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arxiv: 2605.14433 · v1 · submitted 2026-05-14 · 🌌 astro-ph.EP

Recognition: 2 theorem links

· Lean Theorem

Where Do Hot Jupiters Come From? Revisiting Tidal Disruption and Ejection in High-Eccentricity Migration

Qianli Fan , Shang-Fei Liu
Authors on Pith no claims yet

Pith reviewed 2026-05-15 02:05 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords hot jupitershigh-eccentricity migrationtidal encountershydrodynamic simulationsplanetary coresenvelope strippingexoplanet migrationtidal ejection
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The pith

Planets with dense cores avoid total tidal disruption in close encounters, allowing more to survive as hot Jupiters or stripped remnants.

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

The paper tests whether giant planets with realistic 10-20 Earth-mass cores can survive the close tidal encounters expected during high-eccentricity migration to form hot Jupiters. Traditional coreless models predicted complete disruption or ejection inside roughly 2.7 tidal radii, but the simulations show no total disruptions occur in that zone. Instead, deep encounters strip most of the envelope, leaving dense remnants or ejecting the planet after repeated passes, while wider encounters permit gradual circularization with little mass loss. The orbital energy change depends mainly on periastron distance for highly eccentric orbits, which lets the results be extrapolated across a wide range of initial conditions.

Core claim

Three-dimensional hydrodynamic simulations of giant planets with dense cores demonstrate that no total disruptions occur within 2.7 tidal radii. Deep encounters below 1.7 tidal radii cause severe envelope stripping, producing either progressively smaller dense remnants or ejection after a few passages. Intermediate encounters between 1.7 and 2.0 tidal radii lead to significant partial mass loss over multiple encounters, while wider encounters above 2.0 tidal radii result in minimal mass loss that allows the planets to circularize into hot Jupiters. For eccentricities above 0.9 the change in specific orbital energy depends primarily on periastron distance rather than semi-major axis, enabling

What carries the argument

Three-dimensional hydrodynamic simulations tracking envelope stripping and orbital energy change for giant planets with 10-20 Earth-mass cores during repeated tidal encounters at varying periastron distances.

If this is right

  • Hot Jupiters can form from planets that undergo repeated partial mass loss in the 1.7-2.0 tidal-radius range without being destroyed.
  • Ejected stripped remnants may contribute to the free-floating planet population.
  • The effective tidal exclusion zone shrinks or disappears once cores are included, widening the survival window for high-eccentricity migration.
  • Results for highly eccentric orbits can be extrapolated using periastron distance alone across broad ranges of semi-major axis.

Where Pith is reading between the lines

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

  • Some observed dense sub-Neptunes or super-Earths could be the stripped cores of former hot Jupiters.
  • Migration models that ignore internal structure will overpredict disruption rates and underpredict the number of surviving hot Jupiters.
  • Targeted searches for free-floating planets with remnant atmospheres might reveal signatures of prior envelope stripping.

Load-bearing premise

The simulations with 10-20 Earth-mass cores correctly capture envelope stripping and orbital energy changes without major unmodeled effects from magnetic fields or equation-of-state variations.

What would settle it

An observation or simulation showing complete disruption of a core-bearing giant planet at a periastron of 2.5 tidal radii without prior envelope stripping would falsify the no-total-disruption claim.

Figures

Figures reproduced from arXiv: 2605.14433 by Qianli Fan, Shang-Fei Liu.

