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arxiv: 2604.25263 · v1 · submitted 2026-04-28 · 🌌 astro-ph.EP · astro-ph.SR

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Oxygen Isotopic Compositions of Chondrules as Probes of Solar Protoplanetary Disk Formation

Sota Arakawa , Takayuki Ushikubo , Ryosuke T. Tominaga
Authors on Pith no claims yet

Pith reviewed 2026-05-07 14:41 UTC · model grok-4.3

classification 🌌 astro-ph.EP astro-ph.SR
keywords oxygen isotopeschondrulesprotoplanetary disksolar nebulamass infallisotopic exchangecarbonaceous chondritesordinary chondrites
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The pith

Simulations of solar disk formation show that moderate radial mass infall reproduces oxygen isotopic compositions of carbonaceous chondrules.

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

The paper uses one-dimensional models of protoplanetary disk evolution that include mass falling in from the surrounding cloud to track how oxygen isotopes evolve in the disk material. By applying an isotope exchange model based on laboratory experiments, the authors test different scenarios for how far out the infalling material lands and what the original cloud composition was like. A sympathetic reader would care because chondrules are the building blocks of asteroids and planets, so matching their isotopes to disk conditions provides direct evidence for how the early solar system assembled and processed its materials. The results indicate that either the infall was confined to about 10 astronomical units or the cloud had less ice and weaker self-shielding of carbon monoxide than usually assumed. This framework also points to water vapor escaping during heating events as the cause of observed trends in isotopes and oxidation states.

Core claim

The central claim is that the oxygen isotopic compositions of carbonaceous-chondrite chondrules can be reproduced in the disk evolution model if the radial extent of mass infall is moderate at about 10 au, or if it is larger than 10 au but the parental cloud core was ice-depleted or had weaker CO self-shielding. The model further suggests that the bimodal trends in isotopic composition and redox state arise from partial escape of H2O vapor from chondrule-forming regions. However, ordinary-chondrite chondrules formed inside the snow line at temperatures below 500 K would be difficult to explain because isotopic exchange occurs efficiently only in hotter inner regions above 500-600 K.

What carries the argument

One-dimensional simulations solving the diffusion-advection equation for disk surface density evolution with added mass infall from the parental cloud core, coupled to an experimentally derived model for oxygen isotope exchange between silicates and vapor species.

If this is right

  • The observed oxygen isotopes in carbonaceous chondrules are consistent with either limited radial spread of infalling gas and dust or altered initial cloud conditions.
  • Bimodal distributions in isotopes and oxidation can result from water vapor loss during flash heating of chondrules.
  • Ordinary chondrules require formation conditions where temperatures allow efficient isotope exchange, likely closer to the star.
  • The model constrains the possible radial profiles of material addition during disk formation.

Where Pith is reading between the lines

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

  • Different chondrite groups may sample material from distinct radial zones or epochs in the disk's history.
  • Future observations of protoplanetary disks around other stars could test whether infall radii are typically around 10 au.
  • The assumption of efficient exchange only at high temperatures suggests that ordinary chondrules might have formed earlier or in a different dynamical setting than currently modeled.
  • Linking to redox states implies that volatile loss processes during chondrule formation influenced the final compositions of planetesimals.

Load-bearing premise

The laboratory-derived rates and conditions for oxygen isotope exchange between silicates and gas species hold under the actual temperature, density, and timescale conditions inside the solar protoplanetary disk.

What would settle it

Laboratory experiments demonstrating that significant oxygen isotope exchange between chondrule silicates and surrounding vapor does not occur at temperatures below 500 K in realistic disk gas compositions, or astronomical observations showing that the radial extent of mass infall in the early solar disk greatly exceeded 10 au with standard cloud ice content and shielding.

Figures

Figures reproduced from arXiv: 2604.25263 by Ryosuke T. Tominaga, Sota Arakawa, Takayuki Ushikubo.

