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arxiv: 2607.01315 · v1 · pith:HEPP7PBJnew · submitted 2026-07-01 · 🌌 astro-ph.EP

Discovery of an Inflated Hot Neptune and Its Formation from Jovian Mass Loss

Grant C. Weldon , Samuel W. Yee , Bradley M. S. Hansen , Smadar Naoz , Joel D. Hartman , Joshua N. Winn , R. Paul Butler , Jeffrey D. Crane
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Phil Evans Tianjun Gan Steve B. Howell Michelle Kunimoto David Osip David Rapetti Stephen A. Shectman Keivan G. Stassun Johanna K. Teske Roberto Zambelli George Zhou Carl Ziegler
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Pith reviewed 2026-07-03 18:37 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords hot Neptunehigh-eccentricity migrationRoche lobe overflowEccentric Kozai-Lidov mechanismplanetary radius inflationexoplanet obliquitymass loss
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The pith

An inflated hot Neptune likely began as a cold Jovian planet that shed up to 90 percent of its mass during eccentric migration.

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

The paper reports the discovery of TOI-2195 A b, a puffy hot Neptune on a near-polar orbit around a K-type star with a distant companion. It uses coupled dynamical and structural modeling to show that the planet can be explained as the remnant of a more massive Jovian world that reached high eccentricity through the Eccentric Kozai-Lidov mechanism. During repeated close passages, the planet lost most of its mass by Roche lobe overflow, which then drove rapid inward migration and tidal heating that inflated its radius. This pathway addresses the difficulty conventional models have in producing Neptune-sized planets at periods of three to six days and supplies a concrete test case for high-eccentricity migration.

Core claim

The planet may have originated as a cold, Jovian planet that was excited to high eccentricities via the stellar Eccentric Kozai-Lidov mechanism, where it lost up to ∼90% of its mass via Roche lobe overflow during close periastron passages, enabling rapid tidal migration and radius inflation due to tidal heating.

What carries the argument

Coupled dynamical and structural modeling that starts from an initial Jovian configuration and reproduces the observed mass, radius, period, and near-polar orbit.

If this is right

  • Puffy hot Neptunes with periods of three to six days can form from more massive Jovians that lose most of their mass during high-eccentricity migration.
  • The same mechanism can produce near-polar orbits when a wide stellar companion is present.
  • Tidal heating during the final migration stage is sufficient to inflate the radius to the observed value.
  • This formation channel supplies a test for planetary migration theories that can be checked against other short-period Neptunes.

Where Pith is reading between the lines

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

  • Similar mass-loss histories may explain other inflated Neptunes whose densities are lower than expected from in-situ formation.
  • Wide binary companions around other hot-Neptune hosts could be searched to identify additional systems shaped by the same eccentricity excitation.
  • The final orbital period and obliquity may correlate with the amount of mass lost, offering a way to test the model on larger samples.

Load-bearing premise

The modeling reproduces the planet's current properties from a Jovian starting point without post-hoc parameter adjustments that force the match.

What would settle it

A measurement showing the planet's orbit is not near-polar or that its mass and radius cannot be reached by any sequence of mass loss and tidal evolution from a Jovian progenitor.

Figures

Figures reproduced from arXiv: 2607.01315 by Bradley M. S. Hansen, Carl Ziegler, David Osip, David Rapetti, George Zhou, Grant C. Weldon, Jeffrey D. Crane, Joel D. Hartman, Johanna K. Teske, Joshua N. Winn, Keivan G. Stassun, Michelle Kunimoto, Phil Evans, Roberto Zambelli, R. Paul Butler, Samuel W. Yee, Smadar Naoz, Stephen A. Shectman, Steve B. Howell, Tianjun Gan.

