arxiv: 2604.09122 · v1 · submitted 2026-04-10 · 🌌 astro-ph.EP · astro-ph.GA· astro-ph.SR

Recognition: unknown

Dust Processing in Protoplanetary Discs From Infall to Dispersal: the Origin of Solar System Isotopic Heterogeneities

Mark A. Hutchison , Maria Sch\"onb\"achler , Lucio Mayer , Jean-David Bod\'enan

Authors on Pith no claims yet

Pith reviewed 2026-05-10 17:27 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.GAastro-ph.SR

keywords protoplanetary discsnucleosynthetic heterogeneitydust processingsize sortingisotopic variationssolar system formationthermal processing

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The pith

Disc size sorting redistributed dust to explain Solar System isotopic heterogeneities

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

The paper reviews dynamical, collisional, and thermal processes in protoplanetary discs from initial infall to gas dispersal that shaped the distribution of dust carrying nucleosynthetic anomalies. It establishes that these processes preserved isotopic signatures from stellar sources and redistributed them heterogeneously, with size sorting highlighted as a major but understudied mechanism that can induce variations without full mixing. A sympathetic reader would care because this connects microscopic dust behavior to the distinct isotopic compositions measured in asteroids and planets at the parts-per-million level. The review integrates prior isolated studies into one framework to show how multiple mechanisms interact and to flag previously overlooked contributions to the final Solar System structure.

Core claim

Nucleosynthetic heterogeneity between asteroids and planets originates from anomalous carrier phases in dust that escaped complete homogenization and were instead redistributed by disc processes, including thermal processing and size sorting, during the transition from molecular cloud infall to disc dispersal.

What carries the argument

Size sorting of dust particles in the protoplanetary disc, which selectively transports grains of different sizes and thereby redistributes the carrier phases that hold nucleosynthetic isotopic anomalies.

If this is right

Size sorting likely occurred in the disc and can induce nucleosynthetic heterogeneity.
Disc processes must be examined together because their effects are altered or amplified when combined.
Thermal processing and dynamical transport preserved some stellar isotopic signatures while redistributing others.
Inherited variations from the parental molecular cloud were modified during the protoplanetary disc phase.
Previously underexplored mechanisms such as size sorting contributed to the observed isotopic structure.

Where Pith is reading between the lines

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

Models that include size sorting could predict testable patterns of isotopic variation within individual meteorite parent bodies.
The framework implies that the duration of the disc phase relative to dust processing sets the scale of heterogeneity finally accreted into planets.
Similar dust sorting in other star-forming regions might produce observable isotopic differences in exoplanet compositions if the same carrier phases are present.

Load-bearing premise

Anomalous carrier phases in dust were preserved and heterogeneously distributed by disc processes without complete homogenization.

What would settle it

A meteorite survey showing no correlation between grain size and isotopic anomaly strength, or evidence of uniform isotopic composition across all Solar System materials, would falsify the role of disc processing.

read the original abstract

The nucleosynthetic heterogeneity between different asteroids and planets is well established. These isotopic variations manifest themselves at the part per millions level or larger, in isotopes that were synthesised in various stellar environments. To escape homogenisation, some of these isotopic signatures must have been preserved in dust, which ended up being heterogeneously distributed in the solar protoplanetary disc. The origin of the nucleosynthetic heterogeneity is still poorly constrained, potentially reflecting inherited isotope variations from the Sun's parental molecular cloud and/or processing and redistribution during the subsequent protoplanetary disc phase with thermal processing and size sorting as major processes. This chapter aims to provide a broad review of the dynamical, collisional, and thermal processes in protoplanetary discs -- from initial infall to gas dispersal -- that may have influenced the distribution and survival of the anomalous carrier phases, which finally accreted into asteroids and planets. While several of these mechanisms have been considered in past studies, they are often examined in isolation, which impedes the assessment of how their effects may be altered or amplified by additional disc processes. Size sorting in particular has received little attention, and here we highlight that this process likely occurred in the disc and can induce nucleosynthetic heterogeneity. By placing previous studies within the context of a comprehensive overview, we aim to clarify the broader physical framework in which anomalous carrier transport occurs and identify previously underexplored mechanisms that may have contributed to the final isotopic structure of the Solar System we see today.

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.

