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Assessing the processes behind planet engulfment and its imprints

T0 review · 2 major / 5 minor · reviewed 2026-08-12 · deepseek-v4-flash

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Pith's one-line read Planet engulfment leaves detectable chemical traces in at most 20% of Sun-like stars.

desk verdict Useful population-synthesis estimate of observable planet engulfment, but the headline ≤20% upper bound is undercut by the paper's own admission that cumulative multi-event engulfment was not modeled. read the letter →

arxiv 2411.13455 v1 pith:3PIK7CAO submitted 2024-11-20 astro-ph.EP astro-ph.SR

B. M. T. B. Soares , V. Adibekyan , C. Mordasini , M. Deal , S. G. Sousa , E. Delgado-Mena , N. C. Santos , C. Dorn This is my paper · ORCID
classification astro-ph.EPastro-ph.SR
keywords planetengulfmentstellarchemicalcompositionpopulationsynthesisBernmodelconvectiveenvelopedilutionSun-likestarsexoplanetarysystemsabundanceanomalies
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper asks how often a star that swallows a planet shows it, and what fraction of Sun-like stars carry a detectable chemical scar from planet engulfment. Combining a population synthesis of 1000 planetary systems with stellar evolution models that track how the convective envelope dilutes accreted material, the authors find that most engulfment events are chemically invisible. Events occurring while the protoplanetary disk is still present are fully diluted, and even later events leave a signal that fades over gigayears. Under an optimistic detection threshold of 0.02 dex in $[\mathrm{Fe/H}]$, the rate of systems with a detectable imprint is no higher than 20%; under a more conservative threshold of 0.06 dex it is far smaller. The paper concludes that observable planet engulfment is rare.

What carries the argument

The argument is carried by two coupled models: the Generation III Bern model (NGPPS) provides 1000 synthetic Sun-like planetary systems with full formation and evolution histories and the masses and compositions of engulfed planets, while the Cesam2k20 stellar evolution code converts those events into surface abundance variations by modeling convective-envelope dilution, atomic diffusion, and thermohaline mixing. The key physical quantity is the mass of the convective envelope at the time of accretion: a thick convective layer (early on) dilutes the signal to nothing, while a thin, shrinking convective layer (later in the main sequence) preserves a measurable $[\mathrm{Fe/H}]$ bump. The paper's threshold analysis then maps simulated events onto observability, using 0.02 dex (optimistic) and 0.06 dex (conservative) detection limits.

What would settle it

A homogeneous spectroscopic survey of co-natal Sun-like binary pairs with ages above 3 Gyr that finds chemically anomalous pairs ($\Delta[\mathrm{Fe/H}] > 0.02$ dex) at a rate above about 20% (or above about 11% for anomalies large enough to require >10 $M_\oplus$ events) would contradict the paper's central claim. Conversely, the claim would be strengthened by confirming that younger (<1 Gyr) stars show a higher incidence of engulfment signatures than older stars of the same mass.

Watch

Extended reading notes

Core claim

The central claim is that planet engulfment leaves a detectable chemical imprint on a Sun-like star's surface only under narrow conditions: the event must happen after disk dissipation, the engulfed body must be massive enough (roughly ≥5–10 $M_\oplus$), and the star must be young enough (or the event recent enough) that internal mixing has not erased the signal. Using the NGPPS sample from the Generation III Bern model, the authors identify three engulfment phases—disk migration (0–10 Myr), dynamical interactions (10–100 Myr), and tidal forces (100 Myr–10 Gyr)—and show that systems born from more massive, more metal-rich disks are more likely to engulf planets. Feeding the composition of engulfed planets (refractory-rich) into Cesam2k20 stellar models, they show that convective dilution and thermohaline/atomic diffusion erase the imprint within a few gigayears for all but the most massive engulfed planets. They therefore revise the often-cited engulfment rate of about 27% down to at most 20% in the optimistic case, with the detectable fraction driven by the mass of the engulfed planet and the age of the star.

Load-bearing premise

The result depends on the Bern model turning off dynamical interactions between planets at 100 Myr, so that all later engulfment is driven by tides; if real systems keep undergoing dynamical instabilities at gigayear ages, the timing, masses, and rates of late engulfment, and therefore the detectable fraction, could change.

Editorial extensions

If this is right

  • Most engulfment happens early and involves low-mass planets, so it is chemically invisible; the majority of the 529 systems that engulf planets would not be identifiable by abundance anomalies.
  • Detectable events require engulfment of at least roughly 5–10 $M_\oplus$ after about 60 Myr, and even then the signature fades below 0.02 dex within about 1–3 Gyr.
  • Systems with giant planets, born from massive and metal-rich disks, are the most likely to show engulfment signatures, giving a target population for observational searches.
  • The apparent 20–35% engulfment rate inferred from binary abundance differences overestimates the true observable rate; stellar age and internal mixing must be folded in.
  • The composition of engulfed material is refractory-enriched (Mg, Si, Fe) while surviving planets are water and volatile-rich, so engulfment imprints should be most visible in iron and refractory element abundances.

Reading between the lines

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

  • If the model's tidal-only late phase is too restrictive, the true rate of heavy late engulfment could be higher; a testable extension is to inject late dynamical instabilities into the population synthesis and recompute the observable fraction.
  • The same machinery applied to hotter stars, which have thinner convective envelopes, would predict higher detectable engulfment rates, making early-type stars a promising place to look for chemical scars.
  • The paper's composition model treats ices as pure water and silicates with a fixed Earth-like Mg/Si ratio; refining this with realistic ice mixtures and varied silicate stoichiometry could change the predicted [Mg/Si] and [O/H] signatures, which are observable diagnostics.
  • Because engulfed-planet material is refractory-rich, the $[\mathrm{Fe/H}]$ signal is likely accompanied by correlated [Mg/H], [Si/H], and possibly reduced [O/H]—a pattern that could distinguish engulfment from primordial abundance variations.
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Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. The paper combines the NGPPS Generation III Bern model population synthesis (1000 Sun-like systems) with Cesam2k20 stellar models to estimate the fraction of systems whose surface [Fe/H] would show a detectable enhancement after planet engulfment. It identifies three engulfment phases (disk migration, dynamical interactions, tidal forces), characterizes the masses and compositions of engulfed planets, and uses nine representative cases (2, 5, and 10 M_Earth at 8 Myr, 60 Myr, and 4.5 Gyr) to compute the time evolution of the resulting [Fe/H] perturbation. The headline result is an upper bound of 20% for Sun-like stars with detectable traces under an optimistic 0.02 dex threshold, with lower rates under a 0.06 dex threshold.

Significance. If the upper bound is secure, this is an important result: it would reconcile population-synthesis predictions with recent observational estimates (e.g., Behmard et al.; Liu et al. 2024) and sharpen the interpretation of the higher rate reported by SP21. The analysis is largely transparent: the detectability thresholds are taken from SP21 rather than fitted from the model, the stellar-structure processes are modeled with an established code, and the authors openly list the main model caveats. However, because the headline is stated as an upper bound, the acknowledged omission of cumulative multi-event signatures and the model's termination of dynamical interactions at 100 Myr need to be addressed before the claim can be accepted as stated.

major comments (2)
  1. [§7 (Discussion) and Table 4] The abstract's upper bound "no higher than 20%" is undercut by an omission that the manuscript itself acknowledges in §7: "we did not model each individual engulfment event for each system, even though the cumulative effect of multiple engulfment events could be greater." Section 3.2 states that the multiplicity of engulfment events can range from one to thirty. Table 4, however, counts systems with at least one engulfment event above a given mass threshold (2, 5, or 10 M_Earth) after a given age, so a system that engulfs three 4 M_Earth planets near 4 Gyr would not appear in the M>10 rows, even though the combined enhancement could be comparable to a single 10 M_Earth event, which Table 3 shows remains detectable for several Gyr. Because the omitted channel can only increase the detectable fraction, the reported ≤20% is not a secure upper bound as stated. I request either modeling the cumulative per-system mass before applying the stellar dilution models, or reformulating the conclusion as an upper bound for single-event engulfment with an explicit estimate of the multi-event correction.
  2. [§3.1 (Timing of planet engulfment) and Tables 3–4] The post-100 Myr phase, which is the phase whose events can produce long-lived detectable imprints, is computed with dynamical interactions between planets switched off; §3.1 states this explicitly and notes that the model output "needs to be carefully considered" at that point. Late events in the model therefore come only from tidal effects. If real systems still experience dynamical instabilities at late times, additional late engulfments would occur, and since Table 3 shows that late events are the ones that remain observable, the detectable rate would be higher than the model's. The manuscript should either justify the switch-off as a complete description after 100 Myr or present the ≤20% bound as conditional on this model choice and test the sensitivity to the presence of a late instability channel.
minor comments (5)
  1. [§4.2 (Machine Learning approach)] The ML section reports 88% classification accuracy but does not state the test-set size, the split strategy, or the cross-validation protocol; adding these details would make the result reproducible and interpretable.
  2. [§5, Eq. (2)] The notation m_X = α·n_Y×M_X is ambiguous; please define α, n_Y, and M_X explicitly and check the dimensional consistency of the expression, since the current printed form is hard to follow.
  3. [Table 3] The columns labeled σ[Fe/H] with entries "yes"/"no" could be misread as uncertainties; consider renaming them "Detectable at 0.02 dex?" and "Detectable at 0.06 dex?" to clarify that 0.02 and 0.06 are thresholds rather than measurement errors.
  4. [§6 (Stellar models)] The value α_CGM = 9183 in the solar-calibrated convection sentence is surprising and currently unexplained; please check whether this is a typo and, if not, provide a reference or a brief justification.
  5. [Figure 9] With three colors and three line styles, the curves for the 60 Myr and 4.5 Gyr groups are difficult to distinguish in print; consider labeled curves or a legend with direct mass labels for each case.

Circularity Check

0 steps flagged · score 2.0 of 10

No significant circularity: the ≤20% rate is obtained by chaining independent Bern-model population synthesis, Cesam2k20 stellar-structure models, and externally adopted SP21 detectability thresholds.

full rationale

The paper's central claim, that no more than 20% of Sun-like stars show observable engulfment signatures under a 0.02 dex threshold, is obtained by combining two independent model outputs rather than by reusing a fitted quantity. The Bern NGPPS population synthesis provides the distribution of engulfment masses and times (Section 3, Figures 1-5, Table 1), and the Cesam2k20 stellar models provide the surface [Fe/H] response for the nine representative cases (Section 6, Figure 9, Table 3). The detectability thresholds (0.02 and 0.06 dex) are taken from the external SP21 work, not derived from the model, and the mass and time cutoffs in Table 4 are applied to the simulated population, not fitted to produce the final 20% number. The Bern model and Cesam2k20 are developed or co-developed by authors of this paper, but they are externally published, benchmarked codes with stated assumptions that do not include the target result, so this self-citation is not load-bearing in a circular sense. The paper's own admission that it 'did not model each individual engulfment event for each system, even though the cumulative effect of multiple engulfment events could be greater' (Section 7) is a genuine one-sided modeling limitation: including cumulative multi-event effects could only raise the observable fraction and therefore weaken the security of the 'no higher than 20%' upper bound. That is a robustness concern, not circularity: no parameter is defined in terms of the predicted rate, and no load-bearing premise reduces by construction to the conclusion. Accordingly, no specific circular step is exhibited.

Assumptions & free parameters 5 free parameters · 4 assumptions · 0 invented entities

The analysis rests on two large pre-existing simulation frameworks (Bern NGPPS and Cesam2k20) and on the paper's chosen composition simplifications. No new physical entities are introduced. The free parameters and domain assumptions listed above are the main things the reader must accept to trust the 20% upper bound.

free parameters (5)
  • turbulent diffusion reference depth log(T0) = 6.44
    Calibrated so a solar model reproduces the solar lithium surface abundance (Section 6); this calibration sets the dilution timescale used to estimate how long engulfment signatures survive.
  • turbulent diffusion amplitude omega = 400
    Chosen constant in the D_turb prescription (Eq. 4); directly controls the rate at which engulfed material is mixed below the surface.
  • turbulent diffusion density exponent n = 3
    Chosen exponent in Eq. 4; together with omega and log(T0) it sets the dilution of the engulfment signal.
  • accretion dilution timescale = 1 Myr
    Assumed instantaneous dilution of accreted material over 1 Myr (Section 6); the timescale affects the peak [Fe/H] variation after engulfment.
  • minimum detectable [Fe/H] variation = 0.02 and 0.06 dex
    Taken from SP21 as optimistic and conservative detection thresholds; not fitted here but a key input that defines the reported rate upper limit.
assumptions (4)
  • domain assumption The Generation III Bern model accurately simulates the formation and evolution of planetary systems, including migration, dynamical interactions, and tides.
    The entire population statistics and event timing come from NGPPS (Section 2); the paper inherits all model assumptions without independent validation of the engulfment rate.
  • domain assumption The Cesam2k20 stellar models with the specified input physics reproduce the dilution of engulfed material in real Sun-like stars.
    Section 6 uses these models to convert engulfment events into [Fe/H] variations; the accretion prescription and calibrated transport coefficients are assumed physical.
  • ad hoc to paper Planetary ices are composed only of water; silicates follow a fixed MgSiO3/Mg2SiO4 mix; atmospheres are 76% H and 24% He.
    Section 5 uses these simplifications to convert simulated core and atmosphere masses into element masses; the assumed stoichiometry directly sets the [Fe/H] signal.
  • domain assumption The initial disk mass, metallicity, and lifetime distributions of the 1000 systems are representative of Sun-like stars in the solar neighborhood.
    Section 2 defines the distributions; if the real population differs, the engulfment rates in Tables 1 and 4 would differ.

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Pith. "Pith review of Assessing the processes behind planet engulfment and its imprints." pith.science (2026). https://pith.science/paper/3PIK7CAO

@misc{pith2026241113455,
  author       = {Pith},
  title        = {Pith review of: Assessing the processes behind planet engulfment and its imprints},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/3PIK7CAO}},
  note         = {Machine review of arXiv:2411.13455}
}
abstract

Throughout a planetary system's formation evolution, some of the planetary material may end up falling into the host star and be engulfed by it, leading to a potential variation of the stellar composition. The present study explores how planet engulfment may impact the chemical composition of the stellar surface and discusses what would be the rate of events with an observable imprint, for Sun-like stars. We use data from the NGPPS calculations by the Generation III Bern model to analyse the conditions under which planet engulfment may occur. Additionally, we use stellar models computed with Cesam2k20 to account for how the stellar internal structure and its processes may affect the dilution of the signal caused by planet engulfment. Our results show that there are three different phases associated to different mechanisms under which engulfment events may happen. Moreover, systems that undergo planet engulfment are more likely to come from protoplanetary disks that are more massive and more metal-rich than non-engulfing systems. Engulfment events leading to an observable signal happen after the dissipation of the protoplanetary disk when the convective envelope of the stars becomes thinner. With the stellar convective layer shrinking as the star evolves in the main sequence, they display a higher variation of chemical composition, which also correlates with the amount of engulfed material. By accounting for the physical processes happening in the stellar interior and in the optimistic case of being able to detect variations above 0.02 dex in the stellar composition, we find an engulfment rate no higher than $20\%$ for Sun-like stars that may reveal detectable traces of planet engulfment. Engulfment events that lead to an observable variation of the stellar composition are rare due to the specific conditions required to result in such signatures.

Figures

Figures reproduced from arXiv: 2411.13455 by the authors.

Figure 1
Figure 1. Percentage of systems with at least one engulfment event, for the 10 Gyr. The first transition at 5 × 106 yr marks the first change and is close to the average lifetime of the protoplanetary disks in the simulation (∼ 4 Myr). During this period, disk migration is the main process responsible for the engulfment of planetary mate￾rial. The presence of the disk leads to planets gradually migrat￾ing closer to the star w… view at source ↗
Figure 2
Figure 2. Number of engulfment events at different points in time over 10 Gyr, in logarithmic scale. The solid line represents the KDE of the distribution [PITH_FULL_IMAGE:figures/full_fig_p004_2.png] view at source ↗
Figure 4
Figure 4. Average mass engulfed by the star per event, for each system. The solid line represents the KDE of the distribution. ond around higher amounts (∼ 5 M⊕). The wide range of masses corresponds to different type of planets engulfed. 3.3. Planet engulfment across time and mass The simultaneous analysis of the mass of engulfed material and the point in time when these events happen allows to better un￾derstanding processe… view at source ↗
Figures from the paper (5 more)
Figure 5
Figure 5. Figure 5: 2D histogram representing the timing and amount of material engulfed by the central star, for 1000 systems and across 10 Gyr. loses some of its angular momentum in its orbital motion around the star into the spin of the host (see Emsenhuber et al. 2021a for a detailed …
Figure 6
Figure 6. Figure 6: Initial conditions of the protoplanetary disk, for engulfing and non-engulfing systems. We show the initial mass of solids (planetesimals) in the disk (top left), and initial mass of gas disk (top right). On the bottom, we show metallicity (bottom left) and disk lifeti…
Figure 7
Figure 7. Figure 7: Total mass engulfed depending on initial conditions of the disk, for engulfing systems. perience engulfment. For instance, more than 90% of systems with a massive planet (M > 30 M⊕) and minimum orbital dis￾tances of a > 0.3 AU undergo engulfment during their evolu￾tion…
Figure 8
Figure 8. Figure 8: Fraction of systems with engulfment depending on the maximum planetary mass within the system at 10 Gyr, the minimum orbital distance of planets at 10 Gyr, the disk lifetime, initial metallicity, and the initial mass of planetesimals in the disk, in linear scale (blue)…
Figure 9
Figure 9. Figure 9: Variation of iron abundance on the stellar surface due to an en￾gulfment event occurring at 8 Myr (blue), 60 Myr (orange) or 4.5 Gyr (green). Included are the cases for an engulfed planet with mass of 2 M⊕ (solid line), 5 M⊕ (dashed line) or 10 M⊕ (dotted line) The bla…

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