Figure 1
Figure 1. Figure 1: (a) Oxygen three-isotope diagram of solar system materials. The gray solid line indicates the Primitive Chondrule Materials (PCM) line (Ushikubo et al. 2012), with a slope of approximately 1, whereas the gray dashed line indicates the terrestrial fractionation (TF) line, with a slope of 0.52. Red open circle: solar photosphere inferred from solar-wind samples collected by Genesis (McKeegan et al. 2011). Re… view at source ↗
Figure 2
Figure 2. Figure 2: Phase-transition diagram of the oxygen reservoirs considered in this study. For silicates, we consider four phases: amorphous (amo), crystalline (cry), condensate (cond), and vapor (svap). For H2O, we consider two phases: ice (wice) and vapor (wvap), and for CO we also consider two phases: ice (cice) and vapor (cvap). In the molecular cloud core, we assume that silicates exist as amo, H2O as wice, and CO a… view at source ↗
Figure 4
Figure 4. Figure 4: Temporal evolution of the radial distribution of the protoplanetary disks. The left, middle, and right columns correspond to ωcd = 3 × 10−15 s −1 (i.e., rc,fin ≈ 1 au), ωcd = 1 × 10−14 s −1 (i.e., rc,fin ≈ 10 au), and ωcd = 3 × 10−14 s −1 (i.e., rc,fin ≈ 100 au), respectively. We set aagg,in = aagg,out = 0.1 mm in these calculations. Different lines represent snapshots at different times, and red dashed li… view at source ↗
Figure 5
Figure 5. Figure 5: Radial distribution of each oxygen reservoir and their oxygen isotopic composition at t = 1 Myr. The left, middle, and right columns correspond to ωcd = 3 × 10−15 s −1 (i.e., rc,fin ≈ 1 au), ωcd = 1 × 10−14 s −1 (i.e., rc,fin ≈ 10 au), and ωcd = 3 × 10−14 s −1 (i.e., rc,fin ≈ 100 au), respectively. We set aagg,in = aagg,out = 0.1 mm in these calculations. The vertical cyan lines represent the location of H… view at source ↗
Figure 6
Figure 6. Figure 6: Radial distribution of the disk midplane temperature, each oxygen reservoir, and their oxygen isotopic composition at t = 1 Myr. The left, middle, and right columns correspond to case (i) (aagg,in = 10 mm and aagg,out = 0.1 mm), case (ii) (aagg,in = 0.1 mm and aagg,out = 10 mm), and case (iii) (aagg,in = 10 mm and aagg,out = 10 mm), respectively. We set ωcd = 1 × 10−14 s −1 (i.e., rc,fin ≈ 10 au) in these … view at source ↗
Figure 7
Figure 7. Figure 7: Radial distribution of each oxygen reservoir and their oxygen isotopic composition at t = 1 Myr. The left, middle, and right columns correspond to the fiducial case (χH2O = 2, χCO = 3, δ 18OH2O,0 = +180‰ (i.e., ∆17OH2O,0 = +81.4‰), and δ 18OCO,0 = −220‰ (i.e., ∆17OCO,0 = −105.4‰)), the ice-depleted case (χH2O = 2/3, χCO = 1, δ 18OH2O,0 = +180‰, and δ 18OCO,0 = −220‰), and the weaker CO self-shielding case … view at source ↗
Figure 8
Figure 8. Figure 8: A schematic scenario that may explain the observed trend between the oxygen isotopic composition of chondrules and Mg#. (a) We consider an initial condition in which the mean isotopic composition of the solid phase in regions exterior to the snow line is ∆17Osolid ≈ −2‰. Initially, silicates (red circles) have an isotopic composition close to the solar-system average (∆17O ∼ −30‰), whereas H2O ice (blue he… view at source ↗
read the original abstract

Chondrules are thought to have formed during transient flash-heating events in dust-enriched regions of the solar protoplanetary disk. Although laboratory studies have characterized the oxygen isotopic compositions of chondritic materials, quantitative interpretations based on simulations of disk formation and evolution remain limited. Here, we perform one-dimensional simulations of disk formation and evolution by solving a diffusion--advection equation with mass infall from the parental cloud core. We compute the temporal evolution of oxygen isotopic compositions using an experimentally derived isotope-exchange model. We examine how the oxygen isotopic signatures of the disk depend on the radial distribution of infalling material and the composition of the parental cloud core. We find that the oxygen isotopic compositions of carbonaceous-chondrite chondrules can be reproduced if either (i) the radial extent of mass infall onto the disk is moderate ($\sim 10~{\rm au}$), or (ii) it is large ($> 10~{\rm au}$) and the parental cloud core was ice-depleted and/or experienced weaker CO self-shielding than is commonly assumed. We further suggest the scenario that the observed bimodal trends in oxygen isotopic composition and redox state reflect the partial escape of H$_{2}$O vapor from chondrule-forming regions during heating. In contrast, if ordinary-chondrite chondrules formed inside the snow line under background temperatures of $\lesssim 500~{\rm K}$, their oxygen isotopic compositions may be difficult to explain within the present disk-evolution model, because oxygen isotopic exchange between silicates and vapor species proceeds efficiently only in the inner disk at $T \gtrsim 500$--$600~{\rm K}$.

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

3 major / 2 minor

Summary. The manuscript presents one-dimensional diffusion-advection simulations of protoplanetary disk formation that include mass infall from the parental cloud core. Oxygen isotopic evolution is computed using an experimentally derived isotope-exchange model. The central claim is that carbonaceous-chondrite chondrule compositions are reproduced either when the radial extent of infall is moderate (~10 au) or when it is larger (>10 au) but the parental cloud is ice-depleted and/or has weaker CO self-shielding than standard assumptions; bimodal isotopic and redox trends are attributed to partial H2O vapor escape during heating. Ordinary-chondrite chondrules are argued to be difficult to explain if formed inside the snow line at background temperatures ≲500 K, because efficient exchange occurs only at T ≳500–600 K in the inner disk.

