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arxiv: 2606.18355 · v1 · pith:AXSMPMWGnew · submitted 2026-06-16 · 🌌 astro-ph.EP

Revisiting the Exo-Mercury Candidate GJ 367 b with ESPRESSO and a Self-Consistent Tidal Distortion Model

Rena A. Lee , Fei Dai , Ellen M. Price , Te Han , Davide Gandolfi , Mathias Zechmeister , Gu{\dh}mundur Stef\'ansson , Jiayin Dong
show 13 more authors
Simon H. Albrecht Kristine W.F. Lam Federica Chiti Jennifer L. van Saders Daniel Huber Heather A. Knutson Karen A. Collins Michael Zhang Leslie A. Rogers Eleonora Armano Casey L. Brinkman Nicholas Saunders Daniel Hey
This is my paper

Pith reviewed 2026-06-26 22:21 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords exoplanetsultra-short-period planetsGJ 367 biron fractiontidal distortionradial velocityTESS photometryinterior composition
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The pith

Revised mass and radius measurements show GJ 367 b has a 50-70 percent iron fraction, matching Mercury rather than nearly pure iron.

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

The paper remeasures the mass and radius of the ultra-short-period planet GJ 367 b using new TESS short-cadence photometry and a full-orbit ESPRESSO radial velocity dataset. It introduces a tidal distortion and interior composition model that accounts for the planet's shape under different assumptions about composition and radial aspect ratios. This yields a bulk density of about 6.9 g cm^{-3} and an iron mass fraction of 50-70 percent. The result aligns the planet with Mercury's composition and removes the previous tension with standard planet formation scenarios. A sympathetic reader would care because it shows how observational and modeling refinements can revise extreme density claims for close-in planets.

Core claim

We report a radius of 0.736 +/- 0.035 Earth radii from TESS photometry and a mass of 0.503 +/- 0.078 Earth masses from ESPRESSO radial velocities, giving a density of 6.9 +1.6/-1.4 g cm^{-3}. Using a new self-consistent tidal distortion and interior composition framework, and considering multiple interior assumptions and radial aspect ratios, the iron fraction is found to be approximately 50-70 percent, broadly consistent with Mercury and lower than prior estimates that approached solid iron.

What carries the argument

A self-consistent tidal distortion and interior composition modeling framework that evaluates iron mass fraction from assumed compositions and radial aspect ratios while incorporating the planet's distorted shape.

If this is right

  • GJ 367 b's bulk density is lower than earlier reports that placed it near solid iron.
  • Standard planet formation scenarios face reduced tension from this object's composition.
  • The iron fraction of 50-70 percent matches Mercury across varied interior assumptions.
  • Accounting for tidal distortion is necessary to avoid overestimating iron content in ultra-short-period planets.

Where Pith is reading between the lines

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

  • Similar tidal modeling could revise density estimates for other ultra-short-period planets around M dwarfs.
  • If the framework holds, Mercury-like iron fractions may be common rather than exceptional among the closest-in planets.
  • Future multi-planet system studies could test whether this composition pattern correlates with orbital architecture.

Load-bearing premise

The tidal distortion and interior composition model accurately determines the planet's shape and density without leftover effects from photometric dilution, stellar activity, or unmodeled radial velocity signals.

What would settle it

An independent measurement yielding a bulk density above 9 g cm^{-3} or an iron fraction above 80 percent under the same modeling assumptions would contradict the revised composition range.

Figures

Figures reproduced from arXiv: 2606.18355 by Casey L. Brinkman, Daniel Hey, Daniel Huber, Davide Gandolfi, Eleonora Armano, Ellen M. Price, Federica Chiti, Fei Dai, Gu{\dh}mundur Stef\'ansson, Heather A. Knutson, Jennifer L. van Saders, Jiayin Dong, Karen A. Collins, Kristine W.F. Lam, Leslie A. Rogers, Mathias Zechmeister, Michael Zhang, Nicholas Saunders, Rena A. Lee, Simon H. Albrecht, Te Han.

Figure 1
Figure 1. Figure 1: From left to right: SPOC PDCSAP, TGLC, and JWST photometry. Top: Binned (30-sec) and phase-folded light curve of GJ 367 confirming the transit signal of GJ 367 b (grey points). The best-fit transit model corresponding to each dataset (see Sec. 3.2) is overplotted. The blue shaded region in each panel is the adopted transit depth and 1σ uncertainty from the SPOC photometry fit, showing the transit depths ar… view at source ↗
Figure 2
Figure 2. Figure 2: Radial Velocity (RV) variation of GJ 367 observed with Left: ESPRESSO (black diamonds) and Right: ESPRESSO + HARPS (grey circles). For both left and right plots, panel a) shows the time-seies RV measurements. The best-fit radvel Gaussian Process (GP) single-Keplerian model for the ESPRESSO + HARPS combined dataset (grey line) used to remove stellar and instrumental correlated noise (see Sec. 4) is shown in… view at source ↗
Figure 3
Figure 3. Figure 3: Left: Mass-radius diagram of exoplanets with < 35% mass measurement uncertainty, taken from the NASA Exoplanet Archivea . The adopted RV mass and transit radius measurements of GJ 367 b from this work (teal star) are shown with those from previous works (light blue points). The teal outlined star represents the volumetric radius if we assume tidal distortion according to Love’s theory (see Sec. 5). The mod… view at source ↗
Figure 4
Figure 4. Figure 4: Top: Mass vs. core mass fraction (CMF) and Bottom: mass vs. planet density error as a function of radial aspect ratio (color bars) from tidal distortion. We show the measured mass of GJ 367 b (0.503 ± 0.078 M⊕) as the grey shaded region. We adopt the Fe–pv–en (iron core surrounded by perovskite-enstatite mantle) composition in the right panel of [PITH_FULL_IMAGE:figures/full_fig_p013_4.png] view at source ↗
Figure 5
Figure 5. Figure 5: Contamination factor (%) from SPOC PDCSAP and TGLC light curves for each TESS sector. APPENDIX We compared the sector-wise contamination factors computed from both SPOC and TGLC. The contamination factor is from both pipelines is simply the total flux from nearby stars divided by the total flux from the target star within the pipeline’s aperture. The TGLC pipeline uses a fixed 3x3 pixel aperture while the … view at source ↗
read the original abstract

