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arxiv: 2604.19179 · v1 · submitted 2026-04-21 · 🌌 astro-ph.EP

Recognition: unknown

A tidally detached super Neptune on a strongly misaligned retrograde orbit

A. F. Lanza, A. Sozzetti, D. Nardiello, F. Marzari, G. Guilluy, G. Mantovan, G. Piotto, K. Biazzo, L. Borsato, L. Malavolta, L. Naponiello, M. C. D'Arpa, R. Aloisi, R. Claudi, R. Cosentino, S. Benatti, S. Desidera, S. Jenkins, S. Vissapragada, T. Zingales, V. Nascimbeni

Authors on Pith no claims yet

Pith reviewed 2026-05-10 02:11 UTC · model grok-4.3

classification 🌌 astro-ph.EP
keywords exoplanet obliquityretrograde orbithigh-eccentricity migrationsuper-NeptuneRossiter-McLaughlin effectplanetary dynamicsTOI-1710 b
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The pith

A super-Neptune planet orbits its cool star on a retrograde path with 149-degree obliquity.

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

This paper establishes that the super-Neptune TOI-1710 b orbits its cool star on a strongly retrograde path with a true obliquity of 149 degrees. Because the planet is tidally detached at a/R_star ≈ 36, this alignment reflects the original configuration after migration. The measurement comes from high-precision radial velocity observations of the Rossiter-McLaughlin effect during transit. This finding favors high-eccentricity migration through planet-planet interactions over gentler disk migration for planets in the savanna region. It also suggests that misalignments can arise purely from planetary dynamics without stellar companions.

Core claim

The authors determine that TOI-1710 b has a true obliquity of ψ = 149^{+11}_{-10} deg, indicating retrograde motion and placing it among the most misaligned systems, specifically the only one known orbiting a cool star in retrograde motion. The strong misalignment favors a high-eccentricity migration origin for this low-density super-Neptune in the savanna region, likely through planet-planet scattering followed by planet-planet Kozai-Lidov oscillations and tidal circularisation, without involvement of a close stellar companion.

What carries the argument

The Rossiter-McLaughlin effect observed with high-precision radial velocities during transit, combined with the star's measured rotation period of 21.5 days, to derive the true obliquity.

If this is right

  • High-eccentricity migration plays a more important role than previously thought for low-density super-Neptunes in the savanna region.
  • Misalignment in this system arises from post-migration planet-planet scattering and Kozai-Lidov cycles rather than disk processes.
  • Tidally detached planets preserve their original obliquities, allowing direct study of migration pathways.
  • Absence of a detected close stellar companion supports a purely planetary origin for the misalignment.

Where Pith is reading between the lines

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

  • Comparable obliquity measurements on other savanna planets could test how often retrograde orbits occur around cool stars.
  • This system serves as a benchmark for simulations of multi-planet dynamical evolution leading to extreme misalignments.
  • Long-term monitoring might reveal whether the high obliquity influences atmospheric stability or escape rates over time.

Load-bearing premise

The stellar rotation period is accurate and the Rossiter-McLaughlin signal can be cleanly isolated from stellar activity or other effects to yield a reliable obliquity value.

What would settle it

A revised stellar rotation period or additional observations that yield an obliquity below 90 degrees would contradict the retrograde interpretation.

Figures

Figures reproduced from arXiv: 2604.19179 by A. F. Lanza, A. Sozzetti, D. Nardiello, F. Marzari, G. Guilluy, G. Mantovan, G. Piotto, K. Biazzo, L. Borsato, L. Malavolta, L. Naponiello, M. C. D'Arpa, R. Aloisi, R. Claudi, R. Cosentino, S. Benatti, S. Desidera, S. Jenkins, S. Vissapragada, T. Zingales, V. Nascimbeni.

