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REVIEW 4 major objections 4 minor 146 references

The paper claims that giant impacts in compact planetary systems occur early, while the protoplanetary disk is still gas-rich, so collision remnants re-accrete their hydrogen envelopes.

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2026-08-01 12:09 UTC pith:SLRBT6VV

load-bearing objection A useful dynamical classifier, but the central claim about retained H envelopes rests on censored data and needs a survival analysis before it can carry the early-collision conclusion. the 4 major comments →

arxiv 2607.19632 v1 pith:SLRBT6VV submitted 2026-07-21 astro-ph.EP

Dynamically Selected Mass-Radius Relationship for Low Mass Exoplanets

Brad Hansen , Austin Mao This is my paper
classification astro-ph.EP
keywords mass-radius relationexoplanetsmean motion resonancesgiant impactshydrogen envelopessub-Neptunesdynamical instabilityphotoevaporation
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.

The paper asks whether planets that were later involved in giant impacts differ in composition from planets that escaped collisions. By classifying exoplanets according to their proximity to mean-motion resonances, the authors identify a 'pristine' sample and a 'collision product' sample. They find that collision products are heavier on average, but their hydrogen envelope fractions are no smaller than those of pristine planets. Since giant impacts are expected to strip away such envelopes, the preservation of envelopes points to an early timing: collisions must happen while gas from the protoplanetary disk is still available for re-accretion. This would favor formation models in which dynamical instability begins during disk dispersal rather than long after the gas is gone.

Core claim

On the paper's own terms, the central discovery is that planets whose orbital architectures indicate a past giant impact are systematically more massive than planets that stayed near resonance, yet they carry hydrogen envelopes of comparable mass fraction. This combination—extra mass without envelope loss—cannot be explained by collisions occurring in a gas-free environment, because the energy of a planetary-scale impact would unbind the envelope. The authors interpret the result as evidence that most collisions occurred early, while the dissipating protoplanetary disk could still resupply gas to the collision remnants, and that the observed mass–radius relation of compact systems is shaped

What carries the argument

The paper's load-bearing tool is Δ, defined as the fractional deviation of an observed period ratio from the nearest first-order commensurability (k+1)/k, such as 3:2 or 4:3. N-body simulations of unstable resonant chains—starting from compact chains with randomized resonant angles—map values of Δ to the probability that a planet has undergone a collision. A k-nearest-neighbour classifier trained on these simulations then assigns each observed planet a probability of being pristine or a collision product, and the mass–radius diagrams and inferred hydrogen mass fractions of the two classes are compared.

Load-bearing premise

The central load-bearing premise is that the mapping from period-ratio deviation Δ to collision history, learned from N-body simulations of unstable resonant chains, applies to real systems—so other processes that also shift period ratios (photoevaporation, tidal damping, planetesimal scattering, undetected planets) do not masquerade as collisions.

What would settle it

A single well-measured planet classified as a collision product whose hydrogen envelope fraction is decisively lower than that of pristine planets of the same mass—or a young post-instability system observed before any re-accretion could occur—would contradict the claim that collisions happen early enough for envelope recapture.

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

If this is right

  • The 'breaking-the-chains' model, which puts most dynamical instability after the gas disk has dispersed, is contradicted; magnetospheric rebound models, which drive instability during disk dispersal, are more consistent with the observed envelope fractions.
  • Rocky planets more massive than about three Earth masses are likely the photoevaporated cores of planets that originally had volatile envelopes, rather than primordial rocky bodies.
  • The mass distribution of collision products is consistent with the random merging of two planets drawn from the pristine population, implying that collisions mostly occur between roughly equal-mass bodies.
  • The mass function of sub-Neptune planets shows a characteristic peak around 4.5 Earth masses, with a collision-generated tail toward higher masses.
  • Planets with masses above about 12 Earth masses and large radii (region C) form through a different pathway and should not be treated as products of the same collisional evolution.
  • The small sample of pristine planets shows a sharp split between a rocky branch below about 3 Earth masses and an envelope-bearing branch above it, suggesting a primordial mass threshold for gas accretion.

Where Pith is reading between the lines

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

  • The same Δ-based classifier could be extended to the full exoplanet catalog to identify candidate post-collision systems for atmospheric follow-up; transmission spectroscopy could verify whether their hydrogen envelopes really are as intact as inferred.
  • If collisions typically occur early, young stellar systems (a few million years old) that are just emerging from the disk phase might occasionally show planets still in the act of re-accreting gas, offering a direct test.
  • The paper's perfect-merging assumption ignores the possibility that debris from collisions is later re-accreted; the conclusion that envelope fractions do not decrease would need to be re-examined if extended collision cascades strip more gas than the models assume.
  • A population-level analysis combining the Δ classification with stellar age indicators could separate genuine early collisions from late ones, since the latter would show a deficit of hydrogen even if the average is masked by the pristine contribution.

