Pith. sign in

REVIEW 2 major objections 5 minor 34 references

Planet engulfment can explain TOI-5882's lithium, but only under uncommon timing and orbits.

Reviewed by Pith at T0; open to challenge. T0 means a machine referee read the full paper against a public rubric. the ladder, T0–T4 →

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

T0 review · grok-4.5

2026-07-11 05:42 UTC pith:XQGXNT76

load-bearing objection Solid system-specific N-body+MESA test: engulfment is common overall but rare (~5%) inside the Li window under a frozen BD orbit, so the Kotten scenario stays viable but non-generic. the 2 major comments →

arxiv 2607.05566 v1 pith:XQGXNT76 submitted 2026-07-06 astro-ph.EP astro-ph.SR

Dynamical constraints on planet engulfment as the origin of lithium enhancement in TOI-5882

C. Charalambous , C. Aguilera-G\'omez , S. Urrutia , C. Norambuena This is my paper
classification astro-ph.EP astro-ph.SR
keywords planet engulfmentlithium enhancementsubgiant starsbrown dwarfsN-body dynamicsstellar evolutionTOI-5882
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

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

TOI-5882 is a lithium-rich subgiant with a close-in brown dwarf. Earlier work suggested that swallowing a super-Earth to Neptune-mass planet could have raised its surface lithium. This paper tests whether that story is dynamically possible. The authors couple stellar-evolution tracks to N-body integrations that include the star's changing mass, radius and tides, and they sample hundreds of plausible masses and periods for a hypothetical inner planet. Engulfment itself is common, yet only a few percent of the runs place the engulfment inside the brief evolutionary window when the resulting lithium excess would still be observable. Recent engulfment therefore cannot be ruled out, but under the simplified architecture they explore it is a non-generic outcome that needs tighter constraints on the system's earlier configuration.

Core claim

Across 300 simulations that span the mass and period ranges suggested for a pre-engulfment planet, planet engulfment is the most probable outcome overall, yet only about 5 percent of the runs produce engulfment inside the short lithium-detectability window (roughly 4.23–4.61 Gyr). Thus recent engulfment remains a viable but uncommon explanation for the observed lithium enhancement under the simplified architecture considered.

What carries the argument

MESA stellar tracks interpolated into REBOUND N-body integrations (with REBOUNDx tides and time-dependent stellar mass, radius and Love number) that evolve an inner planet plus the observed brown dwarf while the star leaves the main sequence; outcomes are timed against the narrow convective-envelope window in which accreted lithium would remain detectable.

Load-bearing premise

The brown dwarf is fixed at its currently observed short-period orbit and wind drag is omitted, so the reported 5 percent fraction is conditional on that frozen architecture and force model.

What would settle it

Additional chemical tracers of planetary material, or tighter constraints on the brown dwarf's earlier orbit and the system's primordial architecture, that either place a recent engulfment inside the lithium window or show that no such planet could have survived long enough to be swallowed then.

Watch this falsifier — get emailed when new claim-graph text bears on it.

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

2 major / 5 minor

Summary. The paper tests whether the lithium enhancement of the subgiant TOI-5882 can be explained by recent engulfment of a super-Earth to Neptune-mass planet, as suggested by Kotten et al. (2026). Combining a MESA track for a 1.3 M⊙, [Fe/H]=0.33 star with REBOUND/REBOUNDx N-body integrations (IAS15, equilibrium-tide constant-time-lag model with envelope-dependent Love number), the authors run 300 simulations of a system containing the observed 22 m_Jup brown dwarf (P=7.1 d, e=0.0339) plus a randomly drawn interior planet (mass 9–95 m⊕, period 0.5–3.5 d). They define a lithium-detectability window from the stellar models (4.23–4.61 Gyr) during which accreted material can produce an observable surface A(Li) excess. Planet engulfment is the most common outcome overall (~65%), but only ~5% of runs produce engulfment inside that window; the authors therefore conclude that recent engulfment remains viable but non-generic under the simplified single-interior-planet architecture explored.

