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arxiv: 2605.21407 · v1 · pith:7IWNU6UZnew · submitted 2026-05-20 · 🌌 astro-ph.SR · astro-ph.EP

Lithium Enrichment in a Subgiant Star with a Brown Dwarf Companion: A Planetary Engulfment Candidate

Brooke Kotten , Melinda Soares-Furtado , Ricardo Yarza , Andrew C. Nine , Seth A. Jacobson , Noah Vowell , Olivia Maynard , Allyson Bieryla
show 6 more authors
Andrew Vanderburg Jack Schulte Claudia Aguilera-Gomez Enrico Ramirez-Ruiz Joseph E. Rodriguez David W. Latham
This is my paper

Pith reviewed 2026-05-21 03:06 UTC · model grok-4.3

classification 🌌 astro-ph.SR astro-ph.EP
keywords lithium enrichmentsubgiant starplanetary engulfmentbrown dwarf companionstellar lithium abundanceTOI-5882exoplanet ingestion
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The pith

The lithium excess observed in subgiant star TOI-5882 can result from engulfing a planet with a mass between 9 and 95 Earth masses.

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

This paper tests whether a specific subgiant star with a close brown dwarf companion has retained lithium from swallowing a planet. The star shows lithium levels higher than nearly all comparable subgiants in a large survey. Calculations of how swallowed material would mix through the star's outer layers indicate that a relatively small planet, using realistic compositions from meteorites, supplies exactly the right amount of lithium. If correct, this provides a direct link between a star's chemical makeup and the history of its planetary system. Readers would care because it offers a method to detect past planets that have been destroyed as stars evolve.

Core claim

TOI-5882 exhibits a lithium equivalent width of 75.39 ± 3.58 mÅ and an abundance A(Li) = 2.49 ± 0.12 dex, ranking in the 98.4th percentile among 61 similar subgiants from the GALAH survey. Modeling the deposition of material into the convective zone shows that an engulfed mass of 9-95 Earth masses with CI chondritic lithium abundances reproduces the observed enhancement, which is an order of magnitude lower than estimates using solar abundances and consistent with a super-Earth to Neptune-mass planet.

What carries the argument

The convective zone deposition model combined with an assumption of CI chondritic lithium abundances in the engulfed planetary material, which is used to estimate the minimum mass needed to explain the lithium excess.

If this is right

  • Subgiants in a narrow mass range retain detectable lithium signatures from planetary engulfment.
  • The presence of a massive brown dwarf companion supports the dynamical perturbation needed to cause inner planet engulfment.
  • Lithium measurements can identify candidate planetary engulfment events in evolved stars.
  • The use of chondritic abundances yields more plausible planetary masses than proto-solar assumptions.

Where Pith is reading between the lines

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

  • Similar lithium excesses in other subgiants without known companions might also indicate engulfed planets.
  • This scenario could be tested by searching for other chemical anomalies expected from planetary material.
  • Models of stellar evolution might need to incorporate engulfment events more routinely to explain abundance patterns.

Load-bearing premise

The lithium abundance in the engulfed material is taken to match the levels found in CI chondrites rather than the star's birth composition or solar values.

What would settle it

If spectroscopic measurements or models of the star's convective zone mass show that the required engulfed mass falls well outside the 9-95 Earth mass range, the planetary engulfment explanation would not hold.

Figures

Figures reproduced from arXiv: 2605.21407 by Allyson Bieryla, Andrew C. Nine, Andrew Vanderburg, Brooke Kotten, Claudia Aguilera-Gomez, David W. Latham, Enrico Ramirez-Ruiz, Jack Schulte, Joseph E. Rodriguez, Melinda Soares-Furtado, Noah Vowell, Olivia Maynard, Ricardo Yarza, Seth A. Jacobson.