Desk Editor's Note private letter to a colleague

This review synthesizes disc processes that could preserve isotopic anomalies in the solar system and rightly flags size sorting as understudied, but it offers no new calculations or tests.

read the letter

The paper's core contribution is a broad synthesis of how dynamical, collisional, and thermal processes in protoplanetary discs—from infall to dispersal—might redistribute anomalous dust carriers without complete homogenization, leading to the observed nucleosynthetic variations in asteroids and planets. It does this by pulling together existing literature on radial drift, turbulence, and thermal processing, and it makes a fair case that these mechanisms interact in ways that isolated studies miss. The emphasis on size sorting stands out as useful because the authors note it has received little attention yet could plausibly sort carriers by size and produce heterogeneity at the ppm level or higher. The citations track established work in disc dynamics and meteoritics, and the logic flows without obvious internal contradictions or invented entities. No new derivations or data appear, which is expected for a review. The central assumption—that some anomalous phases survived disc processing and were heterogeneously distributed—rests on observational premises rather than fresh verification here, so the framework stays plausible but untested in the paper itself. Minor soft spot: the discussion of how processes amplify or cancel each other could use more concrete examples from specific simulations, though the authors acknowledge this is an overview. This is aimed at cosmochemists and planet-formation modelers who need context on linking disc physics to solar system isotopes. A reader wanting quantitative predictions or new modeling will come away empty, but someone mapping the open questions will find it organizes the landscape clearly. It deserves peer review as a review article because the synthesis is careful and highlights a concrete gap worth following up.

Referee Report

0 major / 2 minor

Summary. The manuscript is a review chapter synthesizing dynamical, collisional, and thermal processes in protoplanetary discs from initial infall through gas dispersal. It argues that these mechanisms can preserve anomalous carrier phases in dust and redistribute them heterogeneously, thereby explaining the observed nucleosynthetic isotopic variations (at ppm levels or larger) between asteroids and planets. The review particularly highlights size sorting as an understudied process capable of inducing such heterogeneity and places prior isolated studies into a unified physical framework.

Significance. If the synthesis holds, the work offers a valuable integrative framework that connects established literature on disc dynamics, radial drift, turbulence, thermal processing, and isotopic data. Its main contribution lies in emphasizing size sorting's potential role and identifying underexplored mechanisms, which can guide future quantitative modeling. The review does not advance new simulations or predictions but organizes the field effectively and notes the need to avoid complete homogenization of carriers.

minor comments (2)

[Abstract] Abstract: the phrasing 'part per millions level' is nonstandard and should be corrected to 'parts per million level' for precision and grammatical consistency.
[Throughout] The review would benefit from explicit cross-references or a summary table linking specific disc processes (e.g., radial drift, turbulence) to their predicted effects on carrier preservation and isotopic heterogeneity, to improve readability across the comprehensive overview.

Simulated Author's Rebuttal

0 responses · 0 unresolved

We thank the referee for their supportive summary and recommendation of minor revision. Our manuscript is a review chapter that synthesizes dynamical, collisional, and thermal processes across the lifetime of protoplanetary discs, with emphasis on how size sorting and related mechanisms can preserve and redistribute anomalous carrier phases to produce the observed nucleosynthetic isotopic heterogeneities at ppm levels. We value the recognition that the work places prior studies into a unified framework and highlights underexplored aspects.

Circularity Check

0 steps flagged

No significant circularity in this review synthesis

full rationale

This paper is a broad review synthesizing dynamical, collisional, and thermal processes across protoplanetary disc stages without advancing new quantitative predictions, simulations, equations, or fitted parameters. The emphasis on size sorting as a likely inducer of nucleosynthetic heterogeneity rests on observational premises from external isotopic data and prior disc dynamics studies, not on any internal derivation chain that reduces to self-defined inputs or self-citations. No load-bearing steps match the enumerated circularity patterns; the text explicitly notes mechanisms are often examined in isolation in past work and positions its overview as contextual clarification rather than a self-referential result.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

This is a review paper; no new free parameters, axioms, or invented entities are introduced.

pith-pipeline@v0.9.0 · 5598 in / 963 out tokens · 39208 ms · 2026-05-10T17:27:48.957752+00:00 · methodology

discussion (0)

Reference graph

Works this paper leans on

239 extracted references · 9 canonical work pages · 1 internal anchor

[1]

Ábrahám P., et al., 2009, Nature, 459, 224

2009
[2]