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

4 major / 4 minor

Summary. This paper uses N-body simulations of resonant chain instabilities to define a quantitative boundary in the period-ratio deviation \Delta that separates planets that have experienced giant impacts ('collision products') from those that have not ('pristine'). Applying this classifier to observed multiplanet systems with measured masses and radii, the authors find that collision products are more massive than pristine planets, while Hydrogen envelope mass fractions are no smaller. They conclude that collisions must occur early, while disk gas remains, to allow re-accretion of envelopes. The mass-shift result is consistent with prior work; the envelope-retention claim is the new contribution.

Significance. The dynamical classification approach is a useful and physically motivated way to connect orbital architecture to collisional history. If the early-collision conclusion is robust, it would discriminate between 'breaking-the-chains' and magnetospheric rebound formation models, and is therefore of broad interest. The paper is commendably transparent about several limitations, including the use of upper limits and the ambiguity of classifications. However, the central new claim rests on a comparison that does not properly handle censored data, and on post-hoc exclusion of planets that contradict the hypothesis. With the current analysis, the conclusion is suggestive rather than quantitatively established.

major comments (4)
  1. [§4.2, Figure 10] The statement that collision products have H envelope mass fractions 'no smaller' than pristine planets is asserted from visual inspection of f_H estimates, many of which are upper limits. Because the collision-product sample is systematically more massive (Figure 9), and high-mass planets are more likely to fall below the Lopez & Fortney (2014) grid, the censoring is differential. Treating upper limits as scatter points can conceal a real deficit in collision-product f_H. A survival analysis or a mass-matched comparison that treats upper limits as censored is required before the early-collision conclusion in §5 can be supported.
  2. [§4.3, Region C] Region C planets (M>12 M⊕, large radii) are excluded from the collision-product sample in Figures 9 and 10 because they are deemed to require a different formation channel. However, these planets were originally classified as collision products by the Δ classifier. Excluding them after the fact because they do not show envelope depletion is circular, as it removes the most direct counterexamples to the claim. An independent criterion for exclusion, or an analysis that includes them, is needed to avoid biasing the central comparison.
  3. [§4.1, Figure 9] The claim that the collision-product mass distribution is consistent with random pair mergers of the pristine population is based on visual comparison with a simulated pair-combination histogram. No statistical test (e.g., two-sample Kolmogorov–Smirnov test) is provided, despite sample sizes of only 27 and 35. A quantitative test is necessary to support the merger interpretation and to solidify the mass-shift result that underpins the paper's first conclusion.
  4. [§3, K-NN classification] The pristine/collision classifier is trained on the authors' N-body simulations (§2.1) with specific initial conditions and total masses 9.75–30 M⊕. Deployed on observed planets up to 100 M⊕, it requires extrapolation beyond the training set. Although outliers are flagged, no sensitivity analysis is presented to show that the results are robust to the choice of probability threshold (75%), K-NN parameters, or the inclusion of extrapolated points. This is particularly important because the early-collision conclusion depends on the classification of the most massive planets, which are most likely to lie outside the simulation range.
minor comments (4)
  1. [Figure 1 caption] Typo: 'probablity' should be 'probability'.
  2. [§2.1, text near Figure 2] The phrase 'the lower panel' appears twice; the first instance should be 'the upper panel' when referring to outer planets.
  3. [§4.4] The mass range '5–7M ⊙' should be '5–7M ⊕' (also in the same paragraph, 'M⊙' should be 'M⊕').
  4. [Table 2] The entry 'W ASP-47 d' contains an extra space and should read 'WASP-47 d'.

Circularity Check

0 steps flagged

No significant circularity: the dynamical classification is a forward-model calibration, and the f_H comparison is an independent empirical test.

full rationale

The paper's central claim is an empirical comparison of masses and H-envelope fractions between dynamically selected samples. The Δ-based classifier is trained on N-body simulations that label planets as pristine or collision products using only orbital dynamics; the labels are not derived from the observed masses, radii, or f_H values. The simulation's assumption that collisions are perfect mergers preserving composition does not enter the Δ-to-collision mapping in a way that forces the observed f_H similarity, since classification uses only period ratios, not composition. The exclusion of Region C planets from some mass comparisons is motivated by their dynamical outlier status (magenta circles) and by external occurrence-rate arguments, not by the envelope-retention hypothesis itself; including them would, if anything, raise the collision-product f_H, so the exclusion does not manufacture the 'no smaller' result. The self-citations to Hansen et al. (2024, 2025) and Yu et al. (2023) are used to interpret the result within a preferred formation model, but the observational finding does not depend on those citations. The paper also flags limitations (censored f_H upper limits, possible undetected planets inflating Δ, alternative mechanisms) rather than hiding them. No equation or fitted parameter is equivalent by construction to the claimed conclusion.