Significance. The work supplies a concrete dynamical test of an externally proposed chemical scenario for a specific system, rather than a generic population statement. Strengths include a carefully defined MESA-based detectability window, self-consistent coupling of time-dependent stellar mass/radius/luminosity and tides into the N-body runs, and an explicit scoping of the ~5% figure as a fraction of explored initial conditions rather than a posterior probability for TOI-5882. The result is useful for the growing literature on planet engulfment and Li-rich subgiants: it shows that timing, not merely the occurrence of engulfment, is the binding constraint, and it flags the need for better primordial-architecture constraints and additional forces (e.g., wind drag). The caveats on frozen BD orbit and omitted physics are already stated in the Discussion, which keeps the claim appropriately limited.

major comments (2)
  1. Discussion (and Methods setup): The integrations initialize the brown dwarf at its currently observed post-MS orbit and omit both secular main-sequence tidal decay and wind-induced drag. The paper itself cites Narayan et al. (2026) for continued orbital decay on ~25–125 Myr timescales and notes that wind drag was not included. Because the Li-window fraction is the central quantitative result, the manuscript should either (i) add a small set of exploratory runs with a modestly wider/closer initial BD period (or a simple drag term) to show how the ~5% figure moves, or (ii) elevate the existing qualitative caveat into a quantitative bound (e.g., order-of-magnitude estimate of how much the window fraction could change). Without that, the load-bearing claim remains conditional on an architecture that the authors acknowledge is transient.
  2. Results / Fig. 3 and Appendix B: The reported ~5% (and ~65%) fractions are raw counts over a uniform random draw in mass and period that deliberately spans both Hill-unstable and Hill-stable regimes. The paper correctly states that this is not a probability for TOI-5882, yet the abstract and conclusions still present “only 5%” as the headline number. A short reweighting or stratified reporting (e.g., fraction among runs that remain stable until the subgiant branch, or among runs with Δ_H ≳ 5) would make the non-generic character of successful cases clearer and less sensitive to the arbitrary prior volume. This is a presentation-of-result issue that affects how the central claim is read, not a flaw in the integrations themselves.
minor comments (5)
  1. Fig. 1 bottom panel and Appendix A: The post-engulfment A(Li) track is described as a post-processing instantaneous-mixing model. A one-sentence statement of the assumed accreted Li mass (or reference to the Kotten et al. budget used) would make the green detectability cutoff fully reproducible.
  2. Fig. 3 caption: The blue and green dashed stability lines are defined in Appendix B; a brief parenthetical in the caption (Δ_H ~ 2√3 and Δ_H = 5) would help readers who do not immediately turn to the appendix.
  3. Methods: The stellar tidal Love number is said to follow Becker & Batygin (2013) and to vary with the convective envelope. A short note on whether the planet and BD Love numbers/tidal quality factors are held fixed would complete the force-model description.
  4. Throughout: Occasional typographical inconsistencies (e.g., “offthe”, “m Jup” spacing, “V owell”) should be cleaned in production.
  5. Conclusions: The suggestion to measure additional chemical tracers is valuable; naming one or two concrete species (e.g., Be, refractory-to-volatile ratios) would strengthen the observational outlook paragraph.

Circularity Check

0 steps flagged

No significant circularity: the ~5% Li-window engulfment fraction is an independent output of the N-body ensemble, not forced by definition, fit, or self-citation.

full rationale

The paper tests an external hypothesis (Kotten et al. 2026 Li budget and suggested super-Earth–Neptune engulfment) by combining MESA stellar tracks with 300 REBOUND N-body runs that sample planet mass/period/eccentricity/inclination ranges motivated by that hypothesis. The detectability window (4.23–4.61 Gyr) is defined from the models’ convective-envelope onset and A(Li) dilution/burning curves; the reported ~65% overall engulfment and <5% in-window fractions are direct counts of simulation outcomes under those fixed initial conditions. No parameter is fitted to the target Li signature and then re-presented as a prediction; no uniqueness theorem or ansatz is imported from the authors’ prior work to force the result; self-citations (Aguilera-Gómez et al. 2016, 2020) supply only background Li-abundance context and are not load-bearing for the dynamical fractions. The Discussion explicitly scopes the claim as conditional on the simplified single-interior-planet architecture and the frozen post-MS BD orbit, confirming the derivation is self-contained numerical exploration rather than circular redefinition.