Significance. If the numerical results hold under independent validation, the work supplies a quantitative dynamical framework linking observed chondrule oxygen isotopes to disk formation parameters such as infall radial extent and cloud-core composition. The use of laboratory-derived exchange rates within a time-dependent infall model is a constructive step toward falsifiable predictions for solar-nebula evolution and the origin of isotopic bimodality.

major comments (3)
  1. [Abstract and results section describing infall scenarios] Abstract and results on parameter exploration: the reproduction of CC chondrule compositions is achieved by varying the free parameters 'radial extent of mass infall' and 'parental cloud ice content and CO self-shielding strength'; no a-priori constraints or grid of untuned runs are shown to demonstrate that the match is not the result of post-hoc selection.
  2. [Methods section on isotope-exchange model] Model implementation of isotope exchange: the manuscript assumes the experimentally derived exchange rates and temperature thresholds (efficient only at T ≳500–600 K) apply directly to disk pressures, densities, and transient heating timescales, but provides no explicit mapping, validation against disk conditions, or sensitivity tests to these assumptions.
  3. [Discussion of ordinary chondrules] Ordinary-chondrule discussion: the claim that OC chondrules are difficult to reproduce rests on the additional assumption of formation inside the snow line at background T ≲500 K; no alternative formation locations, temperature histories, or parameter variations are explored to test the robustness of this difficulty.
minor comments (2)
  1. [Abstract] The abstract states that the model 'further suggest[s] the scenario' of partial H2O escape but does not quantify the vapor-loss fraction or show the corresponding simulation output that supports the bimodal trend.
  2. [Abstract and methods] Notation for radial distances (au) and temperature thresholds is used without an initial definition or reference to standard values.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thorough and constructive review of our manuscript. We address each of the major comments below and have revised the manuscript accordingly to improve clarity and robustness.

read point-by-point responses

  1. Referee: Abstract and results on parameter exploration: the reproduction of CC chondrule compositions is achieved by varying the free parameters 'radial extent of mass infall' and 'parental cloud ice content and CO self-shielding strength'; no a-priori constraints or grid of untuned runs are shown to demonstrate that the match is not the result of post-hoc selection.

    Authors: We agree that a more systematic presentation of the parameter space would strengthen the manuscript. In the revised version, we have added a new figure (Figure X) that displays the oxygen isotopic compositions for a grid of simulations varying the radial extent of infall from 5 to 30 au and the ice content from 0 to 100% of standard, along with a table summarizing the key outcomes. This demonstrates that the reproduction of CC compositions occurs systematically for moderate infall radii or reduced ice contents, rather than isolated tuned cases. We have also updated the abstract to reflect this broader exploration. revision: yes

  2. Referee: Model implementation of isotope exchange: the manuscript assumes the experimentally derived exchange rates and temperature thresholds (efficient only at T ≳500–600 K) apply directly to disk pressures, densities, and transient heating timescales, but provides no explicit mapping, validation against disk conditions, or sensitivity tests to these assumptions.

    Authors: The exchange model is based on laboratory experiments that were conducted under conditions relevant to the solar nebula, as detailed in the cited references. To address the concern, we have performed additional sensitivity tests in the revised manuscript, varying the temperature threshold for efficient exchange between 400-700 K and the exchange rate by factors of 0.5 and 2. The results show that while the exact timing shifts, the overall conclusions regarding the need for inner disk conditions or specific infall scenarios remain unchanged. We have added a new subsection in the methods discussing the mapping to disk conditions, including estimates of how pressure and density affect the rates based on kinetic theory. revision: yes

  3. Referee: Ordinary-chondrule discussion: the claim that OC chondrules are difficult to reproduce rests on the additional assumption of formation inside the snow line at background T ≲500 K; no alternative formation locations, temperature histories, or parameter variations are explored to test the robustness of this difficulty.

    Authors: The paper's primary focus is on the implications of disk formation for chondrule isotopes under commonly assumed formation conditions for OC chondrules. We recognize that alternative scenarios exist, such as formation in warmer regions or with different thermal histories. In the revised discussion section, we have expanded the text to include a brief exploration of how higher background temperatures (e.g., >500 K) or additional heating events could facilitate isotopic exchange for OC chondrules. However, a comprehensive parameter study of all possible OC formation locations is outside the scope of this work, which centers on the infall and disk evolution phase. We believe the conditional statement in the original manuscript is appropriate given the current understanding. revision: partial

Circularity Check

0 steps flagged

No significant circularity; parameter exploration matches observations without reduction to inputs by construction

full rationale

The paper solves a standard 1D diffusion-advection equation for disk evolution with mass infall, inserts an experimentally derived isotope-exchange model, and varies two external parameters (radial extent of infall, parental cloud ice/CO-shielding) to determine the conditions under which observed CC chondrule compositions are reproduced. This is an explicit conditional parameter study, not a closed derivation in which the output isotopic ratios are forced by the inputs via self-definition, fitted parameters renamed as predictions, or load-bearing self-citations. No equations or sections in the provided text exhibit a reduction of the central claim to its own fitted values by construction; the exchange kinetics remain independent laboratory inputs. The result is therefore self-contained against the external observational benchmark.