Axiom & Free-Parameter Ledger

4 free parameters · 5 axioms · 0 invented entities

The paper's central inference rests on a simulation-to-observation transfer: the Δ classifier is trained on self-generated N-body outcomes with hand-picked initial conditions, then applied to a heterogeneous observed catalog. Several region boundaries (A, B, C) are drawn post hoc from the data. No new physical entities are introduced.

free parameters (4)
  • pristine/collision Δ threshold = |Δ|≈0.01 (both neighbors); |Δ_out|<0.01 for inner planets; |Δ_in|<0.025 for outer planets
    Chosen by eye from the simulated collision/no-collision distributions in Figures 1–2; not derived from an external benchmark. It directly determines which observed planets are labeled pristine vs collision products.
  • K-NN classification hyperparameters = k=25, probability >75%, Gaussian weighting in log|Δ| space
    Chosen from the simulation training set (N=2665); classification threshold 75% is arbitrary. The resulting class labels drive all subsequent mass-radius comparisons.
  • Simulation initial condition parameters = N=5–8, total masses 9.75/15/30 M⊕, q=1–5, e dispersion 0.05, inclinations 0–0.5°, 2 Myr integration
    These choices set the training distribution for the collision classifier. If real initial architectures differ, the Δ→collision mapping is biased. Not fitted to observed data, but not externally validated either.
  • Upper-limit floor for H mass fraction = f_H = 0.01%
    Assigned when measured mass/radius fall below the Lopez & Fortney grid; used for many planets in Figure 10, so the 'no smaller' claim rests partly on a floor value rather than measurements.
axioms (5)
  • domain assumption Proximity to first-order mean-motion resonance (small Δ) marks planets that have not undergone late giant impacts.
    All classifications are built on this mapping, calibrated only by the authors' own simulations (§2.1, Fig. 1–2). Real systems may have Δ altered by resonant repulsion, photoevaporation, or planetesimal scattering (§3.3), breaking the mapping.
  • domain assumption The observed multiplanet sample is drawn from the same distribution as the simulated resonant chains (N=5–8, q=1–5, total masses 9.75–30 M⊕, randomized angles).
    K-NN trained on these synthetic systems is applied to observed systems (§3). If real formation pathways differ (e.g., in-situ assembly, different migration histories), the classifier is biased.
  • domain assumption Giant impacts strip H envelopes but perfectly merge rocky cores.
    Used in §4.2 to interpret the mass and envelope differences. The authors cite impact simulations but note in §5 that long-term consequences, core heating, and H sequestration are uncertain.
  • ad hoc to paper Region C planets (>12 M⊕ with large radii) are a separate formation channel and can be excluded from the collision-product analysis.
    In §3.2 and §4.3 they are removed because they would require increased H inventories during a collision—an inference from the same mass-radius pattern the paper is trying to interpret.
  • domain assumption Rocky planets >3 M⊕ in Region A are mostly photoevaporated cores, not collision remnants.
    Based on the irradiation grouping in Fig. 8, this is a post-hoc reinterpretation of planets that do not fit the pristine branch; it is supported by the radius-valley location but not independently tested.

pith-pipeline@v1.3.0-alltime-deepseek · 27383 in / 15303 out tokens · 150038 ms · 2026-08-01T12:09:22.696197+00:00 · methodology

0 comments
read the original abstract

We study the mass-radius relationship of planets in multiplanet systems as a function of their dynamical architecture. We isolate those planets whose proximity to resonance indicates that they have not undergone significant dynamical instability since formation, and therefore have not experienced a late giant impact with another planet. We compare the properties of these planets to those whose orbital architectures suggest a high probability of having experienced a giant impact. We find that planets that are likely to have experienced an impact are, on average, more massive than those that did not -- consistent with prior claims. However, we find that the Hydrogen envelope mass fractions of these planets are no smaller than those of planets that did not experience collisions. Taken together, these findings suggest that dynamical evolution and planetary collisions are an integral part of the evolution of compact planetary systems, but that they must occur early enough that collisional remnants are still able to recapture gaseous envelopes from the dissipating protoplanetary disk.

Figures

Figures reproduced from arXiv: 2607.19632 by Austin Mao, Brad Hansen.