Figure 1
Figure 1. Figure 1: Color-magnitude diagram of TOI-5882 (yellow star) and our GALAH control sample of 61 stars (grey cir￾cles). MIST stellar tracks for 1.35 ± 0.05 M⊙ are overlaid, with [Fe/H] matching TOI-5882’s metallicity. The shaded region represents the [Fe/H] range of 0.33 ± 0.10 dex for 1.35 M⊙. The dotted line illustrates the location of the zero-age-main-sequence for a 0.33 dex population. Dashed segments indicate po… view at source ↗
Figure 2
Figure 2. Figure 2: Li I feature of TOI-5882 centered at 6707.8 ˚A, as seen in the co-added TRES spectra. Continuum is set at 1.0174 with measurement boundaries at 6707.30 ˚A and 6708.37 ˚A. We determined an Li I EW measurement of 93.83 ± 3.58 m˚A (not accounting for the Fe feature at 6707.4 ˚A). The Fe-corrected value is provided in [PITH_FULL_IMAGE:figures/full_fig_p006_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: Top Panel: Li I EW histogram of 61 GALAH control stars. TOI-5882 (dashed line at 75.39 ± 3.58 m˚A) is exceeded by only one control star, ranking in the 98.4th percentile. Bottom Panel: Control sample Li I EW values (color-coded circles) compared with TOI-5882 (star) in CMD space, showing TOI-5882 occupies typical subgiant CMD po￾sition while exhibiting extreme lithium enhancement. While our cross-validatio… view at source ↗
Figure 4
Figure 4. Figure 4: Lithium equivalent width distributions for three comparison samples constructed using tight, nominal, and loose constraints in color–magnitude space and Teff . In all cases, the distributions are strongly peaked at low Li I EW , while TOI-5882 lies in the extreme upper tail. The inferred percentile rank remains consistently high despite the change in sample size, demonstrating that the identification of TO… view at source ↗
Figure 5
Figure 5. Figure 5: Percentile rank of TOI-5882 as a function of the adopted selection window. Left: variation with color–magnitude (CMD) window width. Right: variation with Teff window width. The percentile rank remains above ∼95% across all tested configurations, peaking above ∼98% for intermediate window sizes. The modest decline at large CMD widths reflects the inclusion of less well-matched comparison stars, while the Te… view at source ↗
Figure 6
Figure 6. Figure 6: Left: Comparison of the Li I 6707.8 ˚A region for TOI-5882 (gold) and four representative control stars (colored), spanning a range of Li I EW values. The enhanced depth of the Li feature in TOI-5882 is directly evident in the normalized spectra. The control star with the strongest Li absorption provides a close match to the line depth, with Li I EW consistent within measurement uncertainties, while the re… view at source ↗
read the original abstract

Theoretical models predict that subgiants within a narrow mass regime can retain detectable lithium enrichment signatures from planetary engulfment. We test this prediction using TOI-5882, selected because it occupies this favorable subgiant parameter space and hosts a massive brown dwarf ($22 \, M_{ \rm J}$, $P=7.1 \,{\rm d}$) companion capable of dynamically perturbing inner planets. We investigate whether: (1) TOI-5882 exhibits lithium enhancement among similar subgiants, (2) planetary material would be deposited in the convective zone, and (3) the required engulfed mass lies within a plausible range for planetary engulfment. Using spectra from the Tillinghast Reflector Echelle Spectrograph, we measured a Li I equivalent width of $75.39 \pm 3.58$ mA and an abundance of A(Li) $=2.49 \pm 0.12$ dex. Comparing these values to a control sample of 61 subgiants from the GALactic Archaeology with HERMES (GALAH) DR4 survey, we find that TOI-5882 ranks in the 98.4th percentile in both metrics, confirming significant lithium enrichment. We evaluate the engulfment scenario by modeling convective zone deposition and estimating the mass required to reproduce the observed enhancement relative to the control sample. We perform an estimate of the engulfed planetary mass incorporating CI chondritic Li abundances, as planets formed via core accretion are enriched in heavy elements and lithium partitions with these metals. This yields a required engulfed mass of $9$-$95\,M_\oplus$--an order of magnitude lower than the $5.6 \, M_{\rm J}$ implied by proto-solar assumptions. TOI-5882's lithium excess can plausibly result from the ingestion of a super-Earth to Neptune-mass planet, motivating further studies to test this scenario.

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 paper reports that the subgiant TOI-5882, which hosts a 22 M_J brown dwarf on a 7.1-day orbit, shows significant lithium enrichment. From TRES spectra the authors measure an equivalent width of 75.39 ± 3.58 mÅ and A(Li) = 2.49 ± 0.12 dex; these values place the star in the 98.4th percentile of a 61-star GALAH DR4 control sample of similar subgiants. Convective-zone deposition modeling combined with an assumed CI-chondritic lithium abundance in the engulfed material yields a required planetary mass of 9–95 M_⊕, which the authors argue is consistent with ingestion of a super-Earth to Neptune-mass body and therefore supports TOI-5882 as a planetary-engulfment candidate.

Significance. If the enrichment interpretation holds, the work supplies a concrete observational test of theoretical predictions that subgiants in a narrow mass range can retain detectable lithium signatures from planetary engulfment. The direct spectroscopic measurement, the percentile ranking against an independent control sample, and the quantitative mass estimate (even under stated assumptions) constitute a falsifiable prediction that can be checked with additional observations or refined models.

major comments (2)
  1. [Section 4] Engulfed-mass estimation (Section 4): the reported 9–95 M_⊕ range is obtained only after adopting CI-chondritic lithium mass fraction for the planetary material. The manuscript provides no independent constraint on the planet’s actual Li content; if the fraction is lower (as expected for formation beyond the snow line or different differentiation), the required mass scales upward proportionally and could exceed the range dynamically plausible given the 22 M_J brown-dwarf companion. This assumption is load-bearing for the claim that engulfment remains viable.
  2. [Section 3.3] Convective-zone deposition calculation (Section 3.3): the paper states that lithium from the engulfed body is fully mixed into the convective zone, but does not quantify the sensitivity of the final mass estimate to the adopted convective-zone mass or to possible dilution factors. A brief exploration of these parameters would strengthen the robustness of the 9–95 M_⊕ interval.
minor comments (2)
  1. [Section 2.2] The control-sample selection criteria (Section 2.2) are described only at a high level; adding a short table or explicit cuts on T_eff, log g, and [Fe/H] would improve reproducibility.
  2. [Figure 3] Figure 3 (lithium abundance vs. control sample) would benefit from error bars on the comparison points and a clearer indication of the percentile ranking.

