: 2608.02204 by {\AA}ke Nordlund, Anders Johansen, Christian Granzow Holm, Michael Kuffmeier, Michiel Lambrechts, Troels Haugb{\o}lle.

Figure 1
Figure 1. Figure 1: Time evolution of the column density of the full simulation domain showing the creation of sink particles, including the 9 systems analysed in this paper (see symbols above the plots). Panel a: The formation of the first generation of sinks, including sink 6 (red circle), at a time tGlobal = 0.15 Myr of the global parental run (Sec. 2.2). Panel b: Snapshot in time subsequent to the formation of sink 122, a… view at source ↗
Figure 2
Figure 2. Figure 2: Integrated column densities (Σ) at four different scales, zooming in on system 13 at t = 62 kyr. The integration depths are: 4 pc for panel a, 0.4 pc for panel b, 0.04 pc for panel c, and 0.004 pc for panel d. Panel (a) displays the full computational domain with an average column density of Σ = 3.9 × 10−2 g cm−2 . Zooming in on 13, panel (b) shows how the star and disc form along dense filaments on scales… view at source ↗
Figure 3
Figure 3. Figure 3: Density profiles of the nine selected systems at the star creation time T0 (see row 2 in [PITH_FULL_IMAGE:figures/full_fig_p004_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Time evolution of face-on (top panels) and edge-on (bottom panels) column densities for system 180. The integration depths are 80 au for the face-on panels and 5 au for the edge-on panels, in order to best visualise the empty polar cavities made by outflows. The disc grows with time through filamentary infall, depleting the surroundings of gas. the environment by creating low-density polar cavities through… view at source ↗
Figure 5
Figure 5. Figure 5: Time and azimuthally averaged mass flux M˙ ⟨ϕ⟩ , with the poloidal component of the flow. The spin axis is defined as the total angular momentum vector within 150 au. All values are averages over 1.1 kyr, corresponding to the dynamical timescale of the disc. The streamlines represent the poloidal component of the velocity, i.e. vr and vθ . The black line shows the fitted scale height and the disc edge, tog… view at source ↗
Figure 6
Figure 6. Figure 6: Full time evolution of the mass flux through a 60 au shell for system 180, showing M˙ ⟨ϕ⟩ as a function of latitude with respect to the midplane and time. Blue signifies outflow and red inwards accretion. t ∼ 50 kyr. While the disc midplane (|θ| ≲ 30◦ ) exhibits a highly turbulent flow, the disc surface (30◦ ≲ |θacc| ≲ 50◦ ) is domi￾nated by inwards accretion flows. This mode of layered surface accretion i… view at source ↗
Figure 7
Figure 7. Figure 7: The toroidal and poloidal field of the magnetic field is plotted here at 6 times, averaged over the dynamical scale of the disc (1 kyr). The streamlines show the azimuthally-averaged poloidal field, and the underlying colour map shows the toroidal component. Note the difference in colour scale range between poloidal and toroidal fields. significantly different magnetic field configuration, correspond￾ing t… view at source ↗
Figure 9
Figure 9. Figure 9: High resolution time evolution of disc mass and size for system 180. The uncertainty derived from the disc size determination methods is plotted as the grey area. The disc sizes and masses are time averaged according to the dynamical timescale (Htherm ∝ r 3/2 ). The black dash-dotted line shows Heff for a con￾stant β = 0.1, which is roughly consistent with the plasma-β val￾ues in our simulations (Fig.B.2) … view at source ↗
Figure 8
Figure 8. Figure 8: Panel a: Time evolution of the toroidal velocity over true Kep￾lerian velocity, which is one part of the definition of the disc size. Panel b: Time evolution of the gas scale height. Panel c: Time evolution of surface density of system 180. The dashed line shows the MMSN ra￾dius scaling as reference (Hayashi 1981). Here, Σcalc, is the calculated Σ obtained from Eq. (9) and plotted with the dashed dark gree… view at source ↗
Figure 10
Figure 10. Figure 10: Panel a: Accumulated mass within the disc at a given radius, computed from the fitted surface density. The mass is computed using only 38 % and 48 % of Σ, corresponding to the material contained within |z| < 1 2 H and 1 2 H < |z| < 3 2 H. Panel b: Integrated mass flux through the lateral surface of a cylinder extending |z| < 1 2 H and 1 2 H < |z| < 3 2 H. Panel c: Replenishment time as a function of radiu… view at source ↗
Figure 11
Figure 11. Figure 11: Computed accretion rate for the nine systems as a function of time. The star data has a time resolution of 10 years, making it the data with the highest cadence. The triangles signify the time of the snapshots seen in [PITH_FULL_IMAGE:figures/full_fig_p011_11.png] view at source ↗
Figure 12
Figure 12. Figure 12: Panel a: Time evolution of the Toomre Q parameter as a func￾tion of radius for system 180. The grey-hatched region marks the re￾gion where the Toomre Q parameter has no clear physical meaning, corresponding to periods when no disc is present or locations outside of the outer disc edge marked with a white line. The disc remains glob￾ally gravitationally stable at all times. However, during the disc evolu￾t… view at source ↗
Figure 13
Figure 13. Figure 13: Five streamers in four different systems. The integrated depth for all plots is 2000 au. The colours display the integrated density, and the streamlines are the projected velocity in au yr−1 . The solid black line marks the streamer boundary, while the dashed black line indicates the region, containing 68.2 % of the streamer mass. The red solid line shows the star-disc region. Each streamer is labelled in… view at source ↗
Figure 14
Figure 14. Figure 14: Snapshots of mass accretion as a function of polar angle at dif￾ferent times (t = 20, 30, 40 kyr) for system 13. The flow lines show the mass-averaged poloidal field flow. The panels are azimuthally and tem￾porally averaged over a dynamical timescale of 1 kyr. The disc bound￾aries, as shown in Sec. 4.4, are plotted with a black contour. Panel a (t = 20 kyr) shows prominent outflows along the polar axis (|… view at source ↗
Figure 16
Figure 16. Figure 16: Evolution of disc and star mass as a function of time for all sys￾tems. The disc masses shown here are the accumulated mass enclosed within z ± 3H integrated to the outer disc edge (shown in [PITH_FULL_IMAGE:figures/full_fig_p014_16.png] view at source ↗

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