Axiom & Free-Parameter Ledger

2 free parameters · 3 axioms · 0 invented entities

The central claim depends on varying the radial extent of infall and parental cloud properties to match data, plus standard assumptions about disk physics and temperature thresholds for isotope exchange.

free parameters (2)
  • radial extent of mass infall
    Varied between moderate (~10 au) and large (>10 au) to test reproduction of isotopic signatures.
  • parental cloud ice content and CO self-shielding strength
    Adjusted (ice-depleted or weaker shielding) to achieve match with carbonaceous chondrule data.
axioms (3)
  • standard math One-dimensional diffusion-advection equation governs disk mass and isotope transport
    Invoked for solving temporal evolution of the disk.
  • domain assumption Experimentally derived isotope-exchange model applies to protoplanetary disk conditions
    Used to compute oxygen isotopic evolution between silicates and vapor.
  • domain assumption Ordinary chondrules formed inside snow line at background temperatures ≲500 K
    Basis for concluding difficulty in explaining their isotopes.

pith-pipeline@v0.9.0 · 5615 in / 1645 out tokens · 121029 ms · 2026-05-07T14:41:05.076507+00:00 · methodology

discussion (0)

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Works this paper leans on

154 extracted references · 150 canonical work pages

  1. [1]

    Alexander, C. M. O., Nittler, L. R., Davidson, J., & Ciesla, F. J. 2017, M&PS, 52, 1797, doi: 10.1111/maps.12891

    work page doi:10.1111/maps.12891 2017

  2. [2]

    Alexander, C. M. O. D. 2004, GeoCoA, 68, 3943, doi: 10.1016/j.gca.2004.03.030

    work page doi:10.1016/j.gca.2004.03.030 2004

  3. [3]

    Alexander, C. M. O. D., Grossman, J. N., Ebel, D. S., & Ciesla, F. J. 2008, Science, 320, 1617, doi: 10.1126/science.1156561

    work page doi:10.1126/science.1156561 2008

  4. [4]

    Altwegg, K., Balsiger, H., & Fuselier, S. A. 2019, ARA&A, 57, 113, doi: 10.1146/annurev-astro-091918-104409

    work page doi:10.1146/annurev-astro-091918-104409 2019

  5. [5]

    2010, Earth and Planetary Science Letters, 300, 343, doi: 10.1016/j.epsl.2010.10.015 André, P., Di Francesco, J., Ward-Thompson, D., et al

    Amelin, Y ., Kaltenbach, A., Iizuka, T., et al. 2010, Earth and Planetary Science Letters, 300, 343, doi: 10.1016/j.epsl.2010.10.015 André, P., Di Francesco, J., Ward-Thompson, D., et al. 2014, in Protostars and Planets VI, ed. H. Beuther, R. S. Klessen, C. P. Dullemond, & T. Henning, 27–51, doi: 10.2458/azu_uapress_9780816531240-ch002

    work page doi:10.1016/j.epsl.2010.10.015 2010

  6. [6]

    P., van der Marel, N., et al

    Ansdell, M., Williams, J. P., van der Marel, N., et al. 2016, ApJ, 828, 46, doi: 10.3847/0004-637X/828/1/46

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

  7. [7]

    2021, ApJ, 920, 27, doi: 10.3847/1538-4357/ac157e

    Arakawa, S., Matsumoto, Y ., & Honda, M. 2021, ApJ, 920, 27, doi: 10.3847/1538-4357/ac157e

    work page doi:10.3847/1538-4357/ac157e 2021

  8. [8]

    2024, ApJ, 974, 199, doi: 10.3847/1538-4357/ad7795

    Kawasaki, N. 2024, ApJ, 974, 199, doi: 10.3847/1538-4357/ad7795

    work page doi:10.3847/1538-4357/ad7795 2024

  9. [9]

    Arakawa, S., Yamamoto, D., Ushikubo, T., et al. 2023, Icarus, 405, 115690, doi: 10.1016/j.icarus.2023.115690 20 Figure D1.Radial distribution of each oxygen reservoir and their oxygen isotopic composition att= 0.1 Myr, instead oft= 1 Myr(Figure 5). The left, middle, and right columns correspond toωcd = 3×10 −15 s−1 (i.e.,r c,fin ≈1 au),ω cd = 1×10 −14 s−1...

    work page doi:10.1016/j.icarus.2023.115690 2023

  10. [10]

    M., et al

    Armitage, P. J., Livio, M., & Pringle, J. E. 2001, MNRAS, 324, 705, doi: 10.1046/j.1365-8711.2001.04356.x

    work page doi:10.1046/j.1365-8711.2001.04356.x 2001

  11. [11]

    Arzoumanian, D., Arakawa, S., Kobayashi, M. I. N., et al. 2023, ApJL, 947, L29, doi: 10.3847/2041-8213/acc849

    work page doi:10.3847/2041-8213/acc849 2023

  12. [12]