Axiom & Free-Parameter Ledger

5 free parameters · 5 axioms · 1 invented entities

The central claim rests on standard stellar-evolution and N-body machinery plus domain choices that define the explored prior (planet mass/period window, fixed present-day BD orbit, equilibrium-tide model, and the MESA-derived Li detectability ages). No new physical entities are invented; the putative planet is a hypothesis inherited from Kotten et al. Free parameters are mostly sampling ranges and stellar-model knobs rather than fits to the Li data themselves.

free parameters (5)
  • Inner-planet mass sampling range = [9, 95] m_earth
    Uniform draw over 9–95 m⊕ taken from Kotten et al. Li budget; the reported 5% fraction depends on this prior.
  • Inner-planet period sampling range = [0.5, 3.5] days
    Uniform draw over 0.5–3.5 days chosen to span Hill-stable and unstable separations relative to the BD; changes the mix of early ejections vs late engulfments.
  • Planet eccentricity and inclination priors = e~1e-4–1e-3; |i|≤1°
    Near-circular, near-coplanar draws e in [1e-4, 1e-3], i in [-1°, 1°]; affect scattering pathways.
  • MESA mixing-length, overshooting, Reimers efficiency = α_MLT=1.73; f=0.016; η=0.1
    α_MLT=1.73, f_ov=0.016, Reimers η=0.1 set the track, convective-envelope growth, and thus the 4.23–4.61 Gyr Li window.
  • Stellar tidal Love number prescription = Becker & Batygin (2013) envelope-dependent k
    Computed following Becker & Batygin (2013) and allowed to vary with the convective envelope; controls orbital decay strength, which the authors note may under/overestimate true tides.
axioms (5)
  • domain assumption Equilibrium-tide constant-time-lag model (Hut 1981) adequately captures post-MS tidal evolution for both planet and BD.
    Invoked via REBOUNDx throughout Methods; authors explicitly note tidal dissipation in evolved stars remains uncertain.
  • domain assumption Li delivered by an engulfed 9–95 m⊕ planet is instantaneously mixed in the surface convective envelope and then destroyed under the same burning that sets the baseline A(Li) track.
    Appendix A post-processing model and bottom panel of Fig. 1 define the detectability window used to count ‘successful’ runs.
  • ad hoc to paper The currently observed BD orbit can be used as the initial post-MS condition for the ensemble (neglecting prior MS tidal decay and wind drag).
    Methods initialize P_BD=7.1 d, e=0.0339; Discussion acknowledges Narayan et al. (2026) future decay and missing wind drag as limitations.
  • domain assumption Mutual Hill-radius separations (Gladman/Chambers/Obertas-type criteria) usefully organize stable vs unstable initial placements for this two-companion system.
    Appendix B and Fig. 3 blue/green dashed lines; used to interpret early ejections vs longer-lived systems.
  • ad hoc to paper A single interior planet (not multi-planet or exterior architectures) is a sufficient test of dynamical viability for the Li scenario.
    Stated architecture in Methods and revisited in Conclusions as a simplification for future work.
invented entities (1)
  • Hypothetical pre-engulfment super-Earth to Neptune-mass planet no independent evidence
    purpose: Provide the accreted mass reservoir needed to match TOI-5882’s Li excess under the Kotten et al. budget.
    Not observed; mass range inherited from prior abundance modeling. Independent evidence is only the star’s Li excess itself, which is the quantity under test—so independent_evidence is false for a dynamical confirmation.

pith-pipeline@v1.1.0-grok45 · 15182 in / 3885 out tokens · 36469 ms · 2026-07-11T05:42:07.360236+00:00 · methodology