We report revised mass and radius measurements for GJ 367 b, an ultra-short-period (7.7 hr) sub-Earth in a multi-planet system orbiting a nearby (~9 pc) M dwarf host. Previous mass and radius measurements have suggested GJ 367 b has an anomalously high bulk density, close to that of solid iron. The existence of such an iron-rich planet is in tension with established planet formation scenarios. We utilized newly available TESS short-cadence photometry to constrain the radius of GJ 367 b to 0.736 +/- 0.035 R_Earth. We consider observational and modeling effects such as photometric dilution, stellar activity, and tidal distortion to account for possible inaccuracies in the star and planet radius measurements. From our radial velocity (RV) analysis using VLT/ESPRESSO data covering nearly the full orbit in a single night, we find a mass of 0.503 +/- 0.078 M_Earth, corresponding to a bulk density of 6.9 +1.6/-1.4 g cm-1. We present a new tidal distortion and interior composition modeling framework to assess the iron mass fraction of GJ 367 b. Considering several different interior composition assumptions and radial aspect ratios, we find an iron fraction of ~50-70%, which is broadly consistent with that of Mercury and not as iron rich as previously suggested.

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

1 major / 2 minor

Summary. The manuscript reports revised mass (0.503 ± 0.078 M⊕) and radius (0.736 ± 0.035 R⊕) for the ultra-short-period planet GJ 367 b from new ESPRESSO RV observations and TESS short-cadence photometry. Accounting for photometric dilution, stellar activity, and tidal distortion yields a bulk density of 6.9 +1.6/-1.4 g cm^{-3}. A new self-consistent tidal distortion and interior composition framework is presented, from which an iron mass fraction of ~50-70% is inferred across multiple assumptions and aspect ratios, indicating consistency with Mercury rather than an anomalously high iron content.

Significance. If the new tidal-interior framework is shown to be accurate, the work alleviates tension between the planet's properties and standard formation models. The self-consistent treatment of tidal distortion is a methodological advance over prior analyses, but its reliability is central to the revised iron-fraction conclusion.

major comments (1)
  1. [tidal distortion and interior composition modeling framework (abstract and associated methods section)] The headline result (iron fraction ~50-70%) rests on the new tidal distortion and interior composition framework (abstract, final paragraph) mapping the measured density to composition. No validation of this framework against known planets, synthetic injected signals, or a standard non-tidal interior code is described; without such tests, systematic shifts of even 5-10% in effective volume or density could move the inferred range outside the Mercury-like window.
minor comments (2)
  1. [Abstract] The abstract states that observational effects (photometric dilution, stellar activity, tidal distortion) were considered but supplies no quantitative details on how these were propagated into the final mass, radius, and density uncertainties.
  2. [Abstract] No statement is made regarding code or data availability for the new tidal-interior model, which would aid reproducibility of the 50-70% iron-fraction range.

Simulated Author's Rebuttal

1 responses · 0 unresolved

We thank the referee for their constructive review. We address the major comment on validation of the tidal distortion and interior composition framework below.

read point-by-point responses

  1. Referee: [tidal distortion and interior composition modeling framework (abstract and associated methods section)] The headline result (iron fraction ~50-70%) rests on the new tidal distortion and interior composition framework (abstract, final paragraph) mapping the measured density to composition. No validation of this framework against known planets, synthetic injected signals, or a standard non-tidal interior code is described; without such tests, systematic shifts of even 5-10% in effective volume or density could move the inferred range outside the Mercury-like window.

    Authors: We agree that explicit validation tests would strengthen the manuscript. The framework is constructed to be self-consistent by solving the interior structure equations with tidal distortion included from the outset, and we demonstrate robustness across multiple composition assumptions and aspect ratios. However, the submitted version did not include direct comparisons to standard non-tidal codes or synthetic data injections. In revision we will add a new methods subsection with two validation exercises: (1) recovery of known iron fractions for Earth and Mercury when the framework is applied to their measured densities and radii, and (2) injection-recovery tests using synthetic photometry and RV data. These tests will quantify any systematic offsets in effective volume or density and confirm that the inferred 50-70% iron range is preserved. We view this as a straightforward and necessary addition that does not change the scientific conclusions. revision: yes

Circularity Check

0 steps flagged

Mass/radius from independent RV+photometry; iron fraction from new model with varied priors

full rationale

The paper derives mass (0.503 ± 0.078 M⊕) from ESPRESSO RV data and radius (0.736 ± 0.035 R⊕) from TESS photometry, computes density, then applies a new tidal-distortion + interior model across multiple composition assumptions and aspect ratios to obtain the 50-70% iron range. No equation or step reduces the iron fraction to a quantity defined by the same fitted parameters, no self-citation is load-bearing for the central claim, and the model is presented as an independent framework rather than a fit to this planet's data. The derivation chain remains self-contained against external benchmarks.

Axiom & Free-Parameter Ledger

0 free parameters · 0 axioms · 0 invented entities

Abstract alone supplies insufficient detail to enumerate specific free parameters, axioms, or invented entities; the iron-fraction range is presented as the output of an unspecified set of composition assumptions and aspect ratios.

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