    M., & Grevesse, N

    Asplund, M., Amarsi, A. M., & Grevesse, N. 2021, A&A, 653, A141, doi: 10.1051/0004-6361/202140445

    work page doi:10.1051/0004-6361/202140445 2021

  13. [13]

    1976, Earth and Planetary Science Letters, 31, 341, doi: 10.1016/0012-821X(76)90115-1

    Baertschi, P. 1976, Earth and Planetary Science Letters, 31, 341, doi: 10.1016/0012-821X(76)90115-1

    work page doi:10.1016/0012-821x(76)90115-1 1976

  14. [14]

    2017, ApJ, 845, 75, doi: 10.3847/1538-4357/aa7dda

    Bai, X.-N. 2017, ApJ, 845, 75, doi: 10.3847/1538-4357/aa7dda

    work page doi:10.3847/1538-4357/aa7dda 2017

  15. [15]

    2024, A&A, 687, A158, doi: 10.1051/0004-6361/202449594

    Bhandare, A., Commerçon, B., Laibe, G., et al. 2024, A&A, 687, A158, doi: 10.1051/0004-6361/202449594

    work page doi:10.1051/0004-6361/202449594 2024

  16. [16]

    2018, SSRv, 214, 52, doi: 10.1007/s11214-018-0486-5 Bodénan, J.-D., Starkey, N

    Blum, J. 2018, SSRv, 214, 52, doi: 10.1007/s11214-018-0486-5 Bodénan, J.-D., Starkey, N. A., Russell, S. S., Wright, I. P., &

    work page doi:10.1007/s11214-018-0486-5 2018

  17. [17]

    Franchi, I. A. 2014, Earth and Planetary Science Letters, 401, 327, doi: 10.1016/j.epsl.2014.05.035

    work page doi:10.1016/j.epsl.2014.05.035 2014

  18. [18]

    Bonnor, W. B. 1956, MNRAS, 116, 351, doi: 10.1093/mnras/116.3.351

    work page doi:10.1093/mnras/116.3.351 1956

  19. [19]

    Boogert, A. C. A., Gerakines, P. A., & Whittet, D. C. B. 2015, ARA&A, 53, 541, doi: 10.1146/annurev-astro-082214-122348

    work page Pith review doi:10.1146/annurev-astro-082214-122348 2015

  20. [20]

    1981, Icarus, 48, 353, doi: 10.1016/0019-1035(81)90051-8

    Cassen, P., & Moosman, A. 1981, Icarus, 48, 353, doi: 10.1016/0019-1035(81)90051-8

    work page doi:10.1016/0019-1035(81)90051-8 1981

  21. [21]

    T., & Kita, N

    Chaumard, N., Defouilloy, C., Hertwig, A. T., & Kita, N. T. 2021, GeoCoA, 299, 199, doi: 10.1016/j.gca.2021.02.012

    work page doi:10.1016/j.gca.2021.02.012 2021

  22. [22]

    I., & Goldreich, P

    Chiang, E. I., & Goldreich, P. 1997, ApJ, 490, 368, doi: 10.1086/304869

    work page doi:10.1086/304869 1997

  23. [23]

    doi:10.1016/j.icarus.2005.11.009 , eprint =

    Ciesla, F. J., & Cuzzi, J. N. 2006, Icarus, 181, 178, doi: 10.1016/j.icarus.2005.11.009

    work page doi:10.1016/j.icarus.2005.11.009 2006

  24. [24]

    Clayton, R. N. 2002, Nature, 415, 860, doi: 10.1038/415860b

    work page doi:10.1038/415860b 2002

  25. [25]

    N., Onuma, N., Grossman, L., & Mayeda, T

    Clayton, R. N., Onuma, N., Grossman, L., & Mayeda, T. K. 1977, Earth and Planetary Science Letters, 34, 209, doi: 10.1016/0012-821X(77)90005-X

    work page doi:10.1016/0012-821x(77)90005-x 1977

  26. [26]

    N., Bizzarro, M., Krot, A

    Connelly, J. N., Bizzarro, M., Krot, A. N., et al. 2012, Science, 338, 651, doi: 10.1126/science.1226919

    work page doi:10.1126/science.1226919 2012

  27. [27]

    N., & Zahnle, K

    Cuzzi, J. N., & Zahnle, K. J. 2004, ApJ, 614, 490, doi: 10.1086/423611 21 Figure D2.Radial distribution of each oxygen reservoir and their oxygen isotopic composition att= 0.1 Myr, instead oft= 1 Myr(Figure 6). The left, middle, and right columns correspond to case (i) (a agg,in = 10 mmanda agg,out = 0.1 mm), case (ii) (a agg,in = 0.1 mmand aagg,out = 10 ...

    work page doi:10.1086/423611 2004

  28. [28]

    2023, Icarus, 402, 115607, doi: 10.1016/j.icarus.2023.115607

    Mane, P. 2023, Icarus, 402, 115607, doi: 10.1016/j.icarus.2023.115607

    work page doi:10.1016/j.icarus.2023.115607 2023

  29. [29]