0 comments
read the original abstract

As stars evolve off the main sequence, changes in stellar structure can alter the dynamical architecture of planetary systems and, in some cases, lead to planet engulfment events capable of producing observable chemical signatures such as lithium enhancement. TOI-5882 is a lithium-rich subgiant hosting a 22 m_Jup brown dwarf on a 7.1-day orbit, where the enrichment could plausibly result from the recent engulfment of a super-Earth to Neptune-mass planet. We assess the dynamical viability of a planet engulfment scenario in the TOI-5882 system that could explain its observed Li enrichment. We combine stellar evolution models with N-body simulations that incorporate time-dependent stellar properties as the host star leaves the main sequence, exploring a broad range of pre-engulfment planetary masses and orbital configurations. Planet engulfment is the most probable outcome under the explored configurations. However, only 5% of the simulations produce engulfment within the short detectability window of the lithium-enrichment signature. Engulfment therefore remains a viable explanation for the observed Li enhancement in TOI-5882, but only for a relatively uncommon subset of the initial conditions considered here. Under our simplified architecture, recent engulfment cannot be ruled out as the origin of the observed lithium enhancement. However, because successful cases represent only a small fraction of the initial conditions explored here, and because additional processes such as wind-induced drag forces were not included, additional constraints on the system's primordial architecture are needed to assess how likely this scenario is for TOI-5882.

Figures

Figures reproduced from arXiv: 2607.05566 by C. Aguilera-G\'omez, C. Charalambous, C. Norambuena, S. Urrutia.

Figure 2
Figure 2. Figure 2: Temporal evolution of the stellar mass (dashed line) and radius (solid line) from the end of the main sequence through the completion of the subgiant phase. The gray shaded area indicates the time interval dur￾ing which a planetary engulfment would be observationally detectable. mass and atmospheric parameters naturally account for the small offset between the best-fit track and the position of the star in… view at source ↗
Figure 1
Figure 1. Figure 1: Top: Teff-log g diagram showing the evolutionary track of a 1.3 M⊙ star with [Fe/H] = 0.33 dex, color-coded by stellar age. The position of TOI-5882 is indicated using the atmospheric parameters reported by Kotten et al. (2026). With circles we highlight the age re￾ported in previous studies (4.11 Gyr); the onset of the subgiant branch (4.23 Gyr); and the end of the evolutionary phase during which sur￾face… view at source ↗
Figure 3
Figure 3. Figure 3: Outcome of 300 simulations exploring plausible pre-engulfment orbital configurations in the period–mass plane. The blue dashed line mark the common stability threshold mutual Hill-radius separation between a fixed brown dwarf (m = 22 mJup, PBD = 7.1 d), and an inner planet with varying mass, around a M⋆ = 1.3 M⊙ star. The green dashed line represent a more conservative stability limit. Crosses mark cases i… view at source ↗
Figure 4
Figure 4. Figure 4: Planet engulfment occurring during the lithium-detectable pe￾riod (mpl = 53.95 m⊕, Ppl = 0.91 d). Evolution of the semi-major axes, pericenter, apocenter distances (top) and eccentricities (bottom) of both the planet and the BD, together with the stellar radius. Finally, although the Li detectability window ends at 4.61 Gyr, we extend the simulations until either BD or planet are en￾gulfed or escape the sy… view at source ↗

discussion (0)

Sign in with ORCID, Apple, or X to comment. Anyone can read and Pith papers without signing in.

Reference graph

Works this paper leans on

34 extracted references · 16 canonical work pages · 16 internal anchors

  1. [1]

    , keywords =

    The resonance overlap criterion and the onset of stochastic behavior in the restricted three-body problem. , keywords =. doi:10.1086/112778 , adsurl =

    doi:10.1086/112778

  2. [2]

    , keywords =

    Tidal evolution in close binary systems. , keywords =

  3. [3]

    , keywords =

    Dynamics of Systems of Two Close Planets. , keywords =. doi:10.1006/icar.1993.1169 , adsurl =

    doi:10.1006/icar.1993.1169 1993

  4. [4]

    , year = 1996, month = feb, volume =

    The Stability of Multi-Planet Systems. , year = 1996, month = feb, volume =. doi:10.1006/icar.1996.0019 , adsurl =

    doi:10.1006/icar.1996.0019 1996

  5. [5]

    , keywords =

    Are There Unstable Planetary Systems around White Dwarfs?. , keywords =. doi:10.1086/340291 , archivePrefix =. astro-ph/0202273 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/340291

  6. [6]

    , keywords =

    Can Planets Survive Stellar Evolution?. , keywords =. doi:10.1086/516746 , archivePrefix =. astro-ph/0702724 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/516746