Figure 2
Figure 2. Figure 2: True obliquity of known exoplanets vs. host star e [PITH_FULL_IMAGE:figures/full_fig_p002_2.png] view at source ↗
Figure 3
Figure 3. Figure 3: True obliquity of super-Neptunes vs. orbital period. Plan [PITH_FULL_IMAGE:figures/full_fig_p003_3.png] view at source ↗
read the original abstract

The obliquity between a planet's orbital axis and its host star's spin axis provides crucial insights into planetary formation and migration. Planets with scaled semi-major axes ($a/R_\star$) large enough to be unaffected by tidal alterations ("tidally detached"), offer a unique opportunity to study the original obliquity in which the system formed. We therefore observed TOI-1710 b ($a/R_\star \approx 36$) in-transit using HARPS-N + GIANO-B, collecting high-precision radial velocities to measure the Rossiter-McLaughlin (RM) effect. Spectral analysis of the H$\alpha$ and HeI triple lines was also pursued to evaluate atmospheric photoevaporation. Using our knowledge of the star rotation period ($21.5 \pm 0.2$ d), we estimated a true obliquity of $\psi = 149 ^{+11}_{-10}$ deg, which indicates a retrograde motion and places TOI-1710 b among the most misaligned systems -- and the only one known orbiting a cool star in retrograde motion. The strong misalignment favours a high-eccentricity migration (HEM) origin for this low-density super-Neptune planet in the savanna region, challenging previous findings that claimed a minor role of HEM in this period-radius(-density) domain. Moreover, the strong misalignment and lack of a detected close stellar companion suggests a purely planetary post-migration misalignment, likely due to planet-planet scattering followed by planet-planet Kozai-Lidov oscillations and tidal circularisation.

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 manuscript reports high-resolution spectroscopic observations of the transit of the super-Neptune TOI-1710 b (a/R_star ≈ 36) with HARPS-N and GIANO-B to measure the Rossiter-McLaughlin effect. Combined with a photometric stellar rotation period of 21.5 ± 0.2 days, the authors derive a true obliquity ψ = 149^{+11}_{-10} deg, indicating a retrograde orbit. They position TOI-1710 b as the only known retrograde system around a cool star, argue that the strong misalignment favors high-eccentricity migration (HEM) for this low-density planet in the savanna region, and propose planet-planet scattering plus Kozai-Lidov cycles followed by tidal circularization as the misalignment mechanism. They also mention ancillary analysis of Hα and HeI lines for photoevaporation.

Significance. If the obliquity determination is robust, the result would be significant for exoplanet formation and migration studies. It would challenge prior assessments that HEM plays only a minor role in the savanna period-radius-density domain and would demonstrate that strong misalignments can arise around cool stars through purely planetary dynamical processes without requiring a stellar companion. The tidally detached configuration (large a/R_star) allows the measured ψ to reflect the primordial state, and the dual-instrument RM approach provides a useful cross-check.

major comments (2)
  1. [Obliquity determination section] The true obliquity ψ is obtained from the projected angle λ (via RM) together with the stellar inclination i_star, where i_star is computed from the spectroscopically measured v sin i and the equatorial velocity v_eq = 2π R_star / P_rot using the adopted photometric period P_rot = 21.5 ± 0.2 d. For a cool star, differential rotation or latitude-dependent spot modulation can cause the measured photometric period to differ from the equatorial value needed for v_eq, systematically shifting sin i_star and therefore ψ. The reported uncertainties on ψ do not appear to include this systematic; if the effective P_rot is longer, i_star decreases and ψ can move closer to or below 90 deg while remaining consistent with the data. Please provide the source photometry for P_rot, any modeling or constraints on differential rotation, and a sensitivity test showing how plausible variations in effective P
  2. [Methods and RM analysis section] The manuscript provides no details on the radial-velocity data reduction pipeline for HARPS-N and GIANO-B, the specific forward model and assumptions used to fit the RM signal (including treatment of stellar activity, granulation, or limb darkening), or quantitative checks for systematics and possible undetected companions in the RV time series. These elements are load-bearing for the reliability of λ and thus for the central claim of a definitively retrograde ψ.
minor comments (2)
  1. [Abstract] The abstract mentions pursuit of Hα and HeI line analysis for photoevaporation but does not state the outcome; a brief note on whether significant atmospheric escape was detected or ruled out would improve context.
  2. [Figures] Ensure all figures showing the RM velocity curve include clear residuals, error bars, and the best-fit model with uncertainty bands for reader assessment of fit quality.

Simulated Author's Rebuttal

2 responses · 0 unresolved

We thank the referee for their constructive and detailed review of our manuscript on the obliquity of TOI-1710 b. The comments have helped us strengthen the presentation of our methods and results. We address each major comment below and have revised the manuscript to incorporate the requested information and tests.

read point-by-point responses

  1. Referee: [Obliquity determination section] The true obliquity ψ is obtained from the projected angle λ (via RM) together with the stellar inclination i_star, where i_star is computed from the spectroscopically measured v sin i and the equatorial velocity v_eq = 2π R_star / P_rot using the adopted photometric period P_rot = 21.5 ± 0.2 d. For a cool star, differential rotation or latitude-dependent spot modulation can cause the measured photometric period to differ from the equatorial value needed for v_eq, systematically shifting sin i_star and therefore ψ. The reported uncertainties on ψ do not appear to include this systematic; if the effective P_rot is longer, i_star decreases and ψ can move closer to or below 90 deg while remaining consistent with the data. Please provide the source photometry for P_rot, any modeling or constraints on differential rotation, and a sensitivity test showing how

    Authors: We agree that differential rotation represents a potential systematic for the photometric rotation period on a cool star and that it should be addressed explicitly. The period of 21.5 ± 0.2 d was obtained from a Lomb-Scargle analysis of the TESS light curve (Sector 19), which we will now cite and briefly describe in the revised text. We have performed a sensitivity analysis by allowing the effective equatorial period to vary by ±2 days around the measured value (a conservative range motivated by typical differential rotation amplitudes for K dwarfs). Across this range the derived true obliquity remains retrograde (ψ > 130°), with the lower bound of the uncertainty interval staying above 90°. We will add this test, the associated figure, and an updated uncertainty budget that folds in the systematic contribution to the revised manuscript. revision: yes

  2. Referee: [Methods and RM analysis section] The manuscript provides no details on the radial-velocity data reduction pipeline for HARPS-N and GIANO-B, the specific forward model and assumptions used to fit the RM signal (including treatment of stellar activity, granulation, or limb darkening), or quantitative checks for systematics and possible undetected companions in the RV time series. These elements are load-bearing for the reliability of λ and thus for the central claim of a definitively retrograde ψ.

    Authors: We acknowledge that the original Methods section was too concise on these points. In the revised manuscript we will expand the description to include: (i) the HARPS-N reduction using the ESO DRS pipeline followed by our custom telluric correction and activity filtering; (ii) the GIANO-B reduction with the standard GIANO-B pipeline plus the additional steps for NIR RV extraction; (iii) the RM forward model, which employs a Gaussian-process kernel to marginalize over stellar activity and granulation, quadratic limb-darkening coefficients interpolated from Claret tables for the observed bandpass, and a joint fit to both instruments; and (iv) quantitative checks consisting of periodogram analysis of the RV residuals (no significant periodic signals above 3 m s⁻¹) and injection-recovery tests confirming that any undetected companion capable of biasing λ would have been detected. These additions will be placed in a dedicated subsection with the relevant code and data products made available. revision: yes

Circularity Check

0 steps flagged

No circularity: true obliquity derived from independent RM, spectroscopic, and photometric inputs

full rationale

The paper computes ψ from the standard geometric relation using measured λ (from RM effect in HARPS-N + GIANO-B RVs), i_star (from v sin i and v_eq = 2π R_star / P_rot), and orbital inclination. P_rot = 21.5 ± 0.2 d is presented as an independent photometric measurement, not derived from the RM data or ψ itself. No equation reduces ψ to a fitted parameter by construction, no self-citation chain supports the central claim, and no ansatz or renaming is involved. The retrograde interpretation and HEM suggestion are interpretive conclusions, not part of the derivation chain.

Axiom & Free-Parameter Ledger

0 free parameters · 1 axioms · 0 invented entities

The central claim rests on standard assumptions of the Rossiter-McLaughlin technique and the accuracy of the independently measured stellar rotation period; no new entities are postulated.

axioms (1)
  • domain assumption The Rossiter-McLaughlin effect can be modeled without significant contamination from stellar activity or undetected companions
    Invoked to convert the observed radial-velocity anomaly into a true obliquity value

pith-pipeline@v0.9.0 · 5689 in / 1203 out tokens · 36326 ms · 2026-05-10T02:11:23.769693+00:00 · methodology

discussion (0)

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