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arxiv: 2606.28171 · v1 · pith:7QKQGEL3new · submitted 2026-06-26 · 🌌 astro-ph.EP · astro-ph.IM· astro-ph.SR

Demographics of planet-forming disks with the SKAO

Antonio Garufi , Sebasti\'an P\'erez , John D. Ilee , Daniel J. Price , Paola Pinilla , Marion Villenave , Eleonora Bianchi , Luca Cacciapuoti
show 16 more authors
Greta Guidi Giovanni Sabatini Yinhao Wu Asmita Bhandare Claudio Codella Nicol\'as Cuello Liton Majumdar Mayank Narang Linda Podio Danae Polychroni Isaac Radley Jessica Speedie Leonardo Testi Claudia Toci Diego Turrini David Wilner
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Pith reviewed 2026-06-29 02:03 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.IMastro-ph.SR
keywords planet-forming disksprotoplanetary diskscentimeter-sized grainsdust evolutionSKAOplanet formationdisk demographicspebbles
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The pith

SKAO will enable the first large-scale high-resolution survey of centimeter emission from nearby planet-forming disks.

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

The paper argues that while ALMA has advanced understanding of micron-sized dust in disks, major uncertainties remain about the presence and role of centimeter-sized grains in planet formation. It establishes that the SKAO can address this by surveying disk emission at centimeter wavelengths across hundreds of targets in nearby star-forming regions. This approach would resolve the spatial distribution, spectral properties, and evolutionary trends of these grains. The resulting data would constrain dust growth, disk dynamics, and total dust masses while also offering chances to detect protoplanets and circumplanetary material.

Core claim

The SKAO will fill the observational gap by enabling the first large-scale, high-resolution survey of disk emission at centimeter wavelengths, allowing detection and characterization of pebbles through their spatial distribution, spectral properties, and evolutionary trends to provide essential constraints on dust growth and disk dynamics.

What carries the argument

Centimeter-wavelength high-resolution imaging of protoplanetary disk emission to detect and map centimeter-sized grains.

If this is right

  • Resolving pebble spatial distributions will constrain mechanisms of dust growth and radial drift in disks.
  • Spectral index measurements will reveal grain size distributions and compositions.
  • Comparing trends across multiple star-forming regions will map evolutionary stages of solid material.
  • Improved mass estimates will reduce uncertainties in the total solid content available for planet formation.
  • Detections of localized emission may identify protoplanets or their circumplanetary disks.

Where Pith is reading between the lines

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

  • Pairing SKAO centimeter data with ALMA millimeter maps could trace the full grain size spectrum from microns to centimeters in the same disks.
  • Demographic statistics from the survey might identify environmental factors that accelerate or suppress pebble formation.
  • If pebble emission proves common, it would support models in which these grains act as the main feedstock for core accretion.
  • Target selection strategies outlined here could be adapted to other facilities for multi-wavelength follow-up.

Load-bearing premise

Centimeter-sized grains exist in sufficient abundance and produce detectable emission at SKAO frequencies across a large sample of nearby disks.

What would settle it

A survey returning no detectable centimeter emission from a statistically large number of the targeted disks would show that the grains are either not abundant enough or do not emit as expected.

Figures

Figures reproduced from arXiv: 2606.28171 by Antonio Garufi, Asmita Bhandare, Claudia Toci, Claudio Codella, Danae Polychroni, Daniel J. Price, David Wilner, Diego Turrini, Eleonora Bianchi, Giovanni Sabatini, Greta Guidi, Isaac Radley, Jessica Speedie, John D. Ilee, Leonardo Testi, Linda Podio, Liton Majumdar, Luca Cacciapuoti, Marion Villenave, Mayank Narang, Nicol\'as Cuello, Paola Pinilla, Sebasti\'an P\'erez, Yinhao Wu.