Simulated Author's Rebuttal

2 responses · 1 unresolved

We thank the referee for their careful reading and valuable comments on our manuscript. We have made revisions to address the concerns about the assumptions in the mass estimation and to provide additional sensitivity analysis. Our responses to the major comments are detailed below.

read point-by-point responses

  1. Referee: [Section 4] Engulfed-mass estimation (Section 4): the reported 9–95 M_⊕ range is obtained only after adopting CI-chondritic lithium mass fraction for the planetary material. The manuscript provides no independent constraint on the planet’s actual Li content; if the fraction is lower (as expected for formation beyond the snow line or different differentiation), the required mass scales upward proportionally and could exceed the range dynamically plausible given the 22 M_J brown-dwarf companion. This assumption is load-bearing for the claim that engulfment remains viable.

    Authors: We acknowledge that the CI-chondritic lithium abundance is a key assumption in deriving the 9–95 M_⊕ range, and that no direct measurement of the engulfed material's composition is possible with the current dataset. In the revised manuscript, we have added explicit discussion in Section 4 noting that the required mass scales inversely with the lithium mass fraction in the planet. We argue that CI-chondritic values are appropriate because planets formed by core accretion are expected to be enriched in refractories, and lithium is known to partition with metals in such bodies. We have also included a brief exploration of lower lithium fractions (e.g., 0.5× CI), showing that the mass could increase to ~20–190 M_⊕, which remains within the range of plausible Neptune-mass planets that could be dynamically influenced by the brown dwarf companion. We believe this strengthens rather than undermines the engulfment candidate status. revision: yes

  2. Referee: [Section 3.3] Convective-zone deposition calculation (Section 3.3): the paper states that lithium from the engulfed body is fully mixed into the convective zone, but does not quantify the sensitivity of the final mass estimate to the adopted convective-zone mass or to possible dilution factors. A brief exploration of these parameters would strengthen the robustness of the 9–95 M_⊕ interval.

    Authors: We agree that quantifying the sensitivity to convective zone mass and dilution would improve the robustness of our results. In the revised Section 3.3, we now include a sensitivity study varying the convective zone mass by factors of 0.8 to 1.2 based on stellar evolution models for subgiants of similar mass and metallicity. Additionally, we consider dilution factors from 1.0 (full mixing) to 1.5 (partial dilution). The resulting engulfed mass range broadens to 8–110 M_⊕, which does not change our conclusion that a super-Earth to Neptune-mass planet is sufficient to explain the observed lithium enrichment. These additions are presented in a new subsection and a supplementary figure showing the parameter dependence. revision: yes

standing simulated objections not resolved
  • We cannot provide an independent observational constraint on the lithium content of the hypothetical engulfed planet, as this would require direct sampling or advanced atmospheric characterization not available for this system.

Circularity Check

0 steps flagged

No significant circularity: enhancement from external survey comparison; mass estimate uses independent compositional assumption

full rationale

The paper establishes lithium enhancement via direct measurement of A(Li) and equivalent width, then ranks TOI-5882 against an independent GALAH DR4 control sample of 61 subgiants, placing it in the 98.4th percentile. This comparison is external and not derived from the paper's own modeling. The engulfed-mass calculation (9-95 M_earth) proceeds by forward-modeling convective-zone deposition and applying an external assumption of CI chondritic Li abundance justified by core-accretion theory; the observed excess is not used to fit or define the abundance, nor is the mass presented as a fitted prediction. No self-citations, uniqueness theorems, or ansatzes from prior author work are invoked as load-bearing steps. The derivation chain remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 1 axioms · 0 invented entities

The claim rests on the assumption that lithium partitions with heavy elements in core-accretion planets and on the use of CI chondritic abundances to convert observed excess into engulfed mass; no new entities are postulated.

free parameters (1)
  • Engulfed planetary mass
    Calculated range of 9-95 M_earth obtained by scaling observed lithium excess against assumed chondritic lithium content and convective zone deposition efficiency.
axioms (1)
  • domain assumption Lithium partitions with heavy elements in planets formed via core accretion, justifying use of CI chondritic abundances for engulfed material
    Invoked to convert the observed lithium excess into an engulfed mass estimate after convective zone modeling.

pith-pipeline@v0.9.0 · 5951 in / 1356 out tokens · 56709 ms · 2026-05-21T03:06:56.399923+00:00 · methodology

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