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Compact protoplanetary discs can be produced by dead zones

T0 review · 3 major / 6 minor · reviewed 2026-08-08 · deepseek-v4-flash

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Pith's one-line read Dead zones can explain the prevalence of compact protoplanetary discs: when fragile dust fragments in the moderately turbulent region beyond the dead zone, the observed mm-sized dust disc is cut off at the dead zone edge, so disc size…

desk verdict Plausible new compact-disc mechanism via dead-zone fragmentation, but the central claim depends on a narrow parameter regime and the pre-relaxed gas initial condition needs testing. read the letter →

arxiv 2502.04452 v1 pith:YREPDM3M submitted 2025-02-06 astro-ph.EP

Simin Tong , Richard Alexander This is my paper · ORCID
classification astro-ph.EP
keywords protoplanetarydiscsdeadzonesdustfragmentationevolutionmagnetorotationalinstabilitycompactsyntheticobservationssize-luminosityrelation
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

The paper proposes that radially compact protoplanetary discs, common in nearby star-forming regions, can form when fragile dust grains fragment in moderately turbulent regions beyond the dead zone. By running one-dimensional dust transport and collision models and converting them into synthetic ALMA observations, it shows that the mm-sized dust disc is truncated at the dead zone edge, so the observed disc size directly traces the dead zone extent. This offers an alternative to the usual explanations (drift-dominated or born-small discs) and predicts specific observables: similar disc sizes at 1.3 and 3 mm, a sharp outer edge that can appear as a low-contrast ring, and a size–luminosity relation consistent with current samples. The mechanism works with dust porosity and with fragmentation velocities up to a few m/s, but requires both fragile dust and a sharp transition in turbulence at the dead zone edge.

What carries the argument

The load-bearing mechanism is the fragmentation-limited dust growth regime, defined by the balance between turbulent relative velocities and the fragmentation velocity through the Stokes number (St_frag = (1/3 δ_turb) (v_frag/c_s)^2). Beyond the dead zone, α_SS jumps from about $10^{-4}$ to $10^{-3}$ or higher, so the maximum grain size collapses to sub-mm sizes, preventing the growth of detectable mm dust. The dead zone edge acts as a radial gate: a sharp (but continuous) transition in α_SS produces a local steepening of the pressure gradient that accelerates radial drift of ≲ mm dust ('hitchhiking'), which further inhibits growth and creates a slight dust pile-up at the outer edge, visible as a low-contrast ring in synthetic images. The models also track the full dust size distribution with DustPy and post-process it with RADMC-3D and CASA to generate realistic synthetic observations, which are then compared to actual ALMA data. This machinery connects an analytically known growth limit (from Birnstiel et al. 2009, 2012) to a specific disc-structure feature (the dead zone) and uses it to predict an observable property (disc size).

What would settle it

A direct test would be to measure the 1.3-mm and 3-mm disc sizes of a sample of compact discs at high resolution: the model predicts that sharp-transition discs have nearly identical sizes at both wavelengths, whereas drift-dominated discs should appear smaller at longer wavelengths. A second, equally direct check is to measure the fragmentation velocity of realistic icy aggregates in the laboratory; if v_frag ≥ 5 m/s, the models themselves show that mm dust forms across the MRI-active region and the dead-zone-size correspondence breaks down.

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Extended reading notes

Core claim

The central discovery is that the fragmentation of fragile dust (fragmentation velocity ≈ 1 m/s) in moderate turbulence (alpha_SS ≈ $10^{-3}$), as expected in MRI-active regions beyond the dead zone, naturally produces radially compact millimetre-dust discs whose observed size is set by the radial extent of the dead zone. In the models, mm-sized dust cannot grow in the MRI-active region because turbulent relative velocities exceed the fragmentation threshold, so the mm-dust disc is bounded by the transition radius R_t; model discs with R_t = 20, 30, and 50 au have observed radii R_d,90% ≈ 19, 27, and 34 au at 1 Myr. The sharp drop in gas surface density at the dead zone edge accelerates inward drift of sub-mm grains ('hitchhiking'), creating a subtle outer-edge bump that appears as a low-contrast ring or shoulder at high resolution. The paper also shows that pressure bumps inside the dead zone are inefficient dust traps at radii ≲ 10 au because fragile dust fragments near the bump and the small fragments replenish the optically thick inner disc, hiding the trap; only more resilient dust (v_frag ≈ 3 m/s or above) produces a visible ring under those conditions. These synthetic morphologies resemble recent high-resolution observations of compact discs such as Sz 66 and MP Mus.

Load-bearing premise

The mechanism requires both fragile dust (fragmentation velocity around 1 m/s) and a sharp jump in turbulence at the dead zone edge; if real dead zone edges are smooth or if grains can survive collisions at speeds above a few m/s, the dead zone size would no longer set the observed disc size.

Editorial extensions

If this is right

  • If correct, the observed mm-dust size of compact discs becomes a direct tracer of the dead zone radius, turning ALMA size measurements into a probe of dead zone location and hence of disc ionization and magnetic-field structure.
  • The model predicts nearly identical disc sizes at 1.3 mm and 3 mm for sharp dead zone edges, which can be tested against multi-wavelength ALMA observations; a strong size difference would favour drift-dominated or alternative mechanisms.
  • High-resolution (≈0.02 arcsec) imaging of seemingly smooth compact discs should reveal a low-contrast ring or a change in slope at the outer edge, as seen in Sz 66 and MP Mus, providing a concrete observational signature of the hitchhiking effect.
  • Compact discs formed by this mechanism follow the observed size–luminosity relation (R_eff ∝ L_mm^0.5) and naturally yield a shallower slope at later stages, matching the trend seen in older star-forming regions such as Upper Sco.
  • The model predicts that inner pressure bumps (≲ 10 au) are hidden by the optically thick inner disc, so a faint ring in scattered light or CO may still be present even when the mm continuum looks smooth, informing the interpretation of substructure surveys.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A natural extension the paper leaves implicit is that if dead-zone radius sets disc size, then in a population of compact discs the measured sizes should correlate with stellar properties that control ionization (e.g., X-ray luminosity, cosmic-ray rate, magnetic field geometry) - a test that could be done with existing surveys.
  • The hitchhiking effect is not unique to dead zones: it should operate at any sharp outward drop in gas surface density, such as at the outer edge of a deep planetary gap or a photoevaporation front; this could be tested in substructured discs showing a weak outer ring at similar contrast.
  • The degeneracy between turbulence α_SS and fragmentation velocity v_frag highlighted in Section 5.2 implies that dust-size measurements alone cannot separately constrain these parameters; breaking the degeneracy requires independent turbulence estimates from molecular-line widths or dust scale-heights, combined with laboratory and microphysical constraints on v_frag.
  • The models indicate that dust grains in the outer disc are systematically limited to sub-mm sizes in the MRI-active region even at α_SS = 5 × 10^-4; if real discs have such low turbulence, then planetesimal formation by coagulation in the outer disc appears difficult, which may push the field toward alternative growth mechanisms such as streaming instability or gravitational collapse.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 6 minor

Summary. The paper proposes that fragmentation of fragile dust (vfrag ~ 1 m/s) in moderately turbulent MRI-active regions outside a dead zone can explain radially compact protoplanetary discs. Using 1D DustPy models with a radially varying alpha_SS profile, the authors first evolve the gas alone for 6 Myr to remove the dead-zone-edge pressure bump, then introduce dust and follow its coagulation, fragmentation, drift, and emission. They find that the mm-dust disc is truncated near the dead-zone transition radius, yielding Rd,90 values of roughly 19--38 au, wavelength-independent sizes for sharp transitions, and a size--luminosity relation broadly consistent with observed compact discs. The paper also explores planet-carved pressure bumps, porous dust, higher fragmentation velocities, and smooth versus sharp alpha transitions, and compares synthetic ALMA images with objects such as Sz 66 and MP Mus.