Figure 1
Figure 1. Figure 1: Sketch of the dust grain growth and disk structure. The physical processes, observational tech￾niques, and disk components depicted are described in Sect. 1. The horizontal axis in the upper panel repre￾sents increasing particle size (and implicitly evolutionary time), from micron-sized grains to planetary cores. The disk in the sketch coarsely extends to 30–100 au. The inner part highlights the motion of … view at source ↗
Figure 2
Figure 2. Figure 2: Disk demographics from ALMA. The left panel highlights the observed decrease of dust mass as YSOs transition from Class I to Class II, and as we observe older star-forming regions such as Upper Sco (older than 5 Myr – in contrast to Ophiuchus, Chamaleon, Lupus, and Taurus of 1–3 Myr). To the right, an illustrative gallery of disks with different size from various star-forming regions is shown. Very extende… view at source ↗
Figure 3
Figure 3. Figure 3: Sketch of SED from a young stellar object. The dust emission is optically thick up to 3 mm. After 1 cm, the contribution from the free-free emission surpasses that from the dust. The result is an abrupt flattening for the observed photometry with wavelength. In case of gyro-synchrotron emission, the trend becomes positive after a few cm. With SKA in Band 5b, we expect the ionized gas contribution to be dom… view at source ↗
Figure 4
Figure 4. Figure 4: Predicted disk flux versus extent for the explored sample. The various lines indicate the 3𝜎 observ￾ability for different disk extent, integration time, and weighting parameters (red lines for Briggs weighting with Robust 1, orange for a tapered Natural weight, and blue for Uniform for which only the one hour case is shown). Empty and filled arrows indicate the extent over which disks are mildly and highly… view at source ↗
Figure 5
Figure 5. Figure 5: Number of disks detected and resolved with different weighting schemes and integration times. The bars indicate the range of detected or resolved objects depending on the disk extent in Band 5b (from 25% to 100% of the continuum extent measured by ALMA). and thus allows us to resolve a much larger number of disks but prevents the detection of a large reservoir of disks with a putative extent larger than 0.… view at source ↗
Figure 6
Figure 6. Figure 6: Spitzer map of the Ophiuchus molecular cloud from the ’Cores to Disks’ Legacy Project. Cyan circles indicate the locations of planet-forming disks detected in the ODISEA survey (Cieza et al., 2019). The large white circle shows the SKA-Mid primary beam at 1.4 GHz (∼1 deg), while the yellow circles mark the primary beams at 12.5 GHz (6.7’). Field-of-view sizes correspond to the primary beam of a 15-m dish. … view at source ↗
read the original abstract

Understanding how solid material in planet-forming disks evolves from micron-sized dust to planetary cores is a central challenge in modern astrophysics. This study has advanced dramatically in the past decade, largely driven by ALMA and high-contrast imaging facilities. However, major uncertainties remain regarding the presence, evolution, and role of centimeter-sized grains (the pebbles) in planet formation. The SKAO will fill this gap by enabling the first large-scale, high-resolution survey of disk emission at centimeter wavelengths. This chapter presents the scientific rationale and observational strategies to detect and characterize pebbles in the planet-forming disks of nearby star-forming regions. By resolving their spatial distribution, spectral properties, and evolutionary trends, SKA will offer essential constraints on dust growth and disk dynamics. This work provides observational strategies, target selection, and predictions on the detectability of hundreds of nearby disks. The chapter also explores SKA's potential to uncover the actual dust mass in disks, protoplanets and their circumplanetary disks, and other aspects of the planet formation. Together, these capabilities will establish SKAO as a cornerstone facility for planet formation science in the coming decade.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit. Tearing a paper down is the easy half of reading it; the pith above is the substance, this is the friction.

Referee Report

2 major / 2 minor

Summary. The manuscript outlines the scientific rationale for using the SKAO to perform the first large-scale, high-resolution surveys of planet-forming disks at centimeter wavelengths. It argues that this will enable characterization of centimeter-sized grains (pebbles), resolve their spatial distribution and spectral properties, and provide constraints on dust growth and disk dynamics in nearby star-forming regions. The text presents observational strategies, target selection criteria, predictions for detecting hundreds of disks, and potential applications to measuring actual dust masses, identifying protoplanets, and studying circumplanetary disks.