Figure 1
Figure 1. Figure 1: Bound mass versus initial rp/rt for planets with 10 M⊕ (blue) and 20 M⊕ (orange) cores. Progressively darker shades within each color group represent the initial state and the remnant mass after the first, second, and third encounters, respectively. All masses are in Earth masses. 3.2. Orbital Evolution During Repeated Encounters The change in specific orbital energy, ∆Eorb, occurs predominantly during the… view at source ↗
Figure 2
Figure 2. Figure 2: Structural evolution during the most extreme mass-loss case in our simulations (rp/rt = 1.2, Mcore = 10 M⊕). Upper panel: Density slices showing the planet before and after tidal encounters. The post-encounter remnant is visibly distorted and spinning, with a significant portion of the envelope stripped. Lower left: Quantitative comparison of the spherically averaged density profiles before (solid line) an… view at source ↗
Figure 3
Figure 3. Figure 3: Specific orbital energy change ∆Eorb as a function of normalized pericenter distance rp/rt for planets with 10 M⊕ (left) and 20 M⊕ (right) cores (a = 1 AU). Colored symbols show the energy change after the first (red circles), second (blue squares), and third (green triangles) encounters. The discrete data points are connected by cubic spline interpolations to illustrate the trend. The horizontal dashed li… view at source ↗
Figure 4
Figure 4. Figure 4: Predicted Orbital Energy Change in the a − e Parameter Space, rp increases from the top-left to the bottom-right corner. The panels map the cumulative specific orbital energy change, Σ∆Eorb, after three tidal encounters as a function of the initial orbital semi-major axis a and eccentricity e, for planetary models with a 10 M⊕ (upper panel) and a 20 M⊕ (lower panel) core. The color indicates the net energy… view at source ↗
Figure 5
Figure 5. Figure 5: Semi-major axis versus eccentricity diagram for high-eccentricity exoplanets, based on our simulation results for planets with a 10 M⊕ core. Overlaid are contours of constant tidal circularization time for 1 Gyr and 5 Gyr, computed for a Jupiter-mass planet with Jupiter’s radius, for two representative values of the tidal dissipation parameter: Q ′ p = 104 (blue dotted line) and Q ′ p = 106 (black dash-dot… view at source ↗
Figure 6
Figure 6. Figure 6: Density (left) and cumulative mass (right) profiles for planetary models with a 20M⊕ core, under different mass-loss scenarios: no mass loss, 50% mass loss, and 80% mass loss. The blue solid, orange dashed, and green dotted lines correspond to total masses of 1.0MJ, 0.5MJ, and 0.2MJ, respectively [PITH_FULL_IMAGE:figures/full_fig_p015_6.png] view at source ↗
read the original abstract

The origin of hot Jupiters remains a key open question. In the high-eccentricity migration scenario, traditional coreless models predict a strict tidal exclusion zone within $\sim 2.7$ tidal radii $r_\textrm{t}$, in which giant planets are either fully disrupted or ejected. We revisit this limit using three-dimensional hydrodynamic simulations of giant planets with realistic dense cores (10 - 20 $M_\oplus$). We find that even a few-percent-mass core fundamentally changes the outcome: \textbf{no total disruptions} occur within the previously suggested destruction zone ($\lesssim 2.7 \, r_\textrm{t}$). For deep encounters ($\lesssim 1.7 \, r_\textrm{t}$) planets suffer severe envelope stripping and are either progressively downsized to dense remnants or ejected after a few close encounters, possibly contributing to the free-floating planet population. In the intermediate regime ($ \sim 1.7 $--$2.0, r_\mathrm{t}$), planets experience significant partial mass loss over repeated encounters. For wider encounters ($ \gtrsim 2.0\, r_\mathrm{t} $), mass loss is minimal, allowing the planets gradually circularize into hot Jupiters. Furthermore, we show that for highly eccentric orbits ($e\gtrsim 0.9$), the change in specific orbital energy $ \Delta E_{\mathrm{orb}} $ depends primarily on periastron distance $ r_\mathrm{p} $ rather than semi-major axis $ a $. This enables us to extrapolate our fixed-$ a $ results across a broad ($a$, $e$) parameter space and identify a well-defined tidal ejection zone whose sharp boundaries converge asymptotically. Our results highlight the crucial role of planetary internal structure in high-eccentricity migration and suggest that the survival and transformation of core-bearing giant planets are far more common than previously thought.

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 uses three-dimensional hydrodynamic simulations of giant planets with dense cores (10-20 M⊕) to revisit tidal disruption in high-eccentricity migration. It claims that no total disruptions occur for periastron distances ≲ 2.7 tidal radii, unlike coreless models; deep encounters (≲ 1.7 rt) cause severe envelope stripping leading to downsized remnants or ejection, intermediate encounters produce partial mass loss, and wider encounters allow minimal loss and circularization into hot Jupiters. The change in orbital energy ΔE_orb is found to depend primarily on rp rather than a for e ≳ 0.9, enabling extrapolation to map a tidal ejection zone.

Significance. If robust, the results substantially revise the high-eccentricity migration pathway by showing that core-bearing planets survive close encounters far more often than previously thought, potentially explaining the observed hot Jupiter population and contributing to free-floating planets via ejection of stripped remnants. The rp-dependent ΔE_orb relation is a strength, as it is an output of the simulations rather than an input assumption and permits broad parameter-space application without additional free parameters.