Figure 1
Figure 1. Figure 1: — The black open points represent planets that do not experience a collision during the dynamical evolution of the reso￾nant chain. The open red points indicate planets that did experi￾ence a collision, resulting from instabilities that occur during the dynamical evolution. The blue dotted lines delineate the approxi￾mate transition (|∆| = 0.01) between regimes where the majority has/has not experienced a … view at source ↗
Figure 2
Figure 2. Figure 2: — The solid points in the upper panel show the fraction of planets in each bin of |∆| that managed to avoid a collision during the dynamical instability of compact planetary systems. The error bars indicated Poisson counting errors. This panel represents the surviving outer planets in each chain. The lower panel shows the equivalent fraction for the surviving inner planets of these chains. The horizontal d… view at source ↗
Figure 3
Figure 3. Figure 3: — The red solid points represent observed planets with probability p > 0.75 of having survived without undergoing a col￾lision. The blue solid circles represent observed systems with a probability p > 0.75 of having undergone a collision in their evo￾lutionary history. The crosses represent systems that cannot be classified securely into either camp. We also highlight, with ma￾genta circles, those systems … view at source ↗
Figure 6
Figure 6. Figure 6: — The solid black points are those for which our model cannot confidently assign to either the pristine or collision groups. We see that the region A is better populated than in either of the other two plots, but region B is not. As in [PITH_FULL_IMAGE:figures/full_fig_p007_6.png] view at source ↗
Figure 7
Figure 7. Figure 7: — The upper panel shows the properties of the outermost planets in our observed resonant chains. The red points indicate planets that have likely to have not experienced a collision, while the blue points have a probability of having experienced a collision. The lower panel shows the properties of the innermost planets in the chains, with a similar colour scheme. In both panels, the re￾gions labelled A, B … view at source ↗
Figure 8
Figure 8. Figure 8: — Each point shows a radius of a planet in our sample, plotted against the flux incident on the planet from the host star (measured in units of Earth’s Solar irradiance). The sample shown here is the cumulative sum of Tables 1, 2, 3, 4 and 5. The red points indicate those points that fall within box A and the blue points those that fall within box B. The magenta points fall in region C. The dashed line sho… view at source ↗
Figure 10
Figure 10. Figure 10: — The black points represent the Hydrogen atmosphere mass fractions, as a function of mass, for the pristine population from Tables 1 and 5. The red points represent the corresponding mass fractions for the collision products from Tables 2 and 5. Open red points are from the unassigned planets in [PITH_FULL_IMAGE:figures/full_fig_p010_10.png] view at source ↗
Figure 11
Figure 11. Figure 11: — The solid histogram represents the mass function of planets from Tables 1, 2, 3, 4 and 5, excepting those massive plan￾ets that lie in region C – which we assert must have formed from a different mechanism (see discussion in the text). The dotted his￾togram represents a gaussian distribution centered at 4.5 M⊕, with a dispersion of 1.3M⊕. The dashed histogram arises if we add a contribution of equivalen… view at source ↗
Figure 12
Figure 12. Figure 12: shows the properties of planets in Ta￾ble 1, [PITH_FULL_IMAGE:figures/full_fig_p012_12.png] view at source ↗

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Works this paper leans on

146 extracted references · 2 canonical work pages · 2 internal anchors

  1. [1]

    , keywords =

    Mass-Radius Relationships for Solid Exoplanets. , keywords =. doi:10.1086/521346 , archivePrefix =. 0707.2895 , primaryClass =

    Pith/arXiv arXiv

  2. [2]

    , keywords =

    Understanding the Mass-Radius Relation for Sub-neptunes: Radius as a Proxy for Composition. , keywords =. doi:10.1088/0004-637X/792/1/1 , archivePrefix =. 1311.0329 , primaryClass =

    Pith/arXiv arXiv

  3. [3]

    PSJ , keywords =

    Refining the Transit-timing and Photometric Analysis of TRAPPIST-1: Masses, Radii, Densities, Dynamics, and Ephemerides. PSJ , keywords =. doi:10.3847/PSJ/abd022 , archivePrefix =. 2010.01074 , primaryClass =

    Pith/arXiv arXiv 2010

  4. [4]

    , keywords =

    The Mass-Radius Relation for 65 Exoplanets Smaller than 4 Earth Radii. , keywords =. doi:10.1088/2041-8205/783/1/L6 , archivePrefix =. 1312.0936 , primaryClass =

    Pith/arXiv arXiv 2041

  5. [5]

    The Kepler Giant Planet Search. I. A Decade of Kepler Planet-host Radial Velocities from W. M. Keck Observatory. , keywords =. doi:10.3847/1538-4365/ad0cab , archivePrefix =. 2304.00071 , primaryClass =

    Pith/arXiv arXiv

  6. [6]

    , keywords =

    Planet Masses, Radii, and Orbits from NASA's K2 Mission. , keywords =. doi:10.3847/1538-4365/adc5e4 , archivePrefix =. 2502.04436 , primaryClass =