Significance. If the detectability assumptions and strategies prove robust, the work would offer timely guidance for SKAO early-science programs and help address a recognized gap in pebble evolution studies left by ALMA. It correctly identifies centimeter-wave observations as a key missing element for demographic studies of solids in disks. The absence of any quantitative sensitivity calculations or error budgets, however, limits the paper's immediate utility as a planning document.

major comments (2)
  1. [Abstract] Abstract and introductory sections: the central claim that SKAO 'will enable the first large-scale, high-resolution survey' and 'predictions on the detectability of hundreds of nearby disks' is asserted without any sensitivity calculations, assumed flux densities, grain-size distributions, or SKAO performance parameters. These quantities are load-bearing for the prospective conclusions yet are not derived or referenced.
  2. [Observational strategies] Section on observational strategies and target selection: no error budget, confusion limits, or assumed centimeter-grain opacities are provided to support the assertion that a statistically useful sample can be observed. The weakest assumption (sufficient abundance and detectable emission from cm-sized grains) is stated as motivation rather than demonstrated.
minor comments (2)
  1. The manuscript refers to itself as 'this chapter' in several places; clarify whether it is intended as a standalone journal article or a book chapter.
  2. Notation for SKAO versus SKA is used inconsistently; adopt a single acronym throughout.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their thoughtful review and constructive comments on our manuscript. We address each major comment below and agree that incorporating quantitative elements will improve the paper's utility as a planning document for SKAO observations.

read point-by-point responses

  1. Referee: [Abstract] Abstract and introductory sections: the central claim that SKAO 'will enable the first large-scale, high-resolution survey' and 'predictions on the detectability of hundreds of nearby disks' is asserted without any sensitivity calculations, assumed flux densities, grain-size distributions, or SKAO performance parameters. These quantities are load-bearing for the prospective conclusions yet are not derived or referenced.

    Authors: We agree that the current version presents these claims at a high level without explicit derivations. The predictions draw on standard literature values for cm-grain opacities and SKAO sensitivity estimates, but we acknowledge the need for transparency. In revision we will add a dedicated subsection with sensitivity calculations, assumed flux densities, grain-size distributions, and direct references to SKAO performance parameters to support the detectability predictions. revision: yes

  2. Referee: [Observational strategies] Section on observational strategies and target selection: no error budget, confusion limits, or assumed centimeter-grain opacities are provided to support the assertion that a statistically useful sample can be observed. The weakest assumption (sufficient abundance and detectable emission from cm-sized grains) is stated as motivation rather than demonstrated.

    Authors: We accept this point. The manuscript motivates the science case but does not include the requested error budgets, confusion limits, or explicit opacity assumptions. We will revise the observational strategies section to incorporate these quantitative elements, including an error budget and demonstration of detectable cm-grain emission under realistic assumptions, to better support the claim of a statistically useful sample. revision: yes

Circularity Check

0 steps flagged

No significant circularity

full rationale

The document is an observational strategy paper outlining planned SKAO surveys of planet-forming disks at centimeter wavelengths. It presents scientific motivation, target selection criteria, and detectability estimates but contains no derivations, fitted parameters, equations, or predictions that reduce to the paper's own inputs by construction. All claims are prospective and framed as motivations for new data rather than self-referential results. No self-citations serve as load-bearing premises for any asserted theorem or uniqueness result. The central claim (SKAO enabling large-scale cm-wave disk surveys) is independent of any internal fitting or renaming of known patterns.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

The paper is a review of observational strategies and does not introduce new parameters, axioms, or invented entities.

pith-pipeline@v0.9.1-grok · 5835 in / 951 out tokens · 44513 ms · 2026-06-29T02:03:37.717173+00:00 · methodology

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Works this paper leans on

142 extracted references · 141 canonical work pages · 4 internal anchors

  1. [1]

    doi: 10.1088/0004-637X/784/1/62. A. Alaguero et al. A&A, 687:A311, July

    work page doi:10.1088/0004-637x/784/1/62

  2. [2]