Akram W., Schönbächler M., Bisterzo S., Gallino R., 2015, Geochimica Cosmochimica Acta, 165, 484

2015
[3]

Alibert Y., et al., 2018, Nature Astronomy, 2, 873

2018
[4]

J., Bernstein M

Allamandola L. J., Bernstein M. P., Sandford S. A., Walker R. L., 1999, in Altwegg K., Ehren- freund P., Geiss J., Huebner W. F., eds, Composition and Origin of Cometary Materials. Springer Netherlands, Dordrecht, pp 219–232

1999
[5]

H., Ireland T

Amelin Y., Kaltenbach A., Iizuka T., Stirling C. H., Ireland T. R., Petaev M., Jacobsen S. B., 2010, Earth and Planetary Science Letters, 300, 343

2010
[6]

Anand A., Mezger K., 2025, Icarus, 441, 116714

2025
[7]

Anand A., et al., 2024, Geochimica Cosmochimica Acta, 382, 118

2024
[8]

M., et al., 2018, ApJ, 869, L41

Andrews S. M., et al., 2018, ApJ, 869, L41

2018
[9]

pp 387–410, doi:10.2458/azu_uapress_9780816531240-ch017

AudardM.,etal.,2014,inBeutherH.,KlessenR.S.,DullemondC.P.,HenningT.,eds,Protostars and Planets VI. pp 387–410, doi:10.2458/azu_uapress_9780816531240-ch017

work page doi:10.2458/azu_uapress_9780816531240-ch017 2014
[10]

Bai X.-N., 2013, ApJ, 772, 96

2013
[11]

M., 2010, ApJS, 190, 297

Bai X.-N., Stone J. M., 2010, ApJS, 190, 297

2010
[12]

J., Williams I

Baines M. J., Williams I. P., Asebiomo A. S., 1965, MNRAS, 130, 63

1965
[13]

A., Hawley J

Balbus S. A., Hawley J. F., 1991, ApJ, 376, 214

1991
[14]

J., et al., 2025, Nature Astronomy

Barnes J. J., et al., 2025, Nature Astronomy

2025
[15]

Barosch J., et al., 2022, ApJ, 935, L3

2022
[16]

Barthelmy D., 2012, Mineralogy Database,http://webmineral.com/

2012
[17]

Protostars and Planets VII , year = 2023, editor =

Benisty M., et al., 2023, in Inutsuka S., Aikawa Y., Muto T., Tomida K., Tamura M., eds, As- tronomical Society of the Pacific Conference Series Vol. 534, Protostars and Planets VII. p. 605, doi:10.48550/arXiv.2203.09991

work page doi:10.48550/arxiv.2203.09991 2023
[18]

E., 2019, ApJS, 241, 25

Benítez-Llambay P., Krapp L., Pessah M. E., 2019, ApJS, 241, 25

2019
[19]

R., Füri E., Lodders K., Marty B., 2020, Space Sci

Bermingham K. R., Füri E., Lodders K., Marty B., 2020, Space Sci. Rev., 216, 133

2020
[20]

Birnstiel T., 2024, ARA&A, 62, 157

2024
[21]

Birnstiel T., et al., 2010, A&A, 516, L14

2010
[22]

Bischoff A., Scott E. R. D., Metzler K., Goodrich C. A., 2006, in Lauretta D. S., McSween H. Y., eds, , Meteorites and the Early Solar System II. University of Arizona Press, p. 679

2006
[23]

Bischoff A., et al., 2022, Meteoritics & Planetary Science, 57, 1339

2022
[24]

Blum J., Wurm G., 2008, ARA&A, 46, 21

2008
[25]

Blum J., Wurm G., Kempf S., Henning T., 1996, Icarus, 124, 441

1996
[26]

Bodénan J.-D., Surville C., Szulágyi J., Mayer L., Schönbächler M., 2020, ApJ, 901, 60

2020
[27]

Bogdan T., Pillich C., Landers J., Wende H., Wurm G., 2020, A&A, 638, A151

2020
[28]

Bogdan T., Pillich C., Landers J., Wende H., Wurm G., 2023, A&A, 670, A6

2023
[29]

C., Durisen R

Boley A. C., Durisen R. H., 2008, ApJ, 685, 1193

2008
[30]