    Pith/arXiv arXiv

  7. [7]

    , keywords =

    A Five-Planet Resonant Chain: Reevaluation of the Kepler-80 System. , keywords =. doi:10.3847/1538-3881/ac12d5 , archivePrefix =. 2107.05597 , primaryClass =

    Pith/arXiv arXiv

  8. [8]

    Update on the mass-radius relationship of 34 Kepler planets

    Removing biases on the density of sub-Neptunes characterised via transit timing variations. Update on the mass-radius relationship of 34 Kepler planets. , keywords =. doi:10.1051/0004-6361/202244132 , archivePrefix =. 2207.07456 , primaryClass =

    Pith/arXiv arXiv

  9. [9]

    , keywords =

    A resonant sextuplet of sub-Neptunes transiting the bright star HD 110067. , keywords =. doi:10.1038/s41586-023-06692-3 , archivePrefix =. 2311.17775 , primaryClass =

    Pith/arXiv arXiv

  10. [10]

    , keywords =

    A resonant chain of four transiting, sub-Neptune planets. , keywords =. doi:10.1038/nature17445 , archivePrefix =. 1612.07376 , primaryClass =

    Pith/arXiv arXiv

  11. [11]

    , keywords =

    Exoplanet characterisation in the longest known resonant chain: the K2-138 system seen by HARPS. , keywords =. doi:10.1051/0004-6361/201936267 , archivePrefix =. 1909.13527 , primaryClass =

    Pith/arXiv arXiv 1909

  12. [12]

    SPORES-HWO. II. Companion Mass Limits and Updated Planet Properties for 120 Future Exoplanet Imaging Targets from 35 yr of Precise Doppler Monitoring. , keywords =. doi:10.3847/1538-3881/ae0b62 , archivePrefix =. 2409.10679 , primaryClass =

    arXiv

  13. [13]

    , keywords =

    A Fourth Planet in the Kepler-51 System Revealed by Transit Timing Variations. , keywords =. doi:10.3847/1538-3881/ad83d3 , archivePrefix =. 2410.01625 , primaryClass =

    Pith/arXiv arXiv

  14. [14]

    The TESS-Keck Survey. XX. 15 New TESS Planets and a Uniform RV Analysis of All Survey Targets. , keywords =. doi:10.3847/1538-4365/ad4484 , archivePrefix =. 2405.14786 , primaryClass =

    Pith/arXiv arXiv

  15. [15]

    , keywords =

    The minimum-mass extrasolar nebula: in situ formation of close-in super-Earths. , keywords =. doi:10.1093/mnras/stt424 , archivePrefix =. 1211.1673 , primaryClass =

    Pith/arXiv arXiv

  16. [16]

    , keywords =

    Migration Then Assembly: Formation of Neptune-mass Planets inside 1 AU. , keywords =. doi:10.1088/0004-637X/751/2/158 , archivePrefix =. 1105.2050 , primaryClass =

    Pith/arXiv arXiv 2050

  17. [17]

    , keywords =

    Testing in Situ Assembly with the Kepler Planet Candidate Sample. , keywords =. doi:10.1088/0004-637X/775/1/53 , archivePrefix =. 1301.7431 , primaryClass =

    Pith/arXiv arXiv

  18. [18]

    Toward a Deterministic Model of Planetary Formation. V. Accumulation Near the Ice Line and Super-Earths. , keywords =. doi:10.1086/590401 , adsurl =

    doi:10.1086/590401

  19. [19]

    Toward a Deterministic Model of Planetary Formation. VI. Dynamical Interaction and Coagulation of Multiple Rocky Embryos and Super-Earth Systems around Solar-type Stars. , keywords =. doi:10.1088/0004-637X/719/1/810 , archivePrefix =. 1006.2584 , primaryClass =

    Pith/arXiv arXiv

  20. [20]

    , keywords =

    Architectures of Compact Super-Earth Systems Shaped by Instabilities. , keywords =. doi:10.3847/1538-3881/ac5961 , archivePrefix =. 2203.00801 , primaryClass =

    Pith/arXiv arXiv

  21. [21]

    , 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

  22. [22]

    , keywords =

    HD 23472: a multi-planetary system with three super-Earths and two potential super-Mercuries. , keywords =. doi:10.1051/0004-6361/202244293 , archivePrefix =. 2209.13345 , primaryClass =

    Pith/arXiv arXiv

  23. [23]

    Astronomische Nachrichten , keywords =

    Confirmation of a Non-Transiting Planet in the Habitable Zone of the Nearby M Dwarf L 98-59. Astronomische Nachrichten , keywords =. doi:10.1002/asna.70059 , archivePrefix =. 2507.06413 , primaryClass =