    ALMA Partnership et al

    doi: 10.1051/0004-6361/202449683. ALMA Partnership et al. ApJ, 808:L3, July

    work page doi:10.1051/0004-6361/202449683

  3. [3]

    doi: 10.1088/2041-8205/808/1/L3. S. M. Andrews. ARA&A, 58:483–528, Aug

    work page internal anchor Pith review doi:10.1088/2041-8205/808/1/l3 2041

  4. [4]

    doi: 10.1146/annurev-astro-031220-010302. S. M. Andrews and J. P . Williams. ApJ, 631:1134–1160, Oct

    work page doi:10.1146/annurev-astro-031220-010302

  5. [5]

    doi: 10.1086/432712. S. M. Andrews et al. ApJ, 820(2):L40, Apr

    work page doi:10.1086/432712

  6. [6]

    22 Demographics of planet-forming disks Antonio Garufi et al

    doi: 10.3847/2041-8205/820/2/L40. 22 Demographics of planet-forming disks Antonio Garufi et al. S. M. Andrews et al. ApJ, 869(2):L41, Dec

    work page doi:10.3847/2041-8205/820/2/l40 2041

  7. [7]

    doi: 10.3847/2041-8213/aaf741. M. Ansdell et al. ApJ, 828:46, Sept

    work page internal anchor Pith review doi:10.3847/2041-8213/aaf741 2041

  8. [8]

    doi: 10.3847/0004-637X/828/1/46. M. Ansdell et al. AJ, 153(5):240, May

    work page doi:10.3847/0004-637x/828/1/46

  9. [9]

    doi: 10.3847/1538-3881/aa69c0. M. Ansdell et al. ApJ, 859:21, May

    work page doi:10.3847/1538-3881/aa69c0

  10. [10]

    doi: 10.3847/1538-4357/aab890. M. Audard et al. In H. Beuther, R. S. Klessen, C. P . Dullemond, and T. Henning, editors, Protostars and Planets VI, pages 387–410, Jan

    work page doi:10.3847/1538-4357/aab890

  11. [11]

    doi: 10.2458/azu_uapress_9780816531240-ch017. J. Bae et al. In S. Inutsuka et al., editors, Protostars and Planets VII, volume 534 of Astronomical Society of the Pacific Conference Series, page 423, July

    work page doi:10.2458/azu_uapress_9780816531240-ch017

  12. [12]

    doi: 10.48550/arXiv.2210.13314. S. A. Barenfeld, J. M. Carpenter, L. Ricci, and A. Isella. ApJ, 827(2):142, Aug

    work page doi:10.48550/arxiv.2210.13314

  13. [13]

    doi: 10.1086/115385. M. Benisty et al. In S. Inutsuka et al., editors, Astronomical Society of the Pacific Conference Series, volume 534 of Astronomical Society of the Pacific Conference Series, page 605, July

    work page doi:10.1086/115385

  14. [14]

    doi: 10.1038/nature11805. L. M. Bernabò et al. ApJ, 927(2):L22, Mar

    work page doi:10.1038/nature11805

  15. [15]

    doi: 10.3847/2041-8213/ac574e. A. Bhandare et al. A&A, 687:A158, July

    work page doi:10.3847/2041-8213/ac574e 2041

  16. [16]

    doi: 10.1051/0004-6361/202449594. T. Birnstiel et al. ApJ, 869(2):L45, Dec

    work page doi:10.1051/0004-6361/202449594

  17. [17]

    doi: 10.3847/2041-8213/aaf743. I. Bonnell and P . Bastien. ApJ, 401:L31, Dec

    work page doi:10.3847/2041-8213/aaf743 2041

  18. [18]

    doi: 10.1086/186663. E. M. A. Borchert, D. J. Price, C. Pinte, and N. Cuello. MNRAS, 510(1):L37–L41, Feb. 2022a. doi: 10.1093/mnrasl/slab123. E. M. A. Borchert, D. J. Price, C. Pinte, and N. Cuello. MNRAS, 517(3):4436–4446, Dec. 2022b. doi: 10.1093/mnras/stac2872. J. M. Brown et al. ApJ, 704:496–502, Oct

    work page doi:10.1086/186663

  19. [19]

    doi: 10.1088/0004-637X/704/1/496. L. Cacciapuoti et al. ApJ, 961(1):90, Jan

    work page doi:10.1088/0004-637x/704/1/496

  20. [20]

    doi: 10.3847/1538-4357/ad0f17. L. Cacciapuoti et al. A&A, 700:A188, Aug

    work page doi:10.3847/1538-4357/ad0f17

  21. [21]