Significance. If the mechanism survives the model assumptions, it is significant: it gives a physical interpretation of compact discs as tracing the dead-zone radius, and it produces testable predictions (similar 1.3/3 mm sizes for sharp transitions, a weak outer-edge 'shoulder' or ring, and a degeneracy between alpha_SS and vfrag). The study is transparent and well-documented: the parameter space is clearly tabulated, no parameters are fitted to the target observations, and the synthetic observations use standard, reproducible tools (RADMC-3D and CASA). The main reservation is that the central result depends on three conditions --- a sharp alpha transition, vfrag ~ 1 m/s, and dust being absent during the gas relaxation phase --- and the paper does not fully stress-test the third condition, which is the most directly load-bearing for the title claim.

major comments (3)
  1. [Section 4.1 (initial condition)] The central claim that the mm-dust disc size is set by the dead-zone radius depends on the absence of a dust trap at the dead-zone outer edge, but that absence is imposed by construction: the gas is evolved alone for 6 Myr before dust is introduced, so the pressure bump at Rt has relaxed before any dust can encounter it. In a real disc, dust is present throughout the viscous relaxation, and Pinilla et al. (2016) --- cited in this section --- show that the bump can trap dust for several Myr; the text itself says the trap 'remains as a boost to the pressure gradient ... for another a few million years'. The model therefore selects the regime in which the trap has already dissipated, and the reported Rd,90 values at 1 Myr would likely be larger in a co-evolution run that includes dust from t = 0. I recommend adding such a run, or providing a physical justification for why late dust introduction is appropriate. The 6-Myr gas-only preconditioning also means that the quoted 1 Myr and 3 Myr times are time since dust insertion, not the physical age of the disc, which complicates the comparison to young observed discs.
  2. [Section 4.2.1 and Table 2 (Model 4)] The smooth-transition model is presented as only mildly different, but Table 2 shows a substantial quantitative change: at 1 Myr, Model 4 has Rd,90 = 37.68 au and F1.3mm = 97.71 mJy, versus 26.67 au and 19.71 mJy for the sharp-transition Model 2; even at 3 Myr the sizes are 29.93 au versus 23.77 au. Because the slow-transition profile is the case motivated by non-ideal MHD simulations (Bai et al. 2016, cited in Section 4.2.1), the size-limiting mechanism is not established for realistic dead-zone edges. The text should either quantify this sensitivity in the conclusions or explicitly restrict the claim to sharp transitions and explain why that regime is physical.
  3. [Section 5.3.2 and Fig. 14] The robustness test for the fragmentation velocity shows that mm-size dust begins to form beyond the dead zone for vfrag >= 5 m/s (Fig. 14), and the quoted M2',5 case gives Rd,90 = 29.46 au at 0.5 Myr, compared with 26.67 au for Model 2 at 1 Myr. The comparison uses different epochs, so the conclusion that 'less fragile dust does not significantly increase disc sizes' is not cleanly demonstrated. Since vfrag is a free parameter with considerable experimental uncertainty, the abstract and conclusions should state more carefully that the mechanism is contingent on vfrag ~ 1 m/s, and the analysis should specify how much dust outside Rt can be present before the observed size criterion changes.
minor comments (6)
  1. [Section 2.1] There is a typo in the text: 'Sefan-Boltzmann constant' should read 'Stefan-Boltzmann constant'.
  2. [Data Availability] The software list contains 'DustyPyLib'; the correct name used elsewhere in the paper is 'DustPyLib'.
  3. [Section 5.1] The citation '(Anania et al, submitted)' appears in the text but has no entry in the reference list; please add the reference or remove the citation.
  4. [Table 4] Models M2',3 through M2',5 are listed in Table 4 without any resulting quantities; since the note explains why, it would be helpful to point the reader explicitly to Fig. 14 as the quantitative output for these runs.
  5. [Section 5.3.2] The M2' runs with high vfrag are quoted at 0.5 Myr, while all other size measurements in Table 2 are at 1 and 3 Myr; please state the reason for this different evaluation time in the text.
  6. [Appendix B] The caption for Figure B1 says 'orange and green lines', but the text and legend identify the two profiles as 'noise-free' and 'thermal noise'; please make the colour and label terminology consistent.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: the compact-disc size is a simulated output from independently specified physical inputs, not a refit of the target observations.

full rationale

The paper's central claim is that mm-dust fragmentation in the MRI-active region sets the observed disc size to the dead-zone transition radius. The inputs (dead-zone profile Eq. 17 with specified alpha_DZ, alpha_MRI, Rt, and w; fragmentation velocity vfrag=1 m/s from laboratory experiments; alpha values from ALMA constraints) are all fixed before the DustPy runs, and the disc radii Rd,68 and Rd,90 are measured from synthetic observations generated after the evolution. No parameter is fitted to the observed compact-disc sizes or to the size-luminosity relation; the comparison to Long et al. (2019) and Shi et al. (2024) is a post-hoc overlay without tuning. The relation between Rt and Rd,90 is an emergent consequence of the prescribed alpha transition combined with the fragmentation-limited growth expressions in Eqs. (11)-(12), so the output is not identical to the input by definition. The 6-Myr gas-only relaxation before dust is introduced is a modeling choice that could affect robustness, but it is not a circular reduction: the relaxed gas profile is itself recomputed from the same viscous equation and is not defined in terms of the predicted dust size. The only self-citation (Tong et al. 2024) supports a secondary discussion point about long-term gas spreading and is not load-bearing for the main result. Thus the derivation chain is self-contained against external benchmarks and no circular step is exhibited.

Assumptions & free parameters 5 free parameters · 7 assumptions · 0 invented entities

The central claim depends on the dead-zone prescription (Eq. 17) with a sharp alpha transition, on vfrag=1 m/s, and on standard 1-D simplifications (no MHD winds, no back-reaction, no porosity treatment in the default models). These assumptions are acknowledged in Section 5.5 but are not tested within the paper.

free parameters (5)
  • Fragmentation velocity v_frag = 1 m/s (canonical; 3, 5, 7 m/s explored)
    Sets the maximum grain size in the MRI-active region; low value is required for the compact-disc mechanism (Section 3, 5.3.2).
  • Dead-zone transition radius R_t = 30 au canonical; 20 and 50 au explored
    The claim is that observed disc size tracks this radius; chosen from prior numerical dead-zone models, not derived from the model (Section 4.2.2).
  • Transition sharpness parameter w = 30 for sharp, slow profile in Model 4
    Controls whether 'hitchhiking' and size-limiting occur; smooth transitions produce larger discs (Section 4.2.1).
  • MRI-active turbulence alpha_SS,MRI = 1e-3 canonical; 1e-2 and 5e-4 explored
    Determines whether mm dust can grow in the outer disc; within observed range (Section 4.2.1).
  • Dead-zone turbulence alpha_SS,DZ = 1e-4
    Controls dust retention and growth inside the dead zone; chosen as a typical hydrodynamic value.
assumptions (7)
  • standard math Smoluchowski coagulation-fragmentation and advection-diffusion equations for dust (Section 2.2)
    Standard dust evolution framework used by DustPy; not questioned.
  • domain assumption Alpha-viscosity prescription for gas evolution (Shakura-Sunyaev, Eq. 1)
    Assumes turbulence can be parametrized by alpha_SS and that gas evolves viscously; standard but not derived in this work.
  • domain assumption Two-zone dead zone profile with transition function (Eq. 17)
    The sharpness and location of the alpha transition are imposed, not computed from ionization chemistry.
  • domain assumption Constant fragmentation velocity across the entire disc (Section 3)
    vfrag may vary with radius and composition; acknowledged as a limitation in Section 5.5.
  • domain assumption No dust back-reaction on the gas (Section 5.5)
    Assumed negligible except where traps concentrate dust, where it may matter.
  • domain assumption No MHD winds (Section 5.5)
    Winds can add inward advection and mass loss, altering dust transport.
  • domain assumption Vertically averaged 1-D model with Gaussian vertical dust distribution (Eq. 10)
    Vertical structure is imposed analytically and used only for radiative transfer.

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Cite this review

Pith. "Pith review of Compact protoplanetary discs can be produced by dead zones." pith.science (2026). https://pith.science/paper/YREPDM3M

@misc{pith2026250204452,
  author       = {Pith},
  title        = {Pith review of: Compact protoplanetary discs can be produced by dead zones},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/YREPDM3M}},
  note         = {Machine review of arXiv:2502.04452}
}
read the original abstract

Radially compact protoplanetary discs (<=50 au) are ubiquitous in nearby star-forming regions. Multiple mechanisms have been invoked to interpret various compact discs. In this paper, we propose that fragmentation of fragile dust grains in moderate turbulence, as expected beyond the dead zone, provides an effective alternative mechanism to form compact discs which are consistent with current observations. We run 1-D dust transport and collision models with DustPy and generate synthetic observations, and find that discs formed by this mechanism have sizes determined by the extent of their dead zones. Accounting for dust porosity, and considering less fragile dust, do not change disc sizes significantly. The smooth dust morphology can be altered only when pressure bumps are present in the dead zone. However, when present at small radii (<=10 au), pressure bumps cannot effectively trap dust. Dust in these bumps fragments and replenishes the inner discs, effectively hiding dust traps in the optically thick inner disc from observations. We note a striking resemblance in the radial intensity profile between our synthetic observations and some recent high-resolution observations of compact discs. We discuss how such observations can inform our understanding of the underlying disc physics.

Figures

Figures reproduced from arXiv: 2502.04452 by the authors.