    Pith/arXiv arXiv

  24. [24]

    Nature Astronomy , keywords =

    Evidence for the volatile-rich composition of a 1.5-Earth-radius planet. Nature Astronomy , keywords =. doi:10.1038/s41550-022-01835-4 , archivePrefix =. 2212.08477 , primaryClass =

    Pith/arXiv arXiv

  25. [25]

    Exploring the robustness of transit-timing variations and radial velocity mass characterisations

    Photo-dynamical characterisation of the TOI-178 resonant chain. Exploring the robustness of transit-timing variations and radial velocity mass characterisations. , keywords =. doi:10.1051/0004-6361/202450212 , archivePrefix =. 2405.13732 , primaryClass =

    Pith/arXiv arXiv

  26. [26]

    , keywords =

    Kepler-79's Low Density Planets. , keywords =. doi:10.1088/0004-637X/785/1/15 , archivePrefix =. 1310.2642 , primaryClass =

    Pith/arXiv arXiv

  27. [27]

    , keywords =

    Mass determinations of the three mini-Neptunes transiting TOI-125. , keywords =. doi:10.1093/mnras/staa197 , archivePrefix =. 2001.08834 , primaryClass =

    Pith/arXiv arXiv 2001

  28. [28]

    , keywords =

    Following Up the Kepler Field: Masses of Targets for Transit Timing and Atmospheric Characterization. , keywords =. doi:10.3847/1538-3881/abd93f , archivePrefix =. 2101.01202 , primaryClass =

    Pith/arXiv arXiv

  29. [29]

    , keywords =

    TOI-663: A newly discovered multi-planet system with three transiting mini-Neptunes orbiting an early M star. , keywords =. doi:10.1051/0004-6361/202346899 , adsurl =

    doi:10.1051/0004-6361/202346899

  30. [30]

    , keywords =

    Transit timings variations in the three-planet system: TOI-270. , keywords =. doi:10.1093/mnras/stab3483 , archivePrefix =. 2308.10763 , primaryClass =

    Pith/arXiv arXiv

  31. [31]

    , keywords =

    Mass determination of the three long-period Neptune- and sub-Neptune-sized planets transiting TOI-282. , keywords =. doi:10.1051/0004-6361/202556791 , archivePrefix =. 2511.05147 , primaryClass =

    arXiv

  32. [32]

    , keywords =

    Hyades Member K2-136c: The Smallest Planet in an Open Cluster with a Precisely Measured Mass. , keywords =. doi:10.3847/1538-3881/acca1c , archivePrefix =. 2304.02779 , primaryClass =

    Pith/arXiv arXiv

  33. [33]

    , keywords =

    HARPS-N radial velocities confirm the low densities of the Kepler-9 planets. , keywords =. doi:10.1093/mnras/stz181 , archivePrefix =. 1901.05471 , primaryClass =

    Pith/arXiv arXiv 1901

  34. [34]

    Nature Astronomy , keywords =

    An adolescent and near-resonant planetary system near the end of photoevaporation. Nature Astronomy , keywords =. doi:10.1038/s41550-026-02795-9 , archivePrefix =. 2603.02550 , primaryClass =

    arXiv

  35. [35]

    , keywords =

    Updated Mass, Eccentricity, and Tidal Heating Constraints for the Earth-sized Planet LP 791-18 d. , keywords =. doi:10.3847/1538-3881/addf2d , archivePrefix =. 2501.18700 , primaryClass =

    Pith/arXiv arXiv

  36. [36]

    , keywords =

    Tidally Heated Sub-Neptunes, Refined Planetary Compositions, and Confirmation of a Third Planet in the TOI-1266 System. , keywords =. doi:10.3847/1538-3881/adc0fe , archivePrefix =. 2409.16374 , primaryClass =

    Pith/arXiv arXiv

  37. [37]

    , keywords =

    Unveiling the internal structure and formation history of the three planets transiting HIP 29442 (TOI-469) with CHEOPS. , keywords =. doi:10.1051/0004-6361/202450472 , archivePrefix =. 2406.18653 , primaryClass =

    Pith/arXiv arXiv

  38. [38]

    , keywords =

    Architecture of TOI-561 planetary system. , keywords =. doi:10.1093/mnras/stae2440 , archivePrefix =. 2410.18169 , primaryClass =

    arXiv

  39. [39]

    , keywords =

    Discovery of a cold giant planet and mass measurement of a hot super-Earth in the multi-planetary system WASP-132. , keywords =. doi:10.1051/0004-6361/202348177 , archivePrefix =. 2406.15986 , primaryClass =