    2023, ApJ, 957, 11, doi: 10.3847/1538-4357/acf5df

    Doi, K., & Kataoka, A. 2023, ApJ, 957, 11, doi: 10.3847/1538-4357/acf5df

    work page doi:10.3847/1538-4357/acf5df 2023

  30. [30]

    Dominik, C., & Dullemond, C. P. 2024, A&A, 682, A144, doi: 10.1051/0004-6361/202347716

    work page doi:10.1051/0004-6361/202347716 2024

  31. [31]

    P., Apai, D., & Walch, S

    Dullemond, C. P., Apai, D., & Walch, S. 2006, ApJL, 640, L67, doi: 10.1086/503100

    work page doi:10.1086/503100 2006

  32. [32]

    and Monnier, J.D

    Dullemond, C. P., & Monnier, J. D. 2010, ARA&A, 48, 205, doi: 10.1146/annurev-astro-081309-130932

    work page doi:10.1146/annurev-astro-081309-130932 2010

  33. [33]

    S., Alexander, C

    Ebel, D. S., Alexander, C. M. O., & Libourel, G. 2018, in Chondrules: Records of Protoplanetary Disk Processes, ed. S. S

    2018

  34. [34]

    Russell, H. C. Connolly, Jr., & A. N. Krot, 151–174, doi: 10.1017/9781108284073.006

    work page doi:10.1017/9781108284073.006

  35. [35]

    2017, Royal Society Open Science, 4, 170114, doi: 10.1098/rsos.170114

    Ercolano, B., & Pascucci, I. 2017, Royal Society Open Science, 4, 170114, doi: 10.1098/rsos.170114

    work page doi:10.1098/rsos.170114 2017

  36. [36]

    2018, Earth and Planetary Science Letters, 481, 264, doi: 10.1016/j.epsl.2017.10.046

    Fujiya, W. 2018, Earth and Planetary Science Letters, 481, 264, doi: 10.1016/j.epsl.2017.10.046

    work page doi:10.1016/j.epsl.2017.10.046 2018

  37. [37]

    2019, Nature Astronomy, 3, 910, doi: 10.1038/s41550-019-0801-4

    Fujiya, W., Hoppe, P., Ushikubo, T., et al. 2019, Nature Astronomy, 3, 910, doi: 10.1038/s41550-019-0801-4

    work page doi:10.1038/s41550-019-0801-4 2019

  38. [38]

    E., Joswiak, D

    Fukuda, K., Brownlee, D. E., Joswiak, D. J., et al. 2021, GeoCoA, 293, 544, doi: 10.1016/j.gca.2020.09.036

    work page doi:10.1016/j.gca.2020.09.036 2021

  39. [39]

    J., Kimura, M., et al

    Fukuda, K., Tenner, T. J., Kimura, M., et al. 2022, GeoCoA, 322, 194, doi: 10.1016/j.gca.2021.12.027

    work page doi:10.1016/j.gca.2021.12.027 2022

  40. [40]

    2022, ApJ, 938, 29, doi: 10.3847/1538-4357/ac9233

    Furuya, K., Lee, S., & Nomura, H. 2022, ApJ, 938, 29, doi: 10.3847/1538-4357/ac9233

    work page doi:10.3847/1538-4357/ac9233 2022

  41. [41]

    Greenberg, J. M. 1998, A&A, 330, 375

    1998

  42. [42]

    , keywords =

    Guidi, G., Isella, A., Testi, L., et al. 2022, A&A, 664, A137, doi: 10.1051/0004-6361/202142303

    work page doi:10.1051/0004-6361/202142303 2022

  43. [43]

    L., Nuth, III, J

    Hallenbeck, S. L., Nuth, III, J. A., & Nelson, R. N. 2000, ApJ, 535, 247, doi: 10.1086/308810 22

    work page doi:10.1086/308810 2000

  44. [44]

    E., Wooden, D

    Harker, D. E., Wooden, D. H., Kelley, M. S. P., & Woodward, C. E. 2023, PSJ, 4, 242, doi: 10.3847/PSJ/ad0382

    work page doi:10.3847/psj/ad0382 2023

  45. [45]

    Progress of Theoretical Physics Supplement , year = 1981, month = jan, volume =

    Hayashi, C. 1981, Progress of Theoretical Physics Supplement, 70, 35, doi: 10.1143/PTPS.70.35

    work page doi:10.1143/ptps.70.35 1981

  46. [46]

    2008, A&A, 477, 9, doi: 10.1051/0004-6361:20078309

    Hennebelle, P., & Fromang, S. 2008, A&A, 477, 9, doi: 10.1051/0004-6361:20078309

    work page doi:10.1051/0004-6361:20078309 2008

  47. [47]

    2010, ARA&A, 48, 21, doi: 10.1146/annurev-astro-081309-130815 47

    Henning, T. 2010, ARA&A, 48, 21, doi: 10.1146/annurev-astro-081309-130815

    work page doi:10.1146/annurev-astro-081309-130815 2010

  48. [48]

    T., Defouilloy, C., & Kita, N

    Hertwig, A. T., Defouilloy, C., & Kita, N. T. 2018, GeoCoA, 224, 116, doi: 10.1016/j.gca.2017.12.013

    work page doi:10.1016/j.gca.2017.12.013 2018

  49. [49]

    T., Kimura, M., Ushikubo, T., Defouilloy, C., & Kita, N

    Hertwig, A. T., Kimura, M., Ushikubo, T., Defouilloy, C., & Kita, N. T. 2019, GeoCoA, 253, 111, doi: 10.1016/j.gca.2019.02.020

    work page doi:10.1016/j.gca.2019.02.020 2019

  50. [50]

    Hirano, S., Tsukamoto, Y ., Basu, S., & Machida, M. N. 2020, ApJ, 898, 118, doi: 10.3847/1538-4357/ab9f9d

    work page doi:10.3847/1538-4357/ab9f9d 2020

  51. [51]

    2018, ApJ, 868, 118, doi: 10.3847/1538-4357/aae0fb

    Homma, K., & Nakamoto, T. 2018, ApJ, 868, 118, doi: 10.3847/1538-4357/aae0fb

    work page doi:10.3847/1538-4357/aae0fb 2018

  52. [52]

    A., Okuzumi, S., Arakawa, S., & Fukai, R

    Homma, K. A., Okuzumi, S., Arakawa, S., & Fukai, R. 2024, PASJ, 76, 881, doi: 10.1093/pasj/psae052

    work page doi:10.1093/pasj/psae052 2024

  53. [53]

    K., et al

    Honda, M., Kataza, H., Okamoto, Y . K., et al. 2003, ApJL, 585, L59, doi: 10.1086/374034

    work page doi:10.1086/374034 2003

  54. [54]

    2023, SSRv, 219, 32, doi: 10.1007/s11214-023-00977-9

    Hoppe, P., Rubin, M., & Altwegg, K. 2023, SSRv, 219, 32, doi: 10.1007/s11214-023-00977-9

    work page doi:10.1007/s11214-023-00977-9 2023

  55. [55]

    2021, MNRAS, 503, 162, doi: 10.1093/mnras/stab542

    Hu, Z., & Bai, X.-N. 2021, MNRAS, 503, 162, doi: 10.1093/mnras/stab542

    work page doi:10.1093/mnras/stab542 2021

  56. [56]

    Hueso, T

    Hueso, R., & Guillot, T. 2005, A&A, 442, 703, doi: 10.1051/0004-6361:20041905

    work page doi:10.1051/0004-6361:20041905 2005

  57. [57]

    2025, ApJL, 979, L29, doi: 10.3847/2041-8213/ada554

    Iizuka, T., Hibiya, Y ., Yoshihara, S., & Hayakawa, T. 2025, ApJL, 979, L29, doi: 10.3847/2041-8213/ada554

    work page doi:10.3847/2041-8213/ada554 2025

  58. [58]

    2023, ApJ, 957, 47, doi: 10.3847/1538-4357/acf310

    Ishizaki, L., Tachibana, S., Okamoto, T., Yamamoto, D., & Ida, S. 2023, ApJ, 957, 47, doi: 10.3847/1538-4357/acf310

    work page doi:10.3847/1538-4357/acf310 2023

  59. [59]

    Iwasaki, K., Tomida, K., Takasao, S., Okuzumi, S., & Suzuki, T. K. 2024, PASJ, 76, 616, doi: 10.1093/pasj/psae036

    work page doi:10.1093/pasj/psae036 2024

  60. [60]

    C., Chaussidon, M., & Charnoz, S

    Jacquet, E., Pignatale, F. C., Chaussidon, M., & Charnoz, S. 2019, ApJ, 884, 32, doi: 10.3847/1538-4357/ab38c1

    work page doi:10.3847/1538-4357/ab38c1 2019

  61. [61]

    B., & Michaut, M

    Jaoul, O., Froidevaux, C., Durham, W. B., & Michaut, M. 1980, Earth and Planetary Science Letters, 47, 391, doi: 10.1016/0012-821X(80)90026-6

    work page doi:10.1016/0012-821x(80)90026-6 1980

  62. [62]

    2014, in Protostars and Planets VI, ed

    Johansen, A., Blum, J., Tanaka, H., et al. 2014, in Protostars and Planets VI, ed. H. Beuther, R. S. Klessen, C. P. Dullemond, & T. Henning, 547–570, doi: 10.2458/azu_uapress_9780816531240-ch024

    work page doi:10.2458/azu_uapress_9780816531240-ch024 2014

  63. [63]

    H., Villeneuve, J., & Libourel, G

    Jones, R. H., Villeneuve, J., & Libourel, G. 2018, in Chondrules: Records of Protoplanetary Disk Processes, ed. S. S. Russell, H. C. Connolly, Jr., & A. N. Krot, 57–90, doi: 10.1017/9781108284073.003

    work page doi:10.1017/9781108284073.003 2018

  64. [64]

    2025, Communications Earth and Environment, 6, 537, doi: 10.1038/s43247-025-02511-x

    Kawasaki, N., Arakawa, S., Miyamoto, Y ., et al. 2025, Communications Earth and Environment, 6, 537, doi: 10.1038/s43247-025-02511-x

    work page doi:10.1038/s43247-025-02511-x 2025

  65. [65]

    2017, GeoCoA, 201, 83, doi: 10.1016/j.gca.2015.12.031

    Kawasaki, N., Itoh, S., Sakamoto, N., & Yurimoto, H. 2017, GeoCoA, 201, 83, doi: 10.1016/j.gca.2015.12.031

    work page doi:10.1016/j.gca.2015.12.031 2017

  66. [66]

    2020, GeoCoA, 279, 1, doi: 10.1016/j.gca.2020.03.045

    Kawasaki, N., Wada, S., Park, C., Sakamoto, N., & Yurimoto, H. 2020, GeoCoA, 279, 1, doi: 10.1016/j.gca.2020.03.045

    work page doi:10.1016/j.gca.2020.03.045 2020

  67. [67]

    Kawasaki, Y ., & Machida, M. N. 2025, ApJ, 985, 106, doi: 10.3847/1538-4357/adc67b

    work page doi:10.3847/1538-4357/adc67b 2025

  68. [68]

    J., & Tielens, A

    Kemper, F., Vriend, W. J., & Tielens, A. G. G. M. 2004, ApJ, 609, 826, doi: 10.1086/421339

    work page doi:10.1086/421339 2004

  69. [69]

    T., Nagahara, H., Tachibana, S., et al

    Kita, N. T., Nagahara, H., Tachibana, S., et al. 2010, GeoCoA, 74, 6610, doi: 10.1016/j.gca.2010.08.011

    work page doi:10.1016/j.gca.2010.08.011 2010

  70. [70]

    T., & Ushikubo, T

    Kita, N. T., & Ushikubo, T. 2012, M&PS, 47, 1108, doi: 10.1111/j.1945-5100.2011.01264.x

    work page doi:10.1111/j.1945-5100.2011.01264.x 2012

  71. [71]

    2020, SSRv, 216, 55, doi: 10.1007/s11214-020-00675-w

    Kleine, T., Budde, G., Burkhardt, C., et al. 2020, SSRv, 216, 55, doi: 10.1007/s11214-020-00675-w

    work page doi:10.1007/s11214-020-00675-w 2020

  72. [72]

    2023, ApJ, 949, 119, doi: 10.3847/1538-4357/acc840

    Kondo, K., Okuzumi, S., & Mori, S. 2023, ApJ, 949, 119, doi: 10.3847/1538-4357/acc840

    work page doi:10.3847/1538-4357/acc840 2023

  73. [73]

    , keywords =

    Krijt, S., Bosman, A. D., Zhang, K., et al. 2020, ApJ, 899, 134, doi: 10.3847/1538-4357/aba75d

    work page doi:10.3847/1538-4357/aba75d 2020

  74. [74]

    Krot, A. N. 2019, M&PS, 54, 1647, doi: 10.1111/maps.13350

    work page doi:10.1111/maps.13350 2019

  75. [75]

    N., Nagashima, K., Lyons, J

    Krot, A. N., Nagashima, K., Lyons, J. R., Lee, J.-E., & Bizzarro, M. 2020, Science Advances, 6, eaay2724, doi: 10.1126/sciadv.aay2724

    work page doi:10.1126/sciadv.aay2724 2020

  76. [76]

    S., Burkhardt, C., Budde, G., & Kleine, T

    Kruijer, T. S., Burkhardt, C., Budde, G., & Kleine, T. 2017, Proceedings of the National Academy of Science, 114, 6712, doi: 10.1073/pnas.1704461114

    work page doi:10.1073/pnas.1704461114 2017

  77. [77]

    S., Kleine, T., & Borg, L

    Kruijer, T. S., Kleine, T., & Borg, L. E. 2020, Nature Astronomy, 4, 32, doi: 10.1038/s41550-019-0959-9

    work page doi:10.1038/s41550-019-0959-9 2020

  78. [78]

    Kunitomo, T.K

    Kunitomo, M., Suzuki, T. K., & Inutsuka, S.-i. 2020, MNRAS, 492, 3849, doi: 10.1093/mnras/staa087

    work page doi:10.1093/mnras/staa087 2020

  79. [79]

    S., Connolly, H

    Lauretta, D. S., Connolly, H. C., Aebersold, J. E., et al. 2024, M&PS, 59, 2453, doi: 10.1111/maps.14227

    work page doi:10.1111/maps.14227 2024

  80. [80]

    arXiv , author =:2102.07963 , journal =

    Lee, Y .-N., Charnoz, S., & Hennebelle, P. 2021, A&A, 648, A101, doi: 10.1051/0004-6361/202038105

    work page doi:10.1051/0004-6361/202038105 2021

Showing first 80 references.