major comments (3)
  1. [Methods] Methods section on simulation setup: The treatment of the planetary core (finite size, equation of state, and whether it remains intact under extreme stripping) is central to the no-total-disruption claim, yet the manuscript provides insufficient detail on core modeling and any tests against analytic Roche-limit expectations for the coreless limit; this directly affects whether the reported outcomes for rp ≲ 1.7 rt are physically complete.
  2. [Results] Results on deep encounters (rp ≲ 1.7 rt): The progressive downsizing to dense remnants and subsequent ejection is load-bearing for the revised ejection zone, but the manuscript does not report quantitative remnant masses, densities, or post-stripping Roche-limit checks to confirm the remnants do not disrupt in later encounters.
  3. [Discussion] Section on orbital energy extrapolation: The assertion that ΔE_orb depends primarily on rp (rather than a) for e ≳ 0.9 is used to map the ejection zone across broad (a, e) space, but the manuscript lacks explicit validation runs at varied semi-major axes to quantify the residual a-dependence and uncertainty in the zone boundaries.
minor comments (2)
  1. [Abstract] Abstract: The phrase 'a few-percent-mass core' should be replaced with the actual simulated core masses (10-20 M⊕) for precision.
  2. [Figures] Figure captions: All panels showing encounter outcomes should explicitly label the rp/rt regimes (deep, intermediate, wide) to improve readability.

Simulated Author's Rebuttal

3 responses · 0 unresolved

We thank the referee for their thoughtful and constructive comments, which have helped clarify several aspects of our work. We address each of the major comments point by point below.

read point-by-point responses

  1. Referee: [Methods] Methods section on simulation setup: The treatment of the planetary core (finite size, equation of state, and whether it remains intact under extreme stripping) is central to the no-total-disruption claim, yet the manuscript provides insufficient detail on core modeling and any tests against analytic Roche-limit expectations for the coreless limit; this directly affects whether the reported outcomes for rp ≲ 1.7 rt are physically complete.

    Authors: We agree that the Methods section would benefit from expanded details on the core treatment. In the revised manuscript, we will provide additional information on the finite size of the core, the specific equation of state used for the core and envelope, and include validation tests showing that our hydrodynamic code reproduces the analytic Roche-limit expectations in the coreless limit. These additions will strengthen the physical basis for our no-total-disruption results. revision: yes

  2. Referee: [Results] Results on deep encounters (rp ≲ 1.7 rt): The progressive downsizing to dense remnants and subsequent ejection is load-bearing for the revised ejection zone, but the manuscript does not report quantitative remnant masses, densities, or post-stripping Roche-limit checks to confirm the remnants do not disrupt in later encounters.

    Authors: We will revise the Results section to include quantitative values for the remnant masses and densities after severe stripping in deep encounters. We will also add post-stripping Roche-limit calculations to demonstrate that the dense remnants remain intact in subsequent passages, supporting the ejection scenario. revision: yes

  3. Referee: [Discussion] Section on orbital energy extrapolation: The assertion that ΔE_orb depends primarily on rp (rather than a) for e ≳ 0.9 is used to map the ejection zone across broad (a, e) space, but the manuscript lacks explicit validation runs at varied semi-major axes to quantify the residual a-dependence and uncertainty in the zone boundaries.

    Authors: Our simulations at fixed semi-major axis demonstrate that ΔE_orb is primarily a function of rp for e ≳ 0.9, consistent with the close-encounter physics. To address the referee's concern, we will add an explicit discussion in the revised manuscript quantifying the residual a-dependence using the existing simulation data and analytic estimates, along with an assessment of the resulting uncertainty in the tidal ejection zone boundaries. This will be done without requiring new simulations. revision: partial

Circularity Check

0 steps flagged

No significant circularity; central claims are direct outputs of independent hydrodynamic simulations

full rationale

The paper derives its key results—no total disruptions for rp ≲ 2.7 rt, envelope stripping outcomes, and the rp-dependence of ΔE_orb—from three-dimensional hydrodynamic simulations with 10-20 M⊕ cores. These are not reductions of fitted parameters renamed as predictions, nor self-definitional, nor reliant on load-bearing self-citations. The extrapolation across (a,e) space follows from the reported simulation outputs rather than being imposed by construction. No steps match the enumerated circularity patterns; the derivation chain remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

1 free parameters · 2 axioms · 0 invented entities

Central claim rests on standard hydrodynamic modeling of fluid interactions plus the specific choice of core masses as representative of real giant planets; no new entities are postulated.

free parameters (1)
  • core mass fraction = 10-20 M_earth
    Set to 10-20 Earth masses as realistic values for giant planet interiors; affects stripping thresholds.
axioms (2)
  • standard math Three-dimensional hydrodynamic equations accurately describe the planet's response to tidal forces during periastron passages.
    Invoked throughout the simulation description as the basis for tracking envelope stripping.
  • domain assumption Initial planetary structure with dense core remains stable prior to encounters.
    Assumed in setup of the 3D models.

pith-pipeline@v0.9.0 · 5655 in / 1412 out tokens · 40604 ms · 2026-05-15T02:05:47.922444+00:00 · methodology

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