Figure 1
Figure 1. Evolution of the gas surface density and the pressure gradient (𝑑 ln 𝑃/𝑑 ln 𝑅) when a dead zone model is applied to a self-similar initial gas disc. The left panels show how the two quantities evolve without relax￾ation; the right panels illustrate the initial gas surface density and its pressure gradient adopted into our DustPy models, mimicking a disc where the dead zone develops gradually. 10 20 30 40 50 R [AU] 2… view at source ↗
Figure 2
Figure 2. [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. The dust distributions and transition profiles for Models 1-4 (from left to right) at 1 Myr. Upper panels: dust density distributions as a function of radius. Middle panels: integrated surface densities of 1-2 𝜇m (purple), 1-2 mm (orange) and 2.5-3.5 mm (yellow) dust. Lower panels: the transition of 𝛼SS from dead zones (𝑟 < 30 au) to MRI-active zones (𝑟 > 30 au). In the upper panels the green and blue solid lines sh… view at source ↗
Figures from the paper (11 more)
Figure 4
Figure 4. Figure 4: Dust distributions plotted as in [PITH_FULL_IMAGE:figures/full_fig_p007_4.png]
Figure 5
Figure 5. Figure 5: Evolution of the dust total mass (left panels); the observed disc radii 𝑅d,90% at 1 Myr (middle panels); and the measured continuum fluxes 𝐹1.3mm at 1 and 3 Myr (right panels) for Models 1-3, 5 and 6. The upper panels show the results from models with different values …
Figure 6
Figure 6. Figure 6: Dust distributions plotted as in [PITH_FULL_IMAGE:figures/full_fig_p009_6.png]
Figure 7
Figure 7. Figure 7: The azimuthally-averaged radial intensity profile extracted from the synthetic observation of Model 7. The beam size is 0. ′′02 and the integration time is 30 mins. The grey shade indicates the root-mean-square noise 𝜎 measured from noisy images, and the grey dotted li…
Figure 8
Figure 8. Figure 8: Upper left: the measured dust disc size 𝑅𝑑,90% at 𝜆 = 1.3 mm for models without (𝑅𝑔 = 0 au, Model 2) and with (𝑅𝑔 > 0 au, Models 7-11) traps at 𝑡 = 1 Myr. Upper right: The measured continuum flux at 1.3 mm for models with and without traps, plotted at 1 Myr (filled gre…
Figure 9
Figure 9. Figure 9: ALMA synthetic observations at 𝜆 = 1.3 mm for models in [PITH_FULL_IMAGE:figures/full_fig_p011_9.png]
Figure 11
Figure 11. Figure 11: The synthetic observations at 𝜆 = 1.3 mm for Model 7 (𝑣frag = 1 m s−1 , left) and modified Model 7 (M7′ ,𝑣frag = 3 m s−1 , right), at𝑡 = 1 Myr. The beam is denoted as an ellipse in the lower left corner of the left panel. Model a Model b 30 0 -30 R [au] 30 0 -30 R [au…
Figure 10
Figure 10. Figure 10: The size-luminosity relation for models from Section 4 (orange open circles are for 𝑅d.90% and orange filled circles are for 𝑅d.68%) and for compact discs (≲ 50 au) observed in ALMA Band 6 (Long et al. 2019; Shi et al. 2024) (green dots). The grey line shows the propo…
Figure 12
Figure 12. Figure 12: The synthetic ALMA observations at 𝜆 = 1.3 mm for Models a-d in Section 5.2, at 𝑡 = 1 Myr. The beam size is plotted as an ellipse in the lower left corner. MNRAS 000, 1–17 (2024) [PITH_FULL_IMAGE:figures/full_fig_p012_12.png]
Figure 13
Figure 13. Figure 13: The integrated surface density of 1-2 𝜇m (purple) and 1-2 mm (orange) dust for Model 2 with compact dust (f=1, solid lines), and for mod￾ified Model 2 with porous dust (M2′ ,1: f=0.1, dashed lines; M2′ , 2: f=0.05, dotted lines). 1 10 100 R [au] 10 5 10 3 10 1 10 1 d …
Figure 14
Figure 14. Figure 14: The integrated surface density of 0.1-1 cm dust for (modified) Model 2 when the fragmentation velocity is set to be 1, 3, 5, 7 m s−1 at 0.5 Myr (darker colours for higher velocities). Filled circles with corre￾sponding colours show the radial extent of disc sizes cut …

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Reference graph

Works this paper leans on

156 extracted references · 5 canonical work pages · cited by 1 Pith paper

  1. [1]

    write newline

    " write newline "" before.all 'output.state := FUNCTION fin.entry write newline FUNCTION new.block output.state before.all = 'skip after.block 'output.state := if FUNCTION new.sentence output.state after.block = 'skip output.state before.all = 'skip after.sentence 'output.state := if if FUNCTION not #0 #1 if FUNCTION and 'skip pop #0 if FUNCTION or pop #1...

  2. [2]

    E., Cridland A

    Alessi M., Pudritz R. E., Cridland A. J., 2020, @doi [ ] 10.1093/mnras/staa308 , https://ui.adsabs.harvard.edu/abs/2020MNRAS.493.1013A 493, 1013

    doi:10.1093/mnras/staa308 2020

  3. [3]

    R., Williams J

    Anderson A. R., Williams J. P., van der Marel N., Law C. J., Ricci L., Tobin J. J., Tong S., 2022, @doi [ ] 10.3847/1538-4357/ac8ff0 , https://ui.adsabs.harvard.edu/abs/2022ApJ...938...55A 938, 55

    work page doi:10.3847/1538-4357/ac8ff0 2022

  4. [4]

    M., Terrell M., Tripathi A., Ansdell M., Williams J

    Andrews S. M., Terrell M., Tripathi A., Ansdell M., Williams J. P., Wilner D. J., 2018, @doi [ ] 10.3847/1538-4357/aadd9f , https://ui.adsabs.harvard.edu/abs/2018ApJ...865..157A 865, 157

    doi:10.3847/1538-4357/aadd9f 2018

  5. [5]

    Ansdell M., et al., 2016, @doi [ ] 10.3847/0004-637X/828/1/46 , https://ui.adsabs.harvard.edu/abs/2016ApJ...828...46A 828, 46

    doi:10.3847/0004-637x/828/1/46 2016

  6. [6]

    P., Manara C

    Ansdell M., Williams J. P., Manara C. F., Miotello A., Facchini S., van der Marel N., Testi L., van Dishoeck E. F., 2017, @doi [ ] 10.3847/1538-3881/aa69c0 , https://ui.adsabs.harvard.edu/abs/2017AJ....153..240A 153, 240

    doi:10.3847/1538-3881/aa69c0 2017

  7. [7]

    Arlt R., Urpin V., 2004, @doi [ ] 10.1051/0004-6361:20035896 , https://ui.adsabs.harvard.edu/abs/2004A&A...426..755A 426, 755

    doi:10.1051/0004-6361:20035896 2004

  8. [8]

    arXiv:2501.03920

    Bacciotti F., et al., 2025, arXiv e-prints, https://ui.adsabs.harvard.edu/abs/2025arXiv250103920B p. arXiv:2501.03920

    arXiv 2025

Show all 156 references
  1. [9]

    Bai X.-N., 2015, @doi [ ] 10.1088/0004-637X/798/2/84 , https://ui.adsabs.harvard.edu/abs/2015ApJ...798...84B 798, 84

    2015 doi

  2. [10]

    M., 2013, @doi [ ] 10.1088/0004-637X/769/1/76 , https://ui.adsabs.harvard.edu/abs/2013ApJ...769...76B 769, 76

    Bai X.-N., Stone J. M., 2013, @doi [ ] 10.1088/0004-637X/769/1/76 , https://ui.adsabs.harvard.edu/abs/2013ApJ...769...76B 769, 76

    2013 doi

  3. [11]

    Bai X.-N., Ye J., Goodman J., Yuan F., 2016, @doi [ ] 10.3847/0004-637X/818/2/152 , https://ui.adsabs.harvard.edu/abs/2016ApJ...818..152B 818, 152

    2016 doi

  4. [12]

    A., Hawley J

    Balbus S. A., Hawley J. F., 1991, @doi [ ] 10.1086/170270 , 376, 214

    1991 doi

  5. [13]

    Banzatti A., et al., 2023, @doi [ ] 10.3847/2041-8213/acf5ec , https://ui.adsabs.harvard.edu/abs/2023ApJ...957L..22B 957, L22

    2023 doi

  6. [14]

    A., Carpenter J

    Barenfeld S. A., Carpenter J. M., Ricci L., Isella A., 2016, @doi [ ] 10.3847/0004-637X/827/2/142 , https://ui.adsabs.harvard.edu/abs/2016ApJ...827..142B 827, 142

    2016 doi

  7. [15]

    B \'e thune W., Lesur G., Ferreira J., 2017, @doi [ ] 10.1051/0004-6361/201630056 , https://ui.adsabs.harvard.edu/abs/2017A&A...600A..75B 600, A75