P., 2008, Earth and Planetary Science Letters, 268, 102

Boss A. P., 2008, Earth and Planetary Science Letters, 268, 102

2008
[31]

J., 2020, Nature Astronomy, 4, 492

Brasser R., Mojzsis S. J., 2020, Nature Astronomy, 4, 492

2020
[32]

P., Henning T., 2008a, A&A, 480, 859

Brauer F., Dullemond C. P., Henning T., 2008a, A&A, 480, 859
[33]

P., 2008b, A&A, 487, L1

Brauer F., Henning T., Dullemond C. P., 2008b, A&A, 487, L1
[34]

C., Escoube R., Münker C., 2018, Geochimica Cos- mochimica Acta, 239, 17

Braukmüller N., Wombacher F., Hezel D. C., Escoube R., Münker C., 2018, Geochimica Cos- mochimica Acta, 239, 17

2018
[35]

J., 2003, Treatise on Geochemistry, 1, 711

Brearley A. J., 2003, Treatise on Geochemistry, 1, 711

2003
[36]

Burkhardt C., Schönbächler M., 2015, Geochimica Cosmochimica Acta, 165, 361

2015
[37]

Burkhardt C., Kleine T., Dauphas N., Wieler R., 2012, Earth and Planetary Science Letters, 357, 298

2012
[38]

A., Lamy P

Burns J. A., Lamy P. L., Soter S., 1979, Icarus, 40, 1

1979
[39]

O., Nittler L

Busemann H., Alexander M. O., Nittler L. R., 2007, Meteoritics & Planetary Science, 42, 1387

2007
[40]

Cacciapuoti L., et al., 2024, A&A, 682, A61

2024
[41]

Chambers J., 2021, ApJ, 914, 102

2021
[42]

C., 2014, ApJ, 780, 53 Dust Processing in Protoplanetary Discs 23

Chatterjee S., Tan J. C., 2014, ApJ, 780, 53 Dust Processing in Protoplanetary Discs 23

2014
[43]

M., Cassen P., 1997, ApJ, 477, 398

Chick K. M., Cassen P., 1997, ApJ, 477, 398

1997
[44]

J., 2009, Icarus, 200, 655

Ciesla F. J., 2009, Icarus, 200, 655

2009
[45]

J., 2010, ApJ, 723, 514

Ciesla F. J., 2010, ApJ, 723, 514

2010
[46]

Y., Ibrahimov M

Clarke C., Lodato G., Melnikov S. Y., Ibrahimov M. A., 2005, MNRAS, 361, 942

2005
[47]

D., 1982, QJRAS, 23, 174

Clayton D. D., 1982, QJRAS, 23, 174

1982
[48]

S., Kaib N

Clement M. S., Kaib N. A., Raymond S. N., Walsh K. J., 2018, Icarus, 311, 340

2018
[49]

J., Lambrechts M., van Kooten E., Johansen A., 2024, A&A, 685, A114

Colmenares M. J., Lambrechts M., van Kooten E., Johansen A., 2024, A&A, 685, A114

2024
[50]

ConnellyJ.N.,BizzarroM.,KrotA.N.,NordlundÅ.,WielandtD.,IvanovaM.A.,2012,Science, 338, 651

2012
[51]

L., Schönbächler M., 2017, AJ, 154, 172

Cook D. L., Schönbächler M., 2017, AJ, 154, 172

2017
[52]

L., Smith T., Leya I., Hilton C

Cook D. L., Smith T., Leya I., Hilton C. D., Walker R. J., Schönbächler M., 2018, Earth and Planetary Science Letters, 503, 29

2018
[53]

L., Leya I., Schönbächler M., 2020, Meteoritics & Planetary Science, 55, 2758

Cook D. L., Leya I., Schönbächler M., 2020, Meteoritics & Planetary Science, 55, 2758

2020
[54]

L., Meyer B

Cook D. L., Meyer B. S., Schönbächler M., 2021, ApJ, 917, 59

2021
[55]

N., Hogan R

Cuzzi J. N., Hogan R. C., Paque J. M., Dobrovolskis A. R., 2001, ApJ, 546, 496

2001
[56]

D’Alessio P., Cantö J., Calvet N., Lizano S., 1998, ApJ, 500, 411

1998
[57]