    doi: 10.1051/0004-6361/202554645. J. M. Carpenter et al. ApJ, 978(1):117, Jan

    work page doi:10.1051/0004-6361/202554645

  22. [22]

    doi: 10.3847/1538-4357/ad8ebc. C. Carrasco-González et al. ApJ, 821(1):L16, Apr

    work page doi:10.3847/1538-4357/ad8ebc

  23. [23]

    doi: 10.3847/2041-8205/821/1/L16. C. Carrasco-González et al. ApJ, 883(1):71, Sept

    work page doi:10.3847/2041-8205/821/1/l16 2041

  24. [24]

    doi: 10.3847/1538-4357/ab3d33. D. Carrera et al. arXiv e-prints , art. arXiv:2504.13246, Apr

    work page doi:10.3847/1538-4357/ab3d33

  25. [25]

    doi: 10.48550/arXiv.2504. 13246. S. Casassus et al. ApJ, 754:L31, Aug

    work page doi:10.48550/arxiv.2504

  26. [26]

    doi: 10.1088/2041-8205/754/2/L31. S. Casassus et al. ApJ, 812(2):126, Oct

    work page doi:10.1088/2041-8205/754/2/l31 2041

  27. [27]

    doi: 10.1088/0004-637X/812/2/126. P . Cazzoletti et al. A&A, 626:A11, June

    work page doi:10.1088/0004-637x/812/2/126

  28. [28]

    doi: 10.1051/0004-6361/201935273. L. A. Cieza et al. Nature, 535(7611):258–261, July

    work page doi:10.1051/0004-6361/201935273

  29. [29]

    doi: 10.1038/nature18612. L. A. Cieza et al. MNRAS, 474(4):4347–4357, Mar

    work page doi:10.1038/nature18612

  30. [30]

    doi: 10.1093/mnras/stx3059. L. A. Cieza et al. MNRAS, 482(1):698–714, Jan

    work page doi:10.1093/mnras/stx3059

  31. [31]

    doi: 10.1093/mnras/sty2653. L. A. Cieza et al. MNRAS, 501(2):2934–2953, Feb

    work page doi:10.1093/mnras/sty2653

  32. [32]

    doi: 10.1093/mnras/staa3787. L. I. Cleeves, E. A. Bergin, and T. J. Harries. ApJ, 807(1):2, July

    work page doi:10.1093/mnras/staa3787

  33. [33]

    doi: 10.1088/0004-637X/ 807/1/2. M. S. Connelley and B. Reipurth. ApJ, 861(2):145, July

    work page doi:10.1088/0004-637x/

  34. [34]

    doi: 10.3847/1538-4357/aaba7b. C. Contreras Peña et al. arXiv e-prints , art. arXiv:2504.21237, Apr

    work page doi:10.3847/1538-4357/aaba7b

  35. [35]

    Design Initiative for a 10 TeV pCM Wakefield Collider,

    doi: 10.48550/arXiv. 2504.21237. 23 Demographics of planet-forming disks Antonio Garufi et al. A. Coutens et al. A&A, 631:A58, Nov

    work page internal anchor Pith review doi:10.48550/arxiv

  36. [36]

    doi: 10.1051/0004-6361/201935340. N. Cuello, F. Ménard, and D. J. Price. European Physical Journal Plus, 138(1):11, Jan

    work page doi:10.1051/0004-6361/201935340

  37. [37]

    doi: 10.1140/epjp/s13360-022-03602-w. N. Cuello, A. Alaguero, and P . P . Poblete. Symmetry, 17(3):344, Feb

    work page doi:10.1140/epjp/s13360-022-03602-w

  38. [38]

    doi: 10.1051/0004-6361/202347042. E. Dartois et al. Nature Astronomy, 8:359–367, Mar

    work page doi:10.1051/0004-6361/202347042

  39. [39]

    doi: 10.1038/s41550-023-02155-x. M. de Juan Ovelar et al. MNRAS, 459(1):L85–L89, June

    work page doi:10.1038/s41550-023-02155-x

  40. [40]

    doi: 10.1093/mnrasl/slw051. G. Dipierro et al. MNRAS, 453(1):L73–L77, Oct

    work page doi:10.1093/mnrasl/slw051

  41. [41]

    doi: 10.1093/mnrasl/slv105. K. Doi and A. Kataoka. ApJ, 912(2):164, May

    work page doi:10.1093/mnrasl/slv105

  42. [42]

    doi: 10.3847/1538-4357/abe5a6. K. Doi and A. Kataoka. ApJ, 957(1):11, Nov

    work page doi:10.3847/1538-4357/abe5a6

  43. [43]

    doi: 10.3847/1538-4357/acf5df. B. T. Draine. ARA&A, 41:241–289, Jan

    work page doi:10.3847/1538-4357/acf5df

  44. [44]

    doi: 10.1146/annurev.astro.41.011802.094840. B. T. Draine and A. Lazarian. ApJ, 508(1):157–179, Nov

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1146/annurev.astro.41.011802.094840

  45. [45]

    doi: 10.1086/306387. J. Drążkowska and J. Szulágyi. ApJ, 866(2):142, Oct

    work page doi:10.1086/306387

  46. [46]

    doi: 10.3847/1538-4357/aae0fd. B. Dubrulle, G. Morfill, and M. Sterzik. Icarus, 114(2):237–246, Apr

    work page doi:10.3847/1538-4357/aae0fd

  47. [47]

    1995.1058

    doi: 10.1006/icar. 1995.1058. G. Duchêne, C. McCabe, A. M. Ghez, and B. A. Macintosh. ApJ, 606(2):969–982, May

    work page doi:10.1006/icar 1995

  48. [48]

    doi: 10.1086/383126. C. P . Dullemond et al. ApJ, 869(2):L46, Dec

    work page doi:10.1086/383126

  49. [49]

    doi: 10.3847/2041-8213/aaf742. M. M. Dunham et al. ApJ, 710(1):470–502, Feb

    work page doi:10.3847/2041-8213/aaf742 2041

  50. [50]

    doi: 10.1088/0004-637X/710/1/470. D. Fedele et al. A&A, 600:A72, Apr

    work page doi:10.1088/0004-637x/710/1/470

  51. [51]

    doi: 10.1051/0004-6361/201629860. R. Franceschi et al. A&A, 657:A74, Jan

    work page doi:10.1051/0004-6361/201629860

  52. [52]

    doi: 10.1051/0004-6361/202141705. L. Francis and N. van der Marel. ApJ, 892(2):111, Apr

    work page doi:10.1051/0004-6361/202141705

  53. [53]

    doi: 10.3847/1538-4357/ab7b63. F. Fressin et al. ApJ, 766(2):81, Apr

    work page doi:10.3847/1538-4357/ab7b63

  54. [54]

    doi: 10.1088/0004-637X/766/2/81. S. Fromang and R. P . Nelson. A&A, 496(3):597–608, Mar

    work page doi:10.1088/0004-637x/766/2/81

  55. [56]

    doi: 10.3847/1538-3881/aa80eb. M. Galametz et al. A&A, 632:A5, Dec

    work page doi:10.3847/1538-3881/aa80eb

  56. [57]

    doi: 10.1051/0004-6361/201936342. A. Garufi et al. A&A, 620:A94, Dec

    work page doi:10.1051/0004-6361/201936342

  57. [58]

    doi: 10.1051/0004-6361/201833872. A. Garufi et al. A&A, 658:A104, Feb

    work page doi:10.1051/0004-6361/201833872

  58. [59]

    doi: 10.1051/0004-6361/202141264. A. Garufi et al. A&A, 694:A290, Feb

    work page doi:10.1051/0004-6361/202141264

  59. [60]

    doi: 10.1051/0004-6361/202452496. S. Giacalone et al. ApJ, 882(1):33, Sept

    work page doi:10.1051/0004-6361/202452496

  60. [61]

    doi: 10.3847/1538-4357/ab311a. J. S. Greaves et al. Nature Astronomy, 2:662–667, June

    work page doi:10.3847/1538-4357/ab311a

  61. [62]

    doi: 10.1038/s41550-018-0495-z. O. Gressel, R. P . Nelson, N. J. Turner, and U. Ziegler. ApJ, 779(1):59, Dec

    work page doi:10.1038/s41550-018-0495-z

  62. [63]

    doi: 10.1051/0004-6361/202349046. G. Guidi et al. A&A, 664:A137, Aug

    work page doi:10.1051/0004-6361/202349046

  63. [64]

    doi: 10.1051/0004-6361/202142303. G. Guidi et al. In Advancing Astrophysics with the SKA – II (AASKAII)

    work page doi:10.1051/0004-6361/202142303

  64. [65]

    doi: 10.3847/1538-4357/acf853. I. Han et al. arXiv e-prints, art. arXiv:2506.16569, June

    work page doi:10.3847/1538-4357/acf853

  65. [66]

    doi: 10.48550/arXiv.2506.16569. G. H. Herbig. ApJ, 214:747–758, Jun

    work page doi:10.48550/arxiv.2506.16569

  66. [67]

    doi: 10.1086/155304. M. Hoare et al. In Advancing Astrophysics with the Square Kilometre Array (AASKA14), page 115, 24 Demographics of planet-forming disks Antonio Garufi et al. Apr

    work page doi:10.1086/155304

  67. [68]

    doi: 10.22323/1.215.0115. J. Huang et al. ApJ, 976(1):132, Nov

    work page doi:10.22323/1.215.0115

  68. [69]

    doi: 10.3847/1538-4357/ad84df. L. A. Hühn et al. A&A, 696:A162, Apr

    work page doi:10.3847/1538-4357/ad84df

  69. [70]

    doi: 10.1051/0004-6361/202452689. A. Isella et al. Phys. Rev. Lett. , 117:251101, Dec

    work page doi:10.1051/0004-6361/202452689

  70. [71]

    URL http://link.aps.org/doi/10.1103/PhysRevLett.117.251101

    doi: 10.1103/PhysRevLett.117.251101. URL http://link.aps.org/doi/10.1103/PhysRevLett.117.251101. S. Jin et al. ApJ, 818(1):76, Feb

    work page doi:10.1103/physrevlett.117.251101

  71. [72]

    doi: 10.3847/0004-637X/818/1/76. A. Johansen, S. Ida, and R. Brasser. A&A, 622:A202, Feb

    work page doi:10.3847/0004-637x/818/1/76

  72. [74]

    doi: 10.1051/0004-6361/201832957. Á. Kóspál et al. ApJS, 256(2):30, Oct

    work page doi:10.1051/0004-6361/201832957

  73. [75]

    doi: 10.3847/1538-4365/ac0f09. M. Lambrechts and A. Johansen. A&A, 544:A32, Aug

    work page doi:10.3847/1538-4365/ac0f09

  74. [76]

    doi: 10.1051/0004-6361/201219127. C.-F. Lee, Z.- Y . Li, and N. J. Turner. Nature Astronomy, page 466, Oct

    work page doi:10.1051/0004-6361/201219127

  75. [77]

    doi: 10.3847/1538-4357/acd5c9. H. B. Liu. ApJ, 914(1):25, June

    work page doi:10.3847/1538-4357/acd5c9

  76. [78]

    doi: 10.3847/1538-4357/abf8b6. H. B. Liu et al. ApJ, 972(2):163, Sept

    work page doi:10.3847/1538-4357/abf8b6

  77. [79]

    doi: 10.3847/1538-4357/ad5dab. G. Lodato et al. MNRAS, 518(3):4481–4493, Jan

    work page doi:10.3847/1538-4357/ad5dab

  78. [80]

    doi: 10.1093/mnras/stac3223. D. Lommen et al. A&A, 495(3):869–879, Mar

    work page doi:10.1093/mnras/stac3223

  79. [81]

    doi: 10.1051/0004-6361:200810999. F. Long et al. ApJ, 869(1):17, Dec

    work page doi:10.1051/0004-6361:200810999

  80. [82]

    doi: 10.3847/1538-4357/aae8e1. F. Long et al. ApJ, 915(2):131, July

    work page doi:10.3847/1538-4357/aae8e1

Showing first 80 references.