    Pith/arXiv arXiv

  40. [40]

    No excess of cold Jupiters in small planet systems

    Cold Jupiters and improved masses in 38 Kepler and K2 small planet systems from 3661 HARPS-N radial velocities. No excess of cold Jupiters in small planet systems. , keywords =. doi:10.1051/0004-6361/202346211 , archivePrefix =. 2304.05773 , primaryClass =

    Pith/arXiv arXiv

  41. [41]

    Nature Astronomy , keywords =

    Transit detection of the long-period volatile-rich super-Earth ^ 2 Lupi d with CHEOPS. Nature Astronomy , keywords =. doi:10.1038/s41550-021-01381-5 , archivePrefix =. 2106.14491 , primaryClass =

    Pith/arXiv arXiv

  42. [42]

    , keywords =

    Discovery of TOI-1260d and the characterization of the multiplanet system. , keywords =. doi:10.1093/mnras/stac3639 , archivePrefix =. 2212.04307 , primaryClass =

    Pith/arXiv arXiv

  43. [43]

    , keywords =

    Three planets transiting the evolved star EPIC 249893012: a hot 8.8-M _ super-Earth and two warm 14.7 and 10.2-M _ sub-Neptunes. , keywords =. doi:10.1051/0004-6361/201937080 , archivePrefix =. 2002.01755 , primaryClass =

    Pith/arXiv arXiv 2002

  44. [44]

    , keywords =

    TOI-4010: A System of Three Large Short-period Planets with a Massive Long-period Companion. , keywords =. doi:10.3847/1538-3881/acd537 , archivePrefix =. 2306.05308 , primaryClass =

    Pith/arXiv arXiv

  45. [45]

    , keywords =

    Kepler-411: a four-planet system with an active host star. , keywords =. doi:10.1051/0004-6361/201834275 , archivePrefix =. 1902.09719 , primaryClass =

    Pith/arXiv arXiv 1902

  46. [46]

    , keywords =

    The Occurrence and Architecture of Exoplanetary Systems. , keywords =. doi:10.1146/annurev-astro-082214-122246 , archivePrefix =. 1410.4199 , primaryClass =

    Pith/arXiv arXiv

  47. [47]

    , keywords =

    Detection of transits of the nearby hot Neptune GJ 436 b. , keywords =. doi:10.1051/0004-6361:20077799 , archivePrefix =. 0705.2219 , primaryClass =

    Pith/arXiv arXiv

  48. [48]

    , keywords =

    A super-Earth transiting a nearby low-mass star. , keywords =. doi:10.1038/nature08679 , archivePrefix =. 0912.3229 , primaryClass =

    Pith/arXiv arXiv

  49. [49]

    , keywords =

    All Six Planets Known to Orbit Kepler-11 Have Low Densities. , keywords =. doi:10.1088/0004-637X/770/2/131 , archivePrefix =. 1303.0227 , primaryClass =

    Pith/arXiv arXiv

  50. [50]

    , keywords =

    Revisiting ^ 1 Cancri e: A New Mass Determination of the Transiting Super-Earth. , keywords =. doi:10.1088/0004-637X/759/1/19 , archivePrefix =. 1208.5709 , primaryClass =

    Pith/arXiv arXiv

  51. [51]

    Architecture of Kepler's Multi-transiting Systems. II. New Investigations with Twice as Many Candidates. , keywords =. doi:10.1088/0004-637X/790/2/146 , archivePrefix =. 1202.6328 , primaryClass =

    Pith/arXiv arXiv

  52. [52]

    , keywords =

    Architecture and Dynamics of Kepler's Candidate Multiple Transiting Planet Systems. , keywords =. doi:10.1088/0067-0049/197/1/8 , archivePrefix =. 1102.0543 , primaryClass =

    Pith/arXiv arXiv

  53. [53]

    , keywords =

    Breaking the chains: hot super-Earth systems from migration and disruption of compact resonant chains. , keywords =. doi:10.1093/mnras/stx1232 , archivePrefix =. 1703.03634 , primaryClass =

    Pith/arXiv arXiv

  54. [54]

    Hot super-Earth systems from breaking compact resonant chains

    Formation of planetary systems by pebble accretion and migration. Hot super-Earth systems from breaking compact resonant chains. , keywords =. doi:10.1051/0004-6361/201935336 , archivePrefix =. 1902.08772 , primaryClass =

    Pith/arXiv arXiv 1902

  55. [55]

    Dynamical rearrangement of super-Earths during disk dispersal. I. Outline of the magnetospheric rebound model. , keywords =. doi:10.1051/0004-6361/201630017 , archivePrefix =. 1702.02059 , primaryClass =

    Pith/arXiv arXiv

  56. [56]