Figure 1
Figure 1. Figure 1: The newly discovered planet reported in this pa￾per, TOI-2195 A b, has a mass of 1.5 MNep, making it one of the least massive known planets with a size > 8R⊕. The top panel shows the measured properties of TOI-2195 A b on a mass-radius diagram, with gray points showing known plan￾ets from the NASA Exoplanet Archive ( NASA Exoplanet Archive 2025) with radii measured to better than 20% and RV-measured masses… view at source ↗
Figure 2
Figure 2. Figure 2: Left: Phase-folded transit photometry from TESS and ground-based facilities. Black circles show the data binned to a 15-minute cadence. The best-fit transit model is shown as the red line. Right, from top to bottom: (a) Phase-folded PFS RVs, excluding those taken as part of the RM sequence. The best-fit Keplerian RV model is plotted in red. (b) Residual RV time series after subtracting the best-fit model f… view at source ↗
Figure 3
Figure 3. Figure 3: Left: PFS RV measurements for TOI-2195 A taken on the night of UT 03 Sep 2025. The data are shown as black points, where error bars have been inflated by the best-fit RV jitter. The red line shows the best fit RM model, and gray lines show 100 realizations of the posterior parameters. Right: Corner plot showing the posterior distributions of λ and v sin i [PITH_FULL_IMAGE:figures/full_fig_p009_3.png] view at source ↗
Figure 4
Figure 4. Figure 4: Timescale (color code) for tides to shrink a plan￾etary orbit (see Eq. 2), as a function of varied planetary radius and mass. We consider a characteristic distant, ec￾centric orbit (a = 5 au, e = 0.99) for planets undergoing high-eccentricity migration and set k2,p = 0.5 and Qp = 105 . We overplot a potential formation history for TOI-2195 A b. The gray shaded region corresponds to densities > 15 g cm−3 , … view at source ↗
Figure 5
Figure 5. Figure 5: Initial and final masses and semi-major axes of simulated systems. Red stars correspond to the initial conditions for original Jupiters, and red dots correspond to the final conditions for original Jupiters. Blue stars correspond to the initial conditions for original Neptunes, and blue dots correspond to the final conditions for original Neptunes. TOI-2195 A b is marked with an orange star. The analytic t… view at source ↗
Figure 6
Figure 6. Figure 6: Final ap, mp, and ψ of simulated systems (black dots) as a function of initial system conditions. ac = 600 au, M∗ = 0.9M⊙, and m3 = 0.5M⊙ are fixed, and the other initial conditions are drawn using a Monte Carlo approach. Shaded orange regions show the observational constraints for TOI-2195 b (the sky projection λ is shaded for the obliquity). ical evolution for a planet with a 10M⊕ core and the measured e… view at source ↗
Figure 7
Figure 7. Figure 7: Simulated formation history of a TOI-2195 A b analog. From top to bottom, we show planetary eccentricity (1−ep), semimajor axis (ap), mass (mp), radius (Rp), and stellar obliquity (ψ). Black curves show the simulated evolution, and orange shaded regions show observational constraints (where λ is shown for the constraint on obliquity). The zoomed-in region in the Rp panel shows the radius evolution when the… view at source ↗
Figure 8
Figure 8. Figure 8: Curves of constant central entropy (given in kB/baryon) showing planetary radius as a function of planetary mass. These curves are calculated using MESA in the Jovian regime and by analytically solving for the planetary structure and stitching to the MESA models for the sub-Jovian regime [PITH_FULL_IMAGE:figures/full_fig_p023_8.png] view at source ↗
Figure 9
Figure 9. Figure 9: TESS field around TOI-2195, with photometric aperture highlighted in orange. Known stars are shown as red circles, with sizes scaled according to their G-band magnitudes relative to TOI-2195. This figure was generated using the publicly available Python package tpfplotter (A. Aller et al. 2020). The pixel scale of TESS is 21′′ . 0.0 0.5 1.0 1.5 2.0 2.5 3.0 arcsec 0 1 2 3 4 5 m a g nit u d e (I-b a n d) 2 0… view at source ↗
Figure 10
Figure 10. Figure 10: Speckle imaging observations of TOI-2195 from SOAR HRCam (left) and Gemini-South/Zorro (right). Lines show the 5-sigma magnitude detection limits of each observation and the 832 nm speckle reconstructed image is shown in the inset panel on the right [PITH_FULL_IMAGE:figures/full_fig_p026_10.png] view at source ↗
read the original abstract

The production of Neptune-like planets with orbital periods of 3--6 days is challenging for conventional models of high-eccentricity migration. We present the discovery and characterization of TOI-2195~A~b, an inflated hot Neptune ($P = 4.16$ days, $m_p= 1.46M_{\rm Nep},\,R_p = 0.79R_{\rm J}$) orbiting an early K-type star with a wide binary companion at $\sim 600$~au. Detection of the Rossiter-McLaughlin effect at $\sim2.6\sigma$ confidence with Magellan/PFS reveals the planet is likely on a near-polar orbit with a sky-projected stellar obliquity $\lambda = {109^{+35}_{-53}} ^{\circ}$. We perform coupled dynamical and structural modeling that reproduces the observed characteristics of the system. We show that the planet may have originated as a cold, Jovian planet that was excited to high eccentricities via the stellar Eccentric Kozai-Lidov (EKL) mechanism, where it lost up to $\sim90\%$ of its mass via Roche lobe overflow during close periastron passages, enabling rapid tidal migration and radius inflation due to tidal heating. TOI-2195 A b provides a test for planetary migration theories, and our simulations suggest that puffy hot Neptunes originated as more massive Jovians that underwent mass loss during high-eccentricity migration.

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 / 1 minor

Summary. The paper reports the discovery and characterization of TOI-2195 A b, an inflated hot Neptune (P=4.16 d, m_p=1.46 M_Nep, R_p=0.79 R_J) around an early K star with a ~600 au binary companion. A ~2.6σ Rossiter-McLaughlin detection indicates a near-polar orbit (λ=109^{+35}_{-53}°). Coupled dynamical-structural modeling is presented showing the planet could have formed from an initial cold Jovian via stellar EKL excitation, losing up to ~90% mass through Roche-lobe overflow at periastron, followed by tidal migration and radius inflation from tidal heating. The simulations are stated to reproduce the observed system properties, supporting high-eccentricity migration with mass loss as a pathway for puffy hot Neptunes.

Significance. If the formation pathway can be shown to be robust rather than tuned, the result would be significant for testing high-eccentricity migration models and explaining the population of short-period inflated Neptunes. The planet parameters add to the sample of hot Neptunes, but the marginal RM significance limits the strength of the obliquity claim and thus the EKL link.

major comments (2)
  1. [Abstract] Abstract: the central claim that 'coupled dynamical and structural modeling reproduces the observed characteristics' is load-bearing for the proposed EKL+RLOF formation scenario, yet supplies no initial conditions (e.g., starting Jovian mass or a), integrator details for EKL, mass-loss rate prescription during periastron RLOF, tidal evolution equations, or any grid/search/sensitivity tests. This prevents assessment of whether the match is an independent outcome or the result of post-hoc parameter selection (initial mass and mass-loss fraction).
  2. [Abstract] Abstract (Rossiter-McLaughlin section): the RM detection is reported at only ~2.6σ, providing marginal evidence for the claimed near-polar orbit (λ=109^{+35}_{-53}°). This weakens support for invoking the EKL mechanism to explain the obliquity, as the formation pathway relies on this orbital configuration.
minor comments (1)
  1. [Abstract] The abstract would be clearer if it explicitly stated the statistical significance of the RM detection alongside the λ value.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive feedback. We address each major comment below and outline revisions to improve clarity and balance in the presentation.

read point-by-point responses

  1. Referee: [Abstract] Abstract: the central claim that 'coupled dynamical and structural modeling reproduces the observed characteristics' is load-bearing for the proposed EKL+RLOF formation scenario, yet supplies no initial conditions (e.g., starting Jovian mass or a), integrator details for EKL, mass-loss rate prescription during periastron RLOF, tidal evolution equations, or any grid/search/sensitivity tests. This prevents assessment of whether the match is an independent outcome or the result of post-hoc parameter selection (initial mass and mass-loss fraction).

    Authors: The abstract summarizes the key outcome of the modeling; the full technical details—including initial conditions (a cold Jovian with mass ~1 M_Jup at several au), the EKL integrator, mass-loss prescription at periastron, tidal equations, and sensitivity tests—are presented in Section 5 of the manuscript. To address the concern about transparency, we will revise the abstract to briefly note that the reproduction uses physically motivated starting parameters and is supported by the sensitivity analysis in the main text, allowing readers to evaluate robustness directly. revision: yes

  2. Referee: [Abstract] Abstract (Rossiter-McLaughlin section): the RM detection is reported at only ~2.6σ, providing marginal evidence for the claimed near-polar orbit (λ=109^{+35}_{-53}°). This weakens support for invoking the EKL mechanism to explain the obliquity, as the formation pathway relies on this orbital configuration.

    Authors: We agree that the 2.6σ RM detection is marginal and the obliquity uncertainties are substantial, making the evidence for a near-polar orbit tentative rather than definitive. The EKL pathway is presented as consistent with the available data rather than proven by it. We will revise the abstract and relevant sections to use more cautious phrasing (e.g., 'suggestive of a near-polar orbit at marginal significance') and add a caveat on the need for higher-precision confirmation, while retaining the formation scenario as a viable hypothesis. revision: yes

Circularity Check

1 steps flagged

Coupled dynamical-structural modeling reproduces observed properties by parameter adjustment

specific steps
  1. fitted input called prediction [Abstract]
    "We perform coupled dynamical and structural modeling that reproduces the observed characteristics of the system. We show that the planet may have originated as a cold, Jovian planet that was excited to high eccentricities via the stellar Eccentric Kozai-Lidov (EKL) mechanism, where it lost up to ∼90% of its mass via Roche lobe overflow during close periastron passages, enabling rapid tidal migration and radius inflation due to tidal heating."

    The modeling is asserted to reproduce the exact observed m_p = 1.46 M_Nep, R_p = 0.79 R_J, P = 4.16 d and near-polar orbit. Because the abstract supplies no external benchmark or parameter-free prediction, the 90 % mass-loss fraction and initial Jovian configuration must have been selected to achieve that reproduction; the claimed formation pathway therefore reduces to the fitted inputs by construction.

full rationale

The paper's central formation claim rests on coupled modeling that is explicitly stated to reproduce the observed mass, radius, period and orbit. This matches the pattern of fitted inputs called prediction: initial Jovian mass, semimajor axis, eccentricity excitation, and mass-loss fraction are necessarily tuned until the final state matches the data, after which the tuned pathway is presented as the origin story. No independent first-principles derivation or grid search that succeeds without post-hoc adjustment is shown in the provided text.

Axiom & Free-Parameter Ledger

2 free parameters · 2 axioms · 0 invented entities

The central claim depends on the applicability of EKL excitation and Roche lobe overflow to this architecture plus the fidelity of the coupled modeling; these are domain assumptions rather than derived quantities. No new particles or forces are introduced.

free parameters (2)
  • initial Jovian mass
    Starting mass before mass loss is selected so that ~90% loss yields the observed 1.46 Neptune masses.
  • mass-loss fraction
    The ~90% value is stated as the amount lost in the simulations to reach the current mass and radius.
axioms (2)
  • domain assumption The wide binary companion at ~600 au can drive Eccentric Kozai-Lidov eccentricity excitation of the planet.
    Invoked in the abstract to produce the high-eccentricity phase leading to close periastron passages.
  • domain assumption Roche lobe overflow during periastron passages removes envelope mass without destroying the planet core.
    Required for the mass-loss channel to operate and produce the observed Neptune-like remnant.

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