D’AlessioP.,CalvetN.,HartmannL.,MuzerolleJ.,SitkoM.,2004,inBurtonM.G.,Jayawardhana R.,BourkeT.L.,eds,IAUSymposiumVol.221,StarFormationatHighAngularResolution.p.403, doi:10.48550/arXiv.astro-ph/0309590

work page internal anchor Pith review doi:10.48550/arxiv.astro-ph/0309590 2004
[58]

Dauphas N., Marty B., Reisberg L., 2002a, ApJ, 565, 640
[59]

Dauphas N., Marty B., Reisberg L., 2002b, ApJ, 569, L139
[60]

DauphasN.,DavisA.M.,MartyB.,ReisbergL.,2004,EarthandPlanetaryScienceLetters,226, 465

2004
[61]

David-Cléris T., Laibe G., Lapeyre Y., 2025, MNRAS

2025
[62]

DavisA.,RichterF.,2014,inHollandH.D.,TurekianK.K.,eds,,TreatiseonGeochemistry(Sec- ond Edition), second edition edn, Elsevier, Oxford, pp 335–360, doi:https://doi.org/10.1016/B978- 0-08-095975-7.00112-1

work page doi:10.1016/b978- 2014
[63]

De Juan Ovelar M., Pinilla P., Min M., Dominik C., Birnstiel T., 2016, MNRAS, 459, L85

2016
[64]

Deng H., Mayer L., Latter H., 2020, ApJ, 891, 154

2020
[65]

Rev., 220, 76

Desch S., Miret-Roig N., 2024, Space Sci. Rev., 220, 76

2024
[66]

534, Protostars and Planets VII

DeschS.J.,YoungE.D.,DunhamE.T.,FujimotoY.,DunlapD.R.,2023,inInutsukaS.,Aikawa Y.,MutoT.,TomidaK.,TamuraM.,eds,AstronomicalSocietyofthePacificConferenceSeriesVol. 534, Protostars and Planets VII. p. 759

2023
[67]

Dipierro G., Pinilla P., Lodato G., Testi L., 2015, MNRAS, 451, 974

2015
[68]

Dipierro G., Laibe G., Alexander R., Hutchison M., 2018, MNRAS, 479, 4187

2018
[69]

N., Wurm G., 2007, Protostars and Planets V, pp 783–800

Dominik C., Blum J., Cuzzi J. N., Wurm G., 2007, Protostars and Planets V, pp 783–800

2007
[70]

P., 2014, A&A, 572, A78

Drążkowska J., Dullemond C. P., 2014, A&A, 572, A78

2014
[71]

P., 2013, A&A, 556, A37

Drążkowska J., Windmark F., Dullemond C. P., 2013, A&A, 556, A37

2013
[72]

M., Li H., 2019, ApJ, 885, 91

Drążkowska J., Li S., Birnstiel T., Stammler S. M., Li H., 2019, ApJ, 885, 91

2019
[73]

DrozdovskayaM.N.,WalshC.,vanDishoeckE.F.,FuruyaK.,MarboeufU.,ThiabaudA.,Harsono D., Visser R., 2016, MNRAS, 462, 977

2016
[74]

Dubrulle B., Morfill G., Sterzik M., 1995, Icarus, 114, 237

1995
[75]

P., Dominik C., 2004, A&A, 421, 1075

Dullemond C. P., Dominik C., 2004, A&A, 421, 1075

2004
[76]

P., Dominik C., 2005, A&A, 434, 971

Dullemond C. P., Dominik C., 2005, A&A, 434, 971

2005
[77]

P., et al., 2018, ApJ, 869, L46

Dullemond C. P., et al., 2018, ApJ, 869, L46

2018
[78]

O., Caselli P., Girart J

Dunham M. M., et al., 2014, in Beuther H., Klessen R. S., Dullemond C. P., Henning T., eds, Protostars and Planets VI. pp 195–218, doi:10.2458/azu_uapress_9780816531240-ch009

work page doi:10.2458/azu_uapress_9780816531240-ch009 2014
[79]

I., Krijt S., 2022, A&A, 667, A121

Eistrup C., Cleeves L. I., Krijt S., 2022, A&A, 667, A121

2022
[80]

C., Lugaro M., Schönbächler M., 2020, Nature Astronomy, 4, 273

Ek M., Hunt A. C., Lugaro M., Schönbächler M., 2020, Nature Astronomy, 4, 273

2020

Showing first 80 references.