    Dynamical rearrangement of super-Earths during disk dispersal. II. Assessment of the magnetospheric rebound model for planet formation scenarios. , keywords =. doi:10.1051/0004-6361/201730882 , archivePrefix =. 1708.01275 , primaryClass =

    Pith/arXiv arXiv

  57. [57]

    , keywords =

    Halting migration in magnetospherically sculpted protoplanetary discs. , keywords =. doi:10.1093/mnras/stad1636 , archivePrefix =. 2210.13674 , primaryClass =

    Pith/arXiv arXiv

  58. [58]

    The Open Journal of Astrophysics , keywords =

    Widespread disruption of resonant chains during protoplanetary disk dispersal. The Open Journal of Astrophysics , keywords =. doi:10.33232/001c.121410 , archivePrefix =. 2405.12388 , primaryClass =

    Pith/arXiv arXiv

  59. [59]

    arXiv e-prints , keywords =

    Dynamical Excitation as a probe of planetary origins. arXiv e-prints , keywords =. doi:10.48550/arXiv.2510.01332 , archivePrefix =. 2510.01332 , primaryClass =

    doi:10.48550/arxiv.2510.01332

  60. [60]

    , keywords =

    Repelling Planet Pairs by Ping-pong Scattering. , keywords =. doi:10.3847/1538-4357/ad5a09 , archivePrefix =. 2405.08893 , primaryClass =

    Pith/arXiv arXiv

  61. [61]

    , keywords =

    Planetesimal Interactions Can Explain the Mysterious Period Ratios of Small Near-Resonant Planets. , keywords =. doi:10.1088/0004-637X/803/1/33 , archivePrefix =. 1406.0521 , primaryClass =

    Pith/arXiv arXiv

  62. [62]

    , keywords =

    Sensitivity bias in the mass-radius distribution from transit timing variations and radial velocity measurements. , keywords =. doi:10.1093/mnras/stw241 , archivePrefix =. 1510.04750 , primaryClass =

    Pith/arXiv arXiv

  63. [63]

    , keywords =

    The Planetary Mass-Radius Relation and Its Dependence on Orbital Period as Measured by Transit Timing Variations and Radial Velocities. , keywords =. doi:10.3847/2041-8213/aa67eb , archivePrefix =. 1703.07790 , primaryClass =

    Pith/arXiv arXiv 2041

  64. [64]

    , keywords =

    Kepler Planet Masses and Eccentricities from TTV Analysis. , keywords =. doi:10.3847/1538-3881/aa71ef , archivePrefix =. 1611.03516 , primaryClass =

    Pith/arXiv arXiv

  65. [65]

    , keywords =

    Planetary Mass Determinations from a Simplified Photodynamical Model Application to the Complete Kepler Dataset. , keywords =. doi:10.3847/1538-3881/ad91a7 , archivePrefix =. 2410.11401 , primaryClass =

    Pith/arXiv arXiv

  66. [66]

    , keywords =

    Dearth of short-period Neptunian exoplanets: A desert in period-mass and period-radius planes. , keywords =. doi:10.1051/0004-6361/201528065 , archivePrefix =. 1602.07843 , primaryClass =

    Pith/arXiv arXiv

  67. [67]

    The California-Kepler Survey. X. The Radius Gap as a Function of Stellar Mass, Metallicity, and Age. , keywords =. doi:10.3847/1538-3881/ac51e3 , archivePrefix =. 2201.10020 , primaryClass =

    Pith/arXiv arXiv

  68. [68]

    The California-Kepler Survey. III. A Gap in the Radius Distribution of Small Planets. , keywords =. doi:10.3847/1538-3881/aa80eb , archivePrefix =. 1703.10375 , primaryClass =

    Pith/arXiv arXiv

  69. [69]

    , keywords =

    Kepler Planets: A Tale of Evaporation. , keywords =. doi:10.1088/0004-637X/775/2/105 , archivePrefix =. 1303.3899 , primaryClass =

    Pith/arXiv arXiv

  70. [70]

    , keywords =

    The Role of Core Mass in Controlling Evaporation: The Kepler Radius Distribution and the Kepler-36 Density Dichotomy. , keywords =. doi:10.1088/0004-637X/776/1/2 , archivePrefix =. 1305.0269 , primaryClass =

    Pith/arXiv arXiv

  71. [71]

    , keywords =

    Core-powered mass-loss and the radius distribution of small exoplanets. , keywords =. doi:10.1093/mnras/sty290 , archivePrefix =. 1708.01621 , primaryClass =

    Pith/arXiv arXiv

  72. [72]

    , keywords =

    Sculpting the valley in the radius distribution of small exoplanets as a by-product of planet formation: the core-powered mass-loