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arxiv: 2603.09749 · v1 · submitted 2026-03-10 · 🌌 astro-ph.EP

Shaken, not stirred: inefficient mixing of CM- and CI-like materials

Sarah E. Anderson , Pierre Vernazza , Miroslav Broz This is my paper

Pith reviewed 2026-05-15 13:03 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords planetesimal scatteringgas dragSaturn growthCM chondritesCI chondritesimplantationasteroid beltsolar system formation
0
0 comments X

The pith

Saturn's growth scatters fewer than 2 percent of CM-like planetesimals beyond 15 au because gas drag damps their eccentricities.

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

The paper tests whether CM chondrite-like planetesimals scattered by Saturn's growth can reach the ice-giant region and contaminate the CI reservoir. N-body integrations that include gas drag show implantation fractions remain below 2 percent even in gas-rich conditions, since drag damps eccentricities and returns bodies to their perihelia instead of allowing circularization at large distances. Adding an ice-giant embryo raises the fraction to at most 4 percent in the most favorable case, but Type-I migration further lowers perihelia and hinders long-term retention at 15-25 au. For a total CM mass budget of about 1 Earth mass, at most 0.02-0.04 Earth masses reach those distances, producing a diluted fraction below 1-2 times 10 to the minus 3 in the outer ring and negligible contamination. Together with the observed distinct radial distributions of CM- and CI-like asteroids, the results indicate limited mixing between the two carbonaceous reservoirs.

Core claim

Outward scattering during Saturn's growth and migration implants fewer than about 2 percent of CM-like planetesimals beyond 15 au, even under gas-rich conditions, because gas drag damps their eccentricities and drives them back toward their perihelia rather than allowing them to circularize at larger distances. Adding an ice-giant core modestly increases the outward reach (up to about 4 percent in the most gas-rich case), but Type-I migration further lowers perihelia, making long-term retention at large distances difficult. For a CM mass budget M_CM,tot about 1 M_Earth, this implies at most M_CM less than 0.02-0.04 M_Earth reaches 15-25 au, corresponding to a diluted mass fraction less than

What carries the argument

N-body integrations of 100 km planetesimals launched from the outer edge of Jupiter's gap, including gas drag and gravitational perturbations of growing Jupiter and Saturn with optional nearby ice-giant embryo, across varied gas surface-density profiles and growth timescales; gas drag is the mechanism that damps eccentricities and prevents sustained outward implantation.

If this is right

  • Saturn's growth scatters CM-like planetesimals efficiently yet gas drag keeps implantation beyond 15 au below 2 percent.
  • An ice-giant embryo raises the implanted fraction modestly to 4 percent at most in gas-rich runs, but Type-I migration reduces perihelia and retention.
  • At most 0.02-0.04 Earth masses of CM material reaches 15-25 au for a total budget of 1 Earth mass.
  • This yields a diluted fraction below 1-2 times 10 to the minus 3 in the outer ring and negligible CI contamination.
  • Combined with distinct radial distributions of CM- and CI-like asteroids, mixing of the carbonaceous reservoirs remains limited.

Where Pith is reading between the lines

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

  • Weaker gas drag than modeled or different migration histories could raise implantation fractions and permit more mixing.
  • Trace CM signatures in outer solar system small bodies would test the predicted isolation of the CI reservoir.
  • The result supports separate formation zones for CM and CI materials with little cross-contamination across the early solar system.

Load-bearing premise

The simulations assume 100 km planetesimals experience the modeled gas-drag regime for the explored range of gas surface-density profiles and growth timescales.

What would settle it

Detection of a CM-like mass fraction exceeding roughly 0.002 in bodies or meteorites from the 15-25 au region would falsify the low implantation efficiency.

Figures

Figures reproduced from arXiv: 2603.09749 by Miroslav Broz, Pierre Vernazza, Sarah E. Anderson.

Figure 1
Figure 1. Figure 1: Cumulative distributions of the semi-major axis [PITH_FULL_IMAGE:figures/full_fig_p002_1.png] view at source ↗
Figure 2
Figure 2. Figure 2: Comparison of the gas profiles used in the various [PITH_FULL_IMAGE:figures/full_fig_p005_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Fraction (%) of planetesimals from each initial formation zone that end up within 1-au-wide semi-major-axis bins at [PITH_FULL_IMAGE:figures/full_fig_p006_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Eccentricity of remaining planetesimals as a function of semi-major axis at [PITH_FULL_IMAGE:figures/full_fig_p006_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p008_5.png] view at source ↗
Figure 6
Figure 6. Figure 6: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p008_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: Same as Fig [PITH_FULL_IMAGE:figures/full_fig_p011_7.png] view at source ↗
read the original abstract

A recent study suggests that CM chondrite-like planetesimals formed in the vicinity of Saturn, in a pressure bump outside the gap carved by proto-Jupiter. While a fraction of these objects was implanted into the asteroid belt as a consequence of Saturn's growth, it remains unclear whether the scattered remainder could reach the ice-giant region and mix with more distant carbonaceous reservoirs. We test whether outward scattering during Saturn's growth and migration can implant CM-like bodies onto long-lived orbits in the Uranus-Neptune region, where they could contaminate the CI reservoir. We performed N-body integrations of 100 km planetesimals launched from the outer edge of Jupiter's gap, including gas drag and the gravitational perturbations of growing Jupiter and Saturn, with optional inclusion of a nearby ice-giant embryo. We explored a range of gas surface-density profiles and growth timescales. While Saturn's growth efficiently scatters CM-like planetesimals, fewer than about 2 percent are implanted beyond 15 au, even under gas-rich conditions, because gas drag damps their eccentricities and drives them back toward their perihelia rather than allowing them to circularize at larger distances. Adding an ice-giant core modestly increases the outward reach (up to about 4 percent in the most gas-rich case), but Type-I migration further lowers perihelia, making long-term retention at large distances difficult. For a CM mass budget M_CM,tot about 1 M_Earth, this implies at most M_CM < 0.02-0.04 M_Earth reaches 15-25 au, corresponding to a diluted mass fraction < (1-2) x 10^-3 in the outer ring, hence negligible contamination of the CI reservoir. Combined with the distinct radial distributions of CM- and CI-like asteroids in the belt, these results imply limited mixing of carbonaceous reservoirs and isolation of the CI reservoir.

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 uses N-body integrations of 100 km planetesimals launched from the outer edge of Jupiter's gap, incorporating gas drag and perturbations from growing Jupiter and Saturn (with optional ice-giant embryo), to test outward implantation during Saturn's growth and migration. It reports that fewer than ~2% of CM-like bodies reach long-lived orbits beyond 15 au even under gas-rich conditions, because gas drag damps eccentricities and returns bodies to smaller perihelia; adding an ice-giant core raises this to ~4% at most, but Type-I migration hinders retention. For a total CM mass budget of ~1 M_Earth this implies at most 0.02-0.04 M_Earth reaches the 15-25 au region, yielding a diluted mass fraction <(1-2)×10^{-3} and thus negligible contamination of the CI reservoir.

Significance. If the implantation fractions hold, the work supplies quantitative limits on radial mixing between inner (CM) and outer (CI) carbonaceous reservoirs during giant-planet growth, reinforcing the interpretation that CM and CI chondrites sample distinct formation zones with limited cross-contamination. The forward N-body approach with explicitly stated initial conditions and drag prescriptions provides a reproducible basis for the <2% figure and the derived mass constraints.

major comments (2)
  1. [Methods / simulation setup] Simulation methods (gas-drag implementation): the headline result of <2% implantation beyond 15 au relies on the explored range of gas surface-density profiles and growth timescales, yet it is not shown that the weakest-drag end (lowest Σ or largest effective planetesimal size) was sampled at sufficient resolution to bound the upper implantation fraction; if weaker drag permits >5% retention at 15-25 au the M_CM <0.02-0.04 M_Earth limit and negligible-contamination conclusion would not hold for all plausible disks.
  2. [Results section] Results on ice-giant embryo runs: the modest increase to ~4% implantation is reported only for the most gas-rich case, but the subsequent effect of Type-I migration on perihelia is described qualitatively; quantitative statistics on final semi-major-axis and eccentricity distributions after migration are needed to confirm that long-term retention at large distances remains difficult.
minor comments (2)
  1. [Abstract] Abstract: the reported implantation percentages lack accompanying uncertainties, particle counts, or convergence tests, which would help readers assess statistical robustness of the <2% and ~4% figures.
  2. [Discussion] Notation: the mass budget M_CM,tot is introduced as ~1 M_Earth without an explicit reference to the source of this value or its uncertainty range.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their careful reading and constructive comments, which help strengthen the presentation of our results. We respond to each major comment below and indicate the revisions planned for the manuscript.

read point-by-point responses

  1. Referee: [Methods / simulation setup] Simulation methods (gas-drag implementation): the headline result of <2% implantation beyond 15 au relies on the explored range of gas surface-density profiles and growth timescales, yet it is not shown that the weakest-drag end (lowest Σ or largest effective planetesimal size) was sampled at sufficient resolution to bound the upper implantation fraction; if weaker drag permits >5% retention at 15-25 au the M_CM <0.02-0.04 M_Earth limit and negligible-contamination conclusion would not hold for all plausible disks.

    Authors: We thank the referee for this observation. Our parameter survey explicitly included the weakest-drag regime through the lowest gas surface densities (0.1×MMSN) and the 100 km planetesimal size, which minimizes the drag force. In these runs the implantation fraction beyond 15 au stayed below 2% (or ~4% with the ice-giant embryo), consistent with the headline result. To make the bounding of the upper limit fully transparent, we will add a supplementary figure showing implantation efficiency as a function of the effective drag parameter across the full range of Σ and growth timescales. This will confirm that even at the weakest drag the fraction remains well below 5%. revision: partial

  2. Referee: [Results section] Results on ice-giant embryo runs: the modest increase to ~4% implantation is reported only for the most gas-rich case, but the subsequent effect of Type-I migration on perihelia is described qualitatively; quantitative statistics on final semi-major-axis and eccentricity distributions after migration are needed to confirm that long-term retention at large distances remains difficult.

    Authors: We agree that quantitative distributions would strengthen the ice-giant embryo section. In the revised manuscript we will add a new figure (or panels to an existing figure) presenting the cumulative distributions of final semi-major axes and eccentricities for the embryo runs, both prior to and after Type-I migration. These statistics will show that the majority of bodies experience perihelion lowering sufficient to prevent stable retention beyond 15 au, thereby providing the requested quantitative support for the conclusion that long-term outward implantation remains inefficient. revision: yes

Circularity Check

0 steps flagged

No circularity: results are direct outputs of forward N-body integrations

full rationale

The paper derives its central claims (<2% implantation beyond 15 au, M_CM < 0.02-0.04 M_Earth) exclusively from explicit N-body simulations with stated initial conditions (100 km planetesimals at outer edge of Jupiter's gap), gas-drag prescriptions (Epstein/Stokes regimes), and a scanned parameter space of gas surface-density profiles plus growth timescales. No step defines a quantity in terms of its own output, renames a fitted parameter as a prediction, or relies on a self-citation chain for a uniqueness theorem or ansatz. The implantation statistics are computed quantities, not tautological re-expressions of the inputs.

Axiom & Free-Parameter Ledger

2 free parameters · 1 axioms · 0 invented entities

The central claim rests on the choice of 100 km planetesimal size, the range of gas surface-density profiles, and the growth timescales of Jupiter and Saturn as inputs that are varied but not derived from first principles.

free parameters (2)
  • gas surface-density profiles
    A range is explored but specific profiles are chosen as simulation inputs rather than derived.
  • growth timescales
    Jupiter and Saturn growth timescales are varied across runs as free parameters.
axioms (1)
  • standard math Newtonian N-body gravity plus standard aerodynamic gas drag on 100 km bodies
    Invoked throughout the integration setup without derivation.

pith-pipeline@v0.9.0 · 5652 in / 1352 out tokens · 79077 ms · 2026-05-15T13:03:38.266037+00:00 · methodology

discussion (0)

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