  7. [7]

    , keywords =

    Dynamical Outcomes of Planet-Planet Scattering. , keywords =. doi:10.1086/590227 , archivePrefix =. astro-ph/0703166 , primaryClass =

    Pith/arXiv arXiv doi:10.1086/590227

  8. [8]

    , keywords =

    The Orbital Evolution of Gas Giant Planets Around Giant Stars. , keywords =. doi:10.1088/0004-637X/705/1/L81 , archivePrefix =. 0910.2396 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/705/1/l81

  9. [9]

    Planet Engulfment by ~1.5-3 Solar-Mass Red Giants

    Planet Engulfment by -0.5ex 1.5-3 M _ sun Red Giants. , keywords =. doi:10.1088/0004-637X/737/2/66 , archivePrefix =. 1106.2251 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/737/2/66

  10. [10]

    , keywords =

    Modules for Experiments in Stellar Astrophysics (MESA). , keywords =. doi:10.1088/0067-0049/192/1/3 , archivePrefix =. 1009.1622 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0067-0049/192/1/3

  11. [11]

    , keywords =

    Foretellings of Ragnar \"o k: World-engulfing Asymptotic Giants and the Inheritance of White Dwarfs. , keywords =. doi:10.1088/0004-637X/761/2/121 , archivePrefix =. 1210.0328 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/761/2/121

  12. [12]

    , keywords =

    REBOUND: an open-source multi-purpose N-body code for collisional dynamics. , keywords =. doi:10.1051/0004-6361/201118085 , archivePrefix =. 1110.4876 , primaryClass =

    Pith/arXiv arXiv doi:10.1051/0004-6361/201118085

  13. [13]

    Dynamical Measurements of the Interior Structure of Exoplanets

    Dynamical Measurements of the Interior Structure of Exoplanets. , keywords =. doi:10.1088/0004-637X/778/2/100 , archivePrefix =. 1309.5363 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/778/2/100

  14. [14]

    First order resonance overlap and the stability of close two planet systems

    First-order Resonance Overlap and the Stability of Close Two-planet Systems. , keywords =. doi:10.1088/0004-637X/774/2/129 , archivePrefix =. 1307.8119 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/774/2/129

  15. [15]

    The Resonance Overlap and Hill Stability Criteria Revisited

    The resonance overlap and Hill stability criteria revisited. Celestial Mechanics and Dynamical Astronomy , keywords =. doi:10.1007/s10569-015-9646-z , archivePrefix =. 1509.03607 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1007/s10569-015-9646-z

  16. [16]

    , keywords =

    IAS15: a fast, adaptive, high-order integrator for gravitational dynamics, accurate to machine precision over a billion orbits. , keywords =. doi:10.1093/mnras/stu2164 , archivePrefix =. 1409.4779 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stu2164

  17. [17]

    , keywords =

    WHFAST: a fast and unbiased implementation of a symplectic Wisdom-Holman integrator for long-term gravitational simulations. , keywords =. doi:10.1093/mnras/stv1257 , archivePrefix =. 1506.01084 , primaryClass =

    Pith/arXiv arXiv doi:10.1093/mnras/stv1257

  18. [18]

    Post-main-sequence planetary system evolution

    Post-main-sequence planetary system evolution. Royal Society Open Science , keywords =. doi:10.1098/rsos.150571 , archivePrefix =. 1601.05419 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1098/rsos.150571

  19. [19]

    On Lithium-6 as diagnostic of the lithium-enrichment mechanism in red giants

    On Lithium-6 as a Diagnostic of the Lithium-enrichment Mechanism in Red Giants. , keywords =. doi:10.3847/2041-8213/ab9d26 , archivePrefix =. 2005.14209 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/ab9d26 2041

  20. [20]

    How Jupiters save or destroy inner Neptunes around evolved stars

    How Jupiters Save or Destroy Inner Neptunes around Evolved Stars. , keywords =. doi:10.3847/2041-8213/aba35f , archivePrefix =. 2007.04337 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/2041-8213/aba35f 2041

  21. [21]

    , keywords =

    The GALAH survey: Data release 4. , keywords =. doi:10.1017/pasa.2025.26 , archivePrefix =. 2409.19858 , primaryClass =

    Pith/arXiv arXiv doi:10.1017/pasa.2025.26 2025

  22. [22]

    , keywords =

    Eleven New Transiting Brown Dwarfs and Very-low-mass Stars from TESS. , keywords =. doi:10.3847/1538-3881/addd17 , archivePrefix =. 2501.09795 , primaryClass =

    Pith/arXiv arXiv doi:10.3847/1538-3881/addd17

  23. [23]

    Observable Signatures of Planet Accretion in Red Giant Stars. I. Rapid Rotation and Light Element Replenishment. , keywords =. doi:10.1088/0004-637X/757/2/109 , archivePrefix =. 1208.1775 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1088/0004-637x/757/2/109

  24. [24]

    , keywords =

    Hot Jupiters and Cool Stars. , keywords =. doi:10.1088/0004-637X/794/1/3 , archivePrefix =. 1407.7879 , primaryClass =

    Pith/arXiv arXiv doi:10.1088/0004-637x/794/1/3

  25. [25]

    Star-planet interactions. II. Is planet engulfment the origin of fast rotating red giants?. , keywords =. doi:10.1051/0004-6361/201628758 , archivePrefix =. 1606.08027 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1051/0004-6361/201628758

  26. [26]

    On Lithium-rich Red Giants. I. Engulfment of Substellar Companions. , keywords =. doi:10.3847/0004-637X/829/2/127 , archivePrefix =. 1605.05332 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/0004-637x/829/2/127

  27. [27]

    , keywords =

    The stability of tightly-packed, evenly-spaced systems of Earth-mass planets orbiting a Sun-like star. , keywords =. doi:10.1016/j.icarus.2017.04.010 , archivePrefix =. 1703.08426 , primaryClass =

    Pith/arXiv arXiv doi:10.1016/j.icarus.2017.04.010 2017

  28. [28]

    REBOUNDx: A Library for Adding Conservative and Dissipative Forces to Otherwise Symplectic N-body Integrations

    REBOUNDx: a library for adding conservative and dissipative forces to otherwise symplectic N-body integrations. , keywords =. doi:10.1093/mnras/stz2870 , archivePrefix =. 1908.05634 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stz2870 1908

  29. [29]

    Lithium Enrichment Signatures of Planetary Engulfment Events in Evolved Stars

    Lithium Enrichment Signatures of Planetary Engulfment Events in Evolved Stars. , keywords =. doi:10.3847/1538-3881/ac273c , archivePrefix =. 2002.05275 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.3847/1538-3881/ac273c 2002

  30. [30]

    Stellar Evolution and Tidal Dissipation in REBOUNDx

    Stellar evolution and tidal dissipation in REBOUNDx. , keywords =. doi:10.1093/mnras/stac043 , archivePrefix =. 2101.12277 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac043

  31. [31]

    Planet Engulfment Detections are Rare According to Observations and Stellar Modeling

    Planet engulfment detections are rare according to observations and stellar modelling. , keywords =. doi:10.1093/mnras/stad745 , archivePrefix =. 2210.12121 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stad745

  32. [32]

    Planet Engulfment Signatures in Twin Stars

    Planet engulfment signatures in twin stars. , keywords =. doi:10.1093/mnras/stac3435 , archivePrefix =. 2210.11679 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.1093/mnras/stac3435

  33. [33]

    arXiv e-prints , keywords =

    Lithium Enrichment in a Subgiant Star with a Brown Dwarf Companion: A Planetary Engulfment Candidate. arXiv e-prints , keywords =

  34. [34]

    The Tale of a Hungry Subgiant and Its Brown Dwarf: Interior Radiative Damping Dominates the Tidal Evolution of TOI-5882

    The Tale of a Hungry Subgiant and Its Brown Dwarf: Interior Radiative Damping Dominates the Tidal Evolution of TOI-5882. arXiv e-prints , keywords =. doi:10.48550/arXiv.2605.04141 , archivePrefix =. 2605.04141 , primaryClass =

    work page internal anchor Pith review Pith/arXiv arXiv doi:10.48550/arxiv.2605.04141