    2017 doi

  8. [16]

    P., Brauer F., 2009, @doi [ ] 10.1051/0004-6361/200912452 , https://ui.adsabs.harvard.edu/abs/2009A&A...503L...5B 503, L5

    Birnstiel T., Dullemond C. P., Brauer F., 2009, @doi [ ] 10.1051/0004-6361/200912452 , https://ui.adsabs.harvard.edu/abs/2009A&A...503L...5B 503, L5

    2009 doi

  9. [17]

    Birnstiel T., Dullemond C., Brauer F., 2010, @doi [ ] 10.1051/0004-6361/200913731 , 513, A79

    2010 doi

  10. [18]

    Birnstiel T., Klahr H., Ercolano B., 2012, @doi [ ] 10.1051/0004-6361/201118136 , https://ui.adsabs.harvard.edu/abs/2012A&A...539A.148B 539, A148

    2012 doi

  11. [19]

    Birnstiel T., et al., 2018, @doi [ ] 10.3847/2041-8213/aaf743 , https://ui.adsabs.harvard.edu/abs/2018ApJ...869L..45B 869, L45

    2018 doi

  12. [20]

    D., Payne D

    Blandford R. D., Payne D. G., 1982, @doi [ ] 10.1093/mnras/199.4.883 , https://ui.adsabs.harvard.edu/abs/1982MNRAS.199..883B 199, 883

    1982 doi

  13. [21]

    Blum J., Wurm G., 2008, @doi [ ] 10.1146/annurev.astro.46.060407.145152 , https://ui.adsabs.harvard.edu/abs/2008ARA&A..46...21B 46, 21

    2008

  14. [22]

    CASA Team et al., 2022, @doi [ ] 10.1088/1538-3873/ac9642 , https://ui.adsabs.harvard.edu/abs/2022PASP..134k4501C 134, 114501

    2022 doi

  15. [23]

    Cazzoletti P., et al., 2019, @doi [ ] 10.1051/0004-6361/201935273 , https://ui.adsabs.harvard.edu/abs/2019A&A...626A..11C 626, A11

    2019 doi

  16. [24]

    J., Cuzzi J

    Ciesla F. J., Cuzzi J. N., 2006, @doi [ ] 10.1016/j.icarus.2005.11.009 , https://ui.adsabs.harvard.edu/abs/2006Icar..181..178C 181, 178

    2006 doi

  17. [25]

    A., et al., 2019, @doi [ ] 10.1093/mnras/sty2653 , 482, 698

    Cieza L. A., et al., 2019, @doi [ ] 10.1093/mnras/sty2653 , 482, 698

    2019 doi

  18. [26]

    G., et al., 2017, @doi [ ] 10.3847/1538-4357/aa97e2 , https://ui.adsabs.harvard.edu/abs/2017ApJ...851...83C 851, 83

    Cox E. G., et al., 2017, @doi [ ] 10.3847/1538-4357/aa97e2 , https://ui.adsabs.harvard.edu/abs/2017ApJ...851...83C 851, 83

    2017 doi

  19. [27]

    N., Okuzumi S., Flock M., Pinilla P., Dzyurkevich N., 2022, @doi [ ] 10.1051/0004-6361/202141689 , https://ui.adsabs.harvard.edu/abs/2022A&A...658A..97D 658, A97

    Delage T. N., Okuzumi S., Flock M., Pinilla P., Dzyurkevich N., 2022, @doi [ ] 10.1051/0004-6361/202141689 , https://ui.adsabs.harvard.edu/abs/2022A&A...658A..97D 658, A97

    2022 doi

  20. [28]

    N., G \'a rate M., Okuzumi S., Yang C.-C., Pinilla P., Flock M., Stammler S

    Delage T. N., G \'a rate M., Okuzumi S., Yang C.-C., Pinilla P., Flock M., Stammler S. M., Birnstiel T., 2023, @doi [ ] 10.1051/0004-6361/202244731 , https://ui.adsabs.harvard.edu/abs/2023A&A...674A.190D 674, A190

    2023 doi

  21. [29]

    M., 2024, @doi [ ] 10.1051/0004-6361/202450328 , https://ui.adsabs.harvard.edu/abs/2024A&A...688A..81D 688, A81

    Delussu L., Birnstiel T., Miotello A., Pinilla P., Rosotti G., Andrews S. M., 2024, @doi [ ] 10.1051/0004-6361/202450328 , https://ui.adsabs.harvard.edu/abs/2024A&A...688A..81D 688, A81

    2024 doi

  22. [30]

    Dipierro G., Laibe G., Alexander R., Hutchison M., 2018, @doi [ ] 10.1093/mnras/sty1701 , 479, 4187

    2018 doi

  23. [31]

    Doi K., Kataoka A., 2021, @doi [ ] 10.3847/1538-4357/abe5a6 , https://ui.adsabs.harvard.edu/abs/2021ApJ...912..164D 912, 164

    2021 doi

  24. [32]

    Dong R., et al., 2018, @doi [ ] 10.3847/1538-4357/aac6cb , https://ui.adsabs.harvard.edu/abs/2018ApJ...860..124D 860, 124

    2018 doi

  25. [33]

    T., 2003, @doi [ ] 10.1146/annurev.astro.41.011802.094840 , https://ui.adsabs.harvard.edu/abs/2003ARA&A..41..241D 41, 241

    Draine B. T., 2003, @doi [ ] 10.1146/annurev.astro.41.011802.094840 , https://ui.adsabs.harvard.edu/abs/2003ARA&A..41..241D 41, 241

    2003 arXiv

  26. [34]

    P., 2014, @doi [ ] 10.1051/0004-6361/201423708 , https://ui.adsabs.harvard.edu/abs/2014A&A...567A..38D 567, A38

    Dr a \.z kowska J., Windmark F., Dullemond C. P., 2014, @doi [ ] 10.1051/0004-6361/201423708 , https://ui.adsabs.harvard.edu/abs/2014A&A...567A..38D 567, A38

    2014 doi

  27. [36]

    Dullemond C. P., Juhasz A., Pohl A., Sereshti F., Shetty R., Peters T., Commercon B., Flock M., 2012, RADMC-3D: A multi-purpose radiative transfer tool , Astrophysics Source Code Library, record ascl:1202.015

    2012

  28. [37]

    P., et al., 2018, @doi [ ] 10.3847/2041-8213/aaf742 , https://ui.adsabs.harvard.edu/abs/2018ApJ...869L..46D 869, L46

    Dullemond C. P., et al., 2018, @doi [ ] 10.3847/2041-8213/aaf742 , https://ui.adsabs.harvard.edu/abs/2018ApJ...869L..46D 869, L46

    2018 doi

  29. [38]

    J., Henning T., Kley W., 2013, @doi [ ] 10.1088/0004-637X/765/2/114 , https://ui.adsabs.harvard.edu/abs/2013ApJ...765..114D 765, 114

    Dzyurkevich N., Turner N. J., Henning T., Kley W., 2013, @doi [ ] 10.1088/0004-637X/765/2/114 , https://ui.adsabs.harvard.edu/abs/2013ApJ...765..114D 765, 114

    2013 doi

  30. [39]

    Eisner J., et al., 2018, @doi [ ] 10.3847/1538-4357/aac3e2 , 860, 77

    2018 doi

  31. [40]

    F., 2017, @doi [ ] 10.1051/0004-6361/201630329 , https://ui.adsabs.harvard.edu/abs/2017A&A...605A..16F 605, A16

    Facchini S., Birnstiel T., Bruderer S., van Dishoeck E. F., 2017, @doi [ ] 10.1051/0004-6361/201630329 , https://ui.adsabs.harvard.edu/abs/2017A&A...605A..16F 605, A16

    2017 doi

  32. [41]

    Facchini S., et al., 2019, @doi [ ] 10.1051/0004-6361/201935496 , 626, L2

    2019 doi

  33. [42]

    Flaherty K., et al., 2020, @doi [ ] 10.3847/1538-4357/ab8cc5 , 895, 109

    2020 doi

  34. [43]

    Flaherty K., et al., 2024, @doi [ ] 10.1093/mnras/stae1480 , https://ui.adsabs.harvard.edu/abs/2024MNRAS.532..363F 532, 363

    2024 doi

  35. [44]

    Flock M., Fromang S., Turner N., Benisty M., 2016, @doi [ ] 10.3847/0004-637X/827/2/144 , 827, 144

    2016 doi

  36. [45]

    J., Mulders G

    Flock M., Turner N. J., Mulders G. D., Hasegawa Y., Nelson R. P., Bitsch B., 2019, @doi [ ] 10.1051/0004-6361/201935806 , https://ui.adsabs.harvard.edu/abs/2019A&A...630A.147F 630, A147

    2019 doi

  37. [46]

    F., 1996, @doi [ ] 10.1086/176735 , https://ui.adsabs.harvard.edu/abs/1996ApJ...457..355G 457, 355

    Gammie C. F., 1996, @doi [ ] 10.1086/176735 , https://ui.adsabs.harvard.edu/abs/1996ApJ...457..355G 457, 355

    1996 doi

  38. [47]

    M., 2020, @doi [ ] 10.1051/0004-6361/201936067 , https://ui.adsabs.harvard.edu/abs/2020A&A...635A.149G 635, A149

    G \'a rate M., Birnstiel T., Dr a \.z kowska J., Stammler S. M., 2020, @doi [ ] 10.1051/0004-6361/201936067 , https://ui.adsabs.harvard.edu/abs/2020A&A...635A.149G 635, A149

    2020 doi

  39. [48]

    G \'a rate M., et al., 2021, @doi [ ] 10.1051/0004-6361/202141444 , https://ui.adsabs.harvard.edu/abs/2021A&A...655A..18G 655, A18

    2021 doi

  40. [49]

    Gundlach B., Blum J., 2015, @doi [ ] 10.1088/0004-637X/798/1/34 , https://ui.adsabs.harvard.edu/abs/2015ApJ...798...34G 798, 34

    2015 doi

  41. [50]

    R., et al., 2020, @doi [ ] 10.1038/s41586-020-2649-2 , https://ui.adsabs.harvard.edu/abs/2020Natur.585..357H 585, 357

    Harris C. R., et al., 2020, @doi [ ] 10.1038/s41586-020-2649-2 , https://ui.adsabs.harvard.edu/abs/2020Natur.585..357H 585, 357

    2020 doi

  42. [51]

    F., Gammie C

    Hawley J. F., Gammie C. F., Balbus S. A., 1995, @doi [ ] 10.1086/175311 , 440, 742

    1995 doi

  43. [52]

    Hendler N., Pascucci I., Pinilla P., Tazzari M., Carpenter J., Malhotra R., Testi L., 2020, @doi [ ] 10.3847/1538-4357/ab70ba , https://ui.adsabs.harvard.edu/abs/2020ApJ...895..126H 895, 126

    2020 doi

  44. [53]

    Henning T., Stognienko R., 1996, , https://ui.adsabs.harvard.edu/abs/1996A&A...311..291H 311, 291

    1996

  45. [54]

    Huang J., et al., 2018, @doi [ ] 10.3847/2041-8213/aaf740 , 869, L42

    2018 doi

  46. [55]

    arXiv:2410.03823

    Huang J., Ansdell M., Birnstiel T., Czekala I., Long F., Williams J., Zhang S., Zhu Z., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2410.03823 , https://ui.adsabs.harvard.edu/abs/2024arXiv241003823H p. arXiv:2410.03823

    2024 doi arXiv

  47. [56]

    D., 2007, @doi [Computing in Science & Engineering] 10.1109/MCSE.2007.55 , 9, 90

    Hunter J. D., 2007, @doi [Computing in Science & Engineering] 10.1109/MCSE.2007.55 , 9, 90

    2007 doi

  48. [57]

    D., Walsh C., Jennings J., Booth R

    Ilee J. D., Walsh C., Jennings J., Booth R. A., Rosotti G. P., Teague R., Tsukagoshi T., Nomura H., 2022, @doi [ ] 10.1093/mnrasl/slac048 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.515L..23I 515, L23

    2022 doi

  49. [58]

    J., Booth R

    Jennings J., Tazzari M., Clarke C. J., Booth R. A., Rosotti G. P., 2022, @doi [ ] 10.1093/mnras/stac1770 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.514.6053J 514, 6053

    2022 doi

  50. [59]

    M., Carrasco-Gonz \'a lez C., 2024, @doi [ ] 10.1051/0004-6361/202348271 , https://ui.adsabs.harvard.edu/abs/2024A&A...682A..32J 682, A32

    Jiang H., Mac \' as E., Guerra-Alvarado O. M., Carrasco-Gonz \'a lez C., 2024, @doi [ ] 10.1051/0004-6361/202348271 , https://ui.adsabs.harvard.edu/abs/2024A&A...682A..32J 682, A32

    2024 doi

  51. [60]

    D., Ueda T., Muto T., Okuzumi S., 2017, @doi [ ] 10.3847/1538-4357/aa7ca1 , https://ui.adsabs.harvard.edu/abs/2017ApJ...844..142K 844, 142

    Kanagawa K. D., Ueda T., Muto T., Okuzumi S., 2017, @doi [ ] 10.3847/1538-4357/aa7ca1 , https://ui.adsabs.harvard.edu/abs/2017ApJ...844..142K 844, 142

    2017 doi

  52. [61]

    D., Tanaka H., Szuszkiewicz E., 2018, @doi [ ] 10.3847/1538-4357/aac8d9 , https://ui.adsabs.harvard.edu/abs/2018ApJ...861..140K 861, 140

    Kanagawa K. D., Tanaka H., Szuszkiewicz E., 2018, @doi [ ] 10.3847/1538-4357/aac8d9 , https://ui.adsabs.harvard.edu/abs/2018ApJ...861..140K 861, 140

    2018 doi

  53. [62]

    P., 2012, @doi [ ] 10.1146/annurev-astro-081811-125523 , https://ui.adsabs.harvard.edu/abs/2012ARA&A..50..211K 50, 211

    Kley W., Nelson R. P., 2012, @doi [ ] 10.1146/annurev-astro-081811-125523 , https://ui.adsabs.harvard.edu/abs/2012ARA&A..50..211K 50, 211

    2012 doi

  54. [63]

    IOS Press, pp 87--90, https://eprints.soton.ac.uk/403913/

    Kluyver T., et al., 2016, in Loizides F., Scmidt B., eds, Positioning and Power in Academic Publishing: Players, Agents and Agendas. IOS Press, pp 87--90, https://eprints.soton.ac.uk/403913/

    2016

  55. [64]

    W., Dominik C., Tielens A

    Krijt S., Ormel C. W., Dominik C., Tielens A. G. G. M., 2015, @doi [ ] 10.1051/0004-6361/201425222 , https://ui.adsabs.harvard.edu/abs/2015A&A...574A..83K 574, A83

    2015 doi

  56. [65]

    S., Haugb lle T., 2023, @doi [European Physical Journal Plus] 10.1140/epjp/s13360-023-03880-y , https://ui.adsabs.harvard.edu/abs/2023EPJP..138..272K 138, 272

    Kuffmeier M., Jensen S. S., Haugb lle T., 2023, @doi [European Physical Journal Plus] 10.1140/epjp/s13360-023-03880-y , https://ui.adsabs.harvard.edu/abs/2023EPJP..138..272K 138, 272

    2023 doi

  57. [66]

    Kurtovic N., et al., 2021, @doi [ ] 10.1051/0004-6361/202038983 , 645, A139

    2021 doi

  58. [67]

    Kuznetsova A., Bae J., Hartmann L., Mac Low M.-M., 2022, The Astrophysical Journal, 928, 92

    2022

  59. [68]

    Lee C.-F., Tabone B., Cabrit S., Codella C., Podio L., Ferreira J., Jacquemin-Ide J., 2021, @doi [ ] 10.3847/2041-8213/abda38 , https://ui.adsabs.harvard.edu/abs/2021ApJ...907L..41L 907, L41

    2021 doi

  60. [69]

    534, Protostars and Planets VII

    Lesur G., et al., 2023, in Inutsuka S., Aikawa Y., Muto T., Tomida K., Tamura M., eds, Astronomical Society of the Pacific Conference Series Vol. 534, Protostars and Planets VII. p. 465 ( @eprint arXiv 2203.09821 ), @doi 10.48550/arXiv.2203.09821

    2023 doi arXiv

  61. [70]

    M., Lovelace R

    Li H., Finn J. M., Lovelace R. V. E., Colgate S. A., 2000, @doi [ ] 10.1086/308693 , https://ui.adsabs.harvard.edu/abs/2000ApJ...533.1023L 533, 1023

    2000 doi

  62. [71]

    Long F., et al., 2019, @doi [ ] 10.3847/1538-4357/ab2d2d , https://ui.adsabs.harvard.edu/abs/2019ApJ...882...49L 882, 49

    2019 doi

  63. [72]

    Louvet F., Dougados C., Cabrit S., Mardones D., M \' e nard F., Tabone B., Pinte C., Dent W., 2018, @doi [ ] 10.1051/0004-6361/201731733 , 618, A120

    2018 doi

  64. [73]

    E., 1974, @doi [ ] 10.1093/mnras/168.3.603 , https://ui.adsabs.harvard.edu/abs/1974MNRAS.168..603L 168, 603

    Lynden-Bell D., Pringle J. E., 1974, @doi [ ] 10.1093/mnras/168.3.603 , https://ui.adsabs.harvard.edu/abs/1974MNRAS.168..603L 168, 603

    1974 doi

  65. [74]

    Lyra W., Johansen A., Zsom A., Klahr H., Piskunov N., 2009, @doi [ ] 10.1051/0004-6361/200811265 , https://ui.adsabs.harvard.edu/abs/2009A&A...497..869L 497, 869

    2009 doi

  66. [75]

    F., et al., 2019, @doi [ ] 10.1051/0004-6361/201935964 , https://ui.adsabs.harvard.edu/abs/2019A&A...628A..95M 628, A95

    Manara C. F., et al., 2019, @doi [ ] 10.1051/0004-6361/201935964 , https://ui.adsabs.harvard.edu/abs/2019A&A...628A..95M 628, A95

    2019 doi

  67. [76]

    S., Rumpl W., Nordsieck K

    Mathis J. S., Rumpl W., Nordsieck K. H., 1977, @doi [ ] 10.1086/155591 , https://ui.adsabs.harvard.edu/abs/1977ApJ...217..425M 217, 425

    1977 doi

  68. [77]

    J., et al., 2024, @doi [ ] 10.1051/0004-6361/202451166 , https://ui.adsabs.harvard.edu/abs/2024A&A...689L...5M 689, L5

    Maureira M. J., et al., 2024, @doi [ ] 10.1051/0004-6361/202451166 , https://ui.adsabs.harvard.edu/abs/2024A&A...689L...5M 689, L5

    2024 doi

  69. [78]

    J., 2024, @doi [ ] 10.1051/0004-6361/202449719 , https://ui.adsabs.harvard.edu/abs/2024A&A...688A..31M 688, A31

    Michoulier S., Gonzalez J.-F., Price D. J., 2024, @doi [ ] 10.1051/0004-6361/202449719 , https://ui.adsabs.harvard.edu/abs/2024A&A...688A..31M 688, A31

    2024 doi

  70. [79]

    M., et al., 2024, @doi [ ] 10.1051/0004-6361/202347135 , https://ui.adsabs.harvard.edu/abs/2024A&A...682A..55M 682, A55

    Miley J. M., et al., 2024, @doi [ ] 10.1051/0004-6361/202347135 , https://ui.adsabs.harvard.edu/abs/2024A&A...682A..55M 682, A55

    2024 doi

  71. [80]

    F., Williams J

    Miotello A., Rosotti G., Ansdell M., Facchini S., Manara C. F., Williams J. P., Bruderer S., 2021, @doi [ ] 10.1051/0004-6361/202140550 , https://ui.adsabs.harvard.edu/abs/2021A&A...651A..48M 651, A48

    2021 doi

  72. [81]

    Morishima R., 2012, @doi [ ] 10.1111/j.1365-2966.2011.19940.x , https://ui.adsabs.harvard.edu/abs/2012MNRAS.420.2851M 420, 2851

    2012

  73. [82]

    Musiolik G., Wurm G., 2019, @doi [ ] 10.3847/1538-4357/ab0428 , https://ui.adsabs.harvard.edu/abs/2019ApJ...873...58M 873, 58

    2019 doi

  74. [83]

    Nakagawa Y., Sekiya M., Hayashi C., 1986, @doi [ ] 10.1016/0019-1035(86)90121-1 , https://ui.adsabs.harvard.edu/abs/1986Icar...67..375N 67, 375

    1986 doi

  75. [84]

    D., Rosotti G

    Nazari P., Sellek A. D., Rosotti G. P., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2410.09042 , https://ui.adsabs.harvard.edu/abs/2024arXiv241009042N p. arXiv:2410.09042

    2024 doi arXiv

  76. [85]

    P., Gressel O., Umurhan O

    Nelson R. P., Gressel O., Umurhan O. M., 2013, @doi [ ] 10.1093/mnras/stt1475 , 435, 2610

    2013 doi

  77. [86]

    Ohashi S., Kataoka A., 2019, @doi [ ] 10.3847/1538-4357/ab5107 , https://ui.adsabs.harvard.edu/abs/2019ApJ...886..103O 886, 103

    2019 doi

  78. [87]

    Okuzumi S., Momose M., Sirono S.-i., Kobayashi H., Tanaka H., 2016, @doi [ ] 10.3847/0004-637X/821/2/82 , https://ui.adsabs.harvard.edu/abs/2016ApJ...821...82O 821, 82

    2016 doi

  79. [88]

    W., Cuzzi J

    Ormel C. W., Cuzzi J. N., 2007, @doi [ ] 10.1051/0004-6361:20066899 , https://ui.adsabs.harvard.edu/abs/2007A&A...466..413O 466, 413

    2007 doi

  80. [89]

    P., Bally J., Eisner J., Goddi C., Plambeck R., Wright M., 2021, @doi [ ] 10.3847/1538-4357/ac29c2 , 923, 221

    Otter J., Ginsburg A., Ballering N. P., Bally J., Eisner J., Goddi C., Plambeck R., Wright M., 2021, @doi [ ] 10.3847/1538-4357/ac29c2 , 923, 221

    2021 doi

  81. [90]

    Pascucci I., et al., 2016, @doi [ ] 10.3847/0004-637X/831/2/125 , 831, 125

    2016 doi

  82. [91]

    J., Mamajek E

    Pecaut M. J., Mamajek E. E., Bubar E. J., 2012, @doi [ ] 10.1088/0004-637X/746/2/154 , https://ui.adsabs.harvard.edu/abs/2012ApJ...746..154P 746, 154

    2012 doi

  83. [92]

    Pi \'e tu V., Guilloteau S., Di Folco E., Dutrey A., Boehler Y., 2014, @doi [ ] 10.1051/0004-6361/201322388 , https://ui.adsabs.harvard.edu/abs/2014A&A...564A..95P 564, A95

    2014 doi

  84. [93]

    P., Uribe A

    Pinilla P., Birnstiel T., Ricci L., Dullemond C. P., Uribe A. L., Testi L., Natta A., 2012, @doi [ ] 10.1051/0004-6361/201118204 , https://ui.adsabs.harvard.edu/abs/2012A&A...538A.114P 538, A114

    2012 doi

  85. [94]

    Pinilla P., Flock M., Ovelar M. d. J., Birnstiel T., 2016, @doi [ ] 10.1051/0004-6361/201628441 , https://ui.adsabs.harvard.edu/abs/2016A&A...596A..81P 596, A81

    2016 doi

  86. [95]

    Pinilla P., et al., 2017a, @doi [ ] 10.3847/1538-4357/aa6973 , https://ui.adsabs.harvard.edu/abs/2017ApJ...839...99P 839, 99

    doi

  87. [96]

    M., Birnstiel T., 2017b, @doi [ ] 10.3847/1538-4357/aa7edb , https://ui.adsabs.harvard.edu/abs/2017ApJ...845...68P 845, 68

    Pinilla P., Pohl A., Stammler S. M., Birnstiel T., 2017b, @doi [ ] 10.3847/1538-4357/aa7edb , https://ui.adsabs.harvard.edu/abs/2017ApJ...845...68P 845, 68

    doi

  88. [97]

    Pinilla P., et al., 2018, @doi [ ] 10.3847/1538-4357/aabf94 , https://ui.adsabs.harvard.edu/abs/2018ApJ...859...32P 859, 32

    2018 doi

  89. [98]

    M., Tazzari M., 2019, @doi [ ] 10.3847/1538-4357/ab1cb8 , https://ui.adsabs.harvard.edu/abs/2019ApJ...878...16P 878, 16

    Pinilla P., Benisty M., Cazzoletti P., Harsono D., P \'e rez L. M., Tazzari M., 2019, @doi [ ] 10.3847/1538-4357/ab1cb8 , https://ui.adsabs.harvard.edu/abs/2019ApJ...878...16P 878, 16

    2019 doi

  90. [99]

    T., Stammler S

    Pinilla P., Lenz C. T., Stammler S. M., 2021a, @doi [ ] 10.1051/0004-6361/202038920 , https://ui.adsabs.harvard.edu/abs/2021A&A...645A..70P 645, A70

    doi

  91. [100]

    Pinilla P., et al., 2021b, @doi [ ] 10.1051/0004-6361/202140371 , https://ui.adsabs.harvard.edu/abs/2021A&A...649A.122P 649, A122

    doi

  92. [101]

    Preibisch T., Brown A. G. A., Bridges T., Guenther E., Zinnecker H., 2002, @doi [ ] 10.1086/341174 , https://ui.adsabs.harvard.edu/abs/2002AJ....124..404P 124, 404

    2002 doi

  93. [102]

    Ribas \'A ., et al., 2023, @doi [ ] 10.1051/0004-6361/202245637 , https://ui.adsabs.harvard.edu/abs/2023A&A...673A..77R 673, A77

    2023 doi

  94. [103]

    J., Dullemond C

    Rodenkirch P. J., Dullemond C. P., 2022, @doi [ ] 10.1051/0004-6361/202142571 , https://ui.adsabs.harvard.edu/abs/2022A&A...659A..42R 659, A42

    2022 doi

  95. [104]

    P., 2023, @doi [ ] 10.1016/j.newar.2023.101674 , https://ui.adsabs.harvard.edu/abs/2023NewAR..9601674R 96, 101674

    Rosotti G. P., 2023, @doi [ ] 10.1016/j.newar.2023.101674 , https://ui.adsabs.harvard.edu/abs/2023NewAR..9601674R 96, 101674

    2023

  96. [105]

    P., Tazzari M., Booth R

    Rosotti G. P., Tazzari M., Booth R. A., Testi L., Lodato G., Clarke C., 2019, @doi [ ] 10.1093/mnras/stz1190 , 486, 4829

    2019 doi

  97. [106]

    A., et al., 2022, @doi [ ] 10.1051/0004-6361/202141035 , https://ui.adsabs.harvard.edu/abs/2022A&A...662A.121R 662, A121

    Rota A. A., et al., 2022, @doi [ ] 10.1051/0004-6361/202141035 , https://ui.adsabs.harvard.edu/abs/2022A&A...662A.121R 662, A121

    2022 doi

  98. [107]

    Salmeron R., Wardle M., 2008, @doi [ ] 10.1111/j.1365-2966.2008.13430.x , https://ui.adsabs.harvard.edu/abs/2008MNRAS.388.1223S 388, 1223

    2008

  99. [108]

    M., Reg \'a ly Z., Lyra W., 2024, @doi [ ] 10.1051/0004-6361/202347605 , https://ui.adsabs.harvard.edu/abs/2024A&A...686A..78S 686, A78

    S \'a ndor Z., Guilera O. M., Reg \'a ly Z., Lyra W., 2024, @doi [ ] 10.1051/0004-6361/202347605 , https://ui.adsabs.harvard.edu/abs/2024A&A...686A..78S 686, A78

    2024 doi

  100. [109]

    M., Umebayashi T., Nakano T., 2000, @doi [ ] 10.1086/317075 , https://ui.adsabs.harvard.edu/abs/2000ApJ...543..486S 543, 486

    Sano T., Miyama S. M., Umebayashi T., Nakano T., 2000, @doi [ ] 10.1086/317075 , https://ui.adsabs.harvard.edu/abs/2000ApJ...543..486S 543, 486

    2000 doi

  101. [110]

    M., et al., 2020, @doi [ ] 10.1038/s41586-020-2779-6 , https://ui.adsabs.harvard.edu/abs/2020Natur.586..228S 586, 228

    Segura-Cox D. M., et al., 2020, @doi [ ] 10.1038/s41586-020-2779-6 , https://ui.adsabs.harvard.edu/abs/2020Natur.586..228S 586, 228

    2020 doi

  102. [111]

    D., Vlasblom M., van Dishoeck E

    Sellek A. D., Vlasblom M., van Dishoeck E. F., 2024, @doi [arXiv e-prints] 10.48550/arXiv.2412.01895 , https://ui.adsabs.harvard.edu/abs/2024arXiv241201895S p. arXiv:2412.01895

    2024 doi arXiv

  103. [112]

    I., Sunyaev R

    Shakura N. I., Sunyaev R. A., 1973, , https://ui.adsabs.harvard.edu/abs/1973A&A....24..337S 24, 337

    1973

  104. [113]

    Shi Y., et al., 2024, @doi [ ] 10.3847/1538-4357/ad2e94 , https://ui.adsabs.harvard.edu/abs/2024ApJ...966...59S 966, 59

    2024 doi

  105. [114]

    V., 1916, Zeitschrift fur Physik, https://ui.adsabs.harvard.edu/abs/1916ZPhy...17..557S 17, 557

    Smoluchowski M. V., 1916, Zeitschrift fur Physik, https://ui.adsabs.harvard.edu/abs/1916ZPhy...17..557S 17, 557

    1916

  106. [115]

    Speedie J., et al., 2024, @doi [ ] 10.1038/s41586-024-07877-0 , https://ui.adsabs.harvard.edu/abs/2024Natur.633...58S 633, 58

    2024 doi

  107. [116]

    P., Birnstiel T., Stammler S

    Stadler J., G \'a rate M., Pinilla P., Lenz C., Dullemond C. P., Birnstiel T., Stammler S. M., 2022, @doi [ ] 10.1051/0004-6361/202243338 , https://ui.adsabs.harvard.edu/abs/2022A&A...668A.104S 668, A104

    2022 doi

  108. [117]

    M., Birnstiel T., 2022, @doi [ ] 10.3847/1538-4357/ac7d58 , https://ui.adsabs.harvard.edu/abs/2022ApJ...935...35S 935, 35

    Stammler S. M., Birnstiel T., 2022, @doi [ ] 10.3847/1538-4357/ac7d58 , https://ui.adsabs.harvard.edu/abs/2022ApJ...935...35S 935, 35

    2022 doi

  109. [118]

    M., Birnstiel T., G \'a rate M., 2023a, DustPyLib: A library of DustPy extensions , Astrophysics Source Code Library, record ascl:2310.005

    Stammler S. M., Birnstiel T., G \'a rate M., 2023a, DustPyLib: A library of DustPy extensions , Astrophysics Source Code Library, record ascl:2310.005

  110. [119]

    M., Lichtenberg T., Dr a \.z kowska J., Birnstiel T., 2023b, @doi [ ] 10.1051/0004-6361/202245512 , https://ui.adsabs.harvard.edu/abs/2023A&A...670L...5S 670, L5

    Stammler S. M., Lichtenberg T., Dr a \.z kowska J., Birnstiel T., 2023b, @doi [ ] 10.1051/0004-6361/202245512 , https://ui.adsabs.harvard.edu/abs/2023A&A...670L...5S 670, L5

    doi

  111. [120]

    K., Ogihara M., Morbidelli A., Crida A., Guillot T., 2016, @doi [ ] 10.1051/0004-6361/201628955 , 596, A74

    Suzuki T. K., Ogihara M., Morbidelli A., Crida A., Guillot T., 2016, @doi [ ] 10.1051/0004-6361/201628955 , 596, A74

    2016 doi

  112. [121]

    Tabone B., et al., 2017, @doi [ ] 10.1051/0004-6361/201731691 , 607, L6

    2017 doi

  113. [122]

    P., Cridland A

    Tabone B., Rosotti G. P., Cridland A. J., Armitage P. J., Lodato G., 2022, @doi [ ] 10.1093/mnras/stab3442 , https://ui.adsabs.harvard.edu/abs/2022MNRAS.512.2290T 512, 2290

    2022 doi

  114. [123]

    Takeuchi T., Lin D. N. C., 2002, @doi [ ] 10.1086/344437 , https://ui.adsabs.harvard.edu/abs/2002ApJ...581.1344T 581, 1344

    2002 doi

  115. [124]

    Tazaki R., Tanaka H., Kataoka A., Okuzumi S., Muto T., 2019, @doi [ ] 10.3847/1538-4357/ab45f0 , https://ui.adsabs.harvard.edu/abs/2019ApJ...885...52T 885, 52

    2019 doi

  116. [125]

    Tazaki R., Ginski C., Dominik C., 2023, @doi [ ] 10.3847/2041-8213/acb824 , https://ui.adsabs.harvard.edu/abs/2023ApJ...944L..43T 944, L43

    2023 doi

  117. [126]

    Tazzari M., et al., 2017, @doi [ ] 10.1051/0004-6361/201730890 , https://ui.adsabs.harvard.edu/abs/2017A&A...606A..88T 606, A88

    2017 doi

  118. [127]

    J., Testi L., Williams J

    Tazzari M., Clarke C. J., Testi L., Williams J. P., Facchini S., Manara C. F., Natta A., Rosotti G., 2021, @doi [ ] 10.1093/mnras/stab1808 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.506.2804T 506, 2804

    2021 doi

  119. [128]

    The Astropy Collaboration et al., 2018, @doi [ ] 10.3847/1538-3881/aabc4f , https://ui.adsabs.harvard.edu/abs/2018AJ....156..123T 156, 123

    2018 doi

  120. [129]

    Tong S., Alexander R., Rosotti G., 2024, @doi [ ] 10.1006/icar.1995.1058 , https://ui.adsabs.harvard.edu/abs/1995Icar..114..237D 114, 237

    2024

  121. [130]

    R., Facchini S., Manara C

    Trapman L., Ansdell M., Hogerheijde M. R., Facchini S., Manara C. F., Miotello A., Williams J. P., Bruderer S., 2020, @doi [ ] 10.1051/0004-6361/201834537 , https://ui.adsabs.harvard.edu/abs/2020A&A...638A..38T 638, A38

    2020 doi

  122. [131]

    M., Birnstiel T., Wilner D

    Tripathi A., Andrews S. M., Birnstiel T., Wilner D. J., 2017, @doi [ ] 10.3847/1538-4357/aa7c62 , https://ui.adsabs.harvard.edu/abs/2017ApJ...845...44T 845, 44

    2017 doi

  123. [132]

    Ueda T., Kataoka A., Tsukagoshi T., 2022, @doi [ ] 10.3847/1538-4357/ac634d , https://ui.adsabs.harvard.edu/abs/2022ApJ...930...56U 930, 56

    2022 doi

  124. [133]

    Ueda T., Tazaki R., Okuzumi S., Flock M., Sudarshan P., 2024, @doi [Nature Astronomy] 10.1038/s41550-024-02308-6 , https://ui.adsabs.harvard.edu/abs/2024NatAs...8.1148U 8, 1148

    2024 doi

  125. [134]

    Villenave M., et al., 2021, @doi [ ] 10.1051/0004-6361/202140496 , https://ui.adsabs.harvard.edu/abs/2021A&A...653A..46V 653, A46

    2021 doi

  126. [135]

    Virtanen P., et al., 2020, @doi [Nature Methods] 10.1038/s41592-019-0686-2 , 17, 261

    2020 doi

  127. [136]

    JWST-MIRI reveals a peculiar CO _2 -rich chemistry in the drift-dominated disk CX Tau ( @eprint arXiv 2412.12715 ), https://arxiv.org/abs/2412.12715

    Vlasblom M., et al., 2024, MINDS. JWST-MIRI reveals a peculiar CO _2 -rich chemistry in the drift-dominated disk CX Tau ( @eprint arXiv 2412.12715 ), https://arxiv.org/abs/2412.12715

    2024 arXiv

  128. [137]

    G., Brandt R

    Warren S. G., Brandt R. E., 2008, @doi [Journal of Geophysical Research (Atmospheres)] 10.1029/2007JD009744 , https://ui.adsabs.harvard.edu/abs/2008JGRD..11314220W 113, D14220

    2008 doi

  129. [138]

    J., 1977, @doi [ ] 10.1093/mnras/180.2.57 , https://ui.adsabs.harvard.edu/abs/1977MNRAS.180...57W 180, 57

    Weidenschilling S. J., 1977, @doi [ ] 10.1093/mnras/180.2.57 , https://ui.adsabs.harvard.edu/abs/1977MNRAS.180...57W 180, 57

    1977 doi

  130. [139]

    pp 56 -- 61, @doi 10.25080/Majora-92bf1922-00a

    W es M c K inney 2010, in S t\'efan van der W alt J arrod M illman eds, P roceedings of the 9th P ython in S cience C onference. pp 56 -- 61, @doi 10.25080/Majora-92bf1922-00a

    2010 doi

  131. [140]

    L., 1972, in Elvius A., ed., From Plasma to Planet

    Whipple F. L., 1972, in Elvius A., ed., From Plasma to Planet. p. 211

    1972

  132. [141]

    W., Dullemond C

    Windmark F., Birnstiel T., Ormel C. W., Dullemond C. P., 2012, @doi [ ] 10.1051/0004-6361/201220004 , https://ui.adsabs.harvard.edu/abs/2012A&A...544L..16W 544, L16

    2012 doi

  133. [142]

    C., Rilinger A

    Xin Z., Espaillat C. C., Rilinger A. M., Ribas \'A ., Mac \' as E., 2023, @doi [ ] 10.3847/1538-4357/aca52b , https://ui.adsabs.harvard.edu/abs/2023ApJ...942....4X 942, 4

    2023 doi

  134. [143]

    Yamaguchi M., Tsukagoshi T., Muto T., Nomura H., Nakazato T., Ikeda S., Tamura M., Kawabe R., 2021, @doi [ ] 10.3847/1538-4357/ac2bfd , https://ui.adsabs.harvard.edu/abs/2021ApJ...923..121Y 923, 121

    2021 doi

  135. [144]

    Yamaguchi M., et al., 2024, @doi [ ] 10.1093/pasj/psae022 , https://ui.adsabs.harvard.edu/abs/2024PASJ...76..437Y 76, 437

    2024 doi

  136. [145]

    N., Lithwick Y., 2007, @doi [ ] 10.1016/j.icarus.2007.07.012 , https://ui.adsabs.harvard.edu/abs/2007Icar..192..588Y 192, 588

    Youdin A. N., Lithwick Y., 2007, @doi [ ] 10.1016/j.icarus.2007.07.012 , https://ui.adsabs.harvard.edu/abs/2007Icar..192..588Y 192, 588

    2007 doi

  137. [146]

    P., Lodato G., 2021a, @doi [ ] 10.1093/mnras/stab985 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.504.2235Z 504, 2235

    Zagaria F., Rosotti G. P., Lodato G., 2021a, @doi [ ] 10.1093/mnras/stab985 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.504.2235Z 504, 2235

    doi

  138. [147]

    P., Lodato G., 2021b, @doi [ ] 10.1093/mnras/stab2024 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.2531Z 507, 2531

    Zagaria F., Rosotti G. P., Lodato G., 2021b, @doi [ ] 10.1093/mnras/stab2024 , https://ui.adsabs.harvard.edu/abs/2021MNRAS.507.2531Z 507, 2531

    doi

  139. [148]

    A., Bergin E

    Zhang K., Blake G. A., Bergin E. A., 2015, @doi [ ] 10.1088/2041-8205/806/1/L7 , https://ui.adsabs.harvard.edu/abs/2015ApJ...806L...7Z 806, L7

    2015 doi

  140. [149]

    E., Bergin E

    Zhang S., Kalscheur M., Long F., Zhang K., Long D. E., Bergin E. A., Zhu Z., Trapman L., 2023a, @doi [ ] 10.3847/1538-4357/acd334 , https://ui.adsabs.harvard.edu/abs/2023ApJ...952..108Z 952, 108

    doi

  141. [150]

    Zhang S., Zhu Z., Ueda T., Kataoka A., Sierra A., Carrasco-Gonz \'a lez C., Mac \' as E., 2023b, @doi [ ] 10.3847/1538-4357/acdb4e , https://ui.adsabs.harvard.edu/abs/2023ApJ...953...96Z 953, 96

    doi

  142. [151]

    P., Andrews S

    Zormpas A., Birnstiel T., Rosotti G. P., Andrews S. M., 2022, @doi [ ] 10.1051/0004-6361/202142046 , https://ui.adsabs.harvard.edu/abs/2022A&A...661A..66Z 661, A66

    2022 doi

  143. [152]

    A., Mardones D., 2020, @doi [ ] 10.1051/0004-6361/201936950 , https://ui.adsabs.harvard.edu/abs/2020A&A...634L..12D 634, L12

    de Valon A., Dougados C., Cabrit S., Louvet F., Zapata L. A., Mardones D., 2020, @doi [ ] 10.1051/0004-6361/201936950 , https://ui.adsabs.harvard.edu/abs/2020A&A...634L..12D 634, L12

    2020 doi

  144. [153]

    pandas development team T., 2020, pandas-dev/pandas: Pandas, @doi 10.5281/zenodo.3509134 , https://doi.org/10.5281/zenodo.3509134

    2020 doi

  145. [154]

    D., 2021, @doi [ ] 10.3847/1538-3881/ac0255 , https://ui.adsabs.harvard.edu/abs/2021AJ....162...28V 162, 28

    van der Marel N., Mulders G. D., 2021, @doi [ ] 10.3847/1538-3881/ac0255 , https://ui.adsabs.harvard.edu/abs/2021AJ....162...28V 162, 28

    2021 doi

  146. [155]

    van der Marel N., et al., 2013, @doi [Science] 10.1126/science.1236770 , 340, 1199

    2013 doi

  147. [156]

    arXiv:2204.08225

    van der Marel N., et al., 2022, @doi [arXiv e-prints] 10.48550/arXiv.2204.08225 , https://ui.adsabs.harvard.edu/abs/2022arXiv220408225V p. arXiv:2204.08225

    2022 doi

  148. [157]

    C., Varoquaux G., 2011, @doi [Computing in Science & Engineering] 10.1109/MCSE.2011.37 , 13, 22

    van der Walt S., Colbert S. C., Varoquaux G., 2011, @doi [Computing in Science & Engineering] 10.1109/MCSE.2011.37 , 13, 22

    2011 doi

Pith tools

Reviewed August 8, 2026 · model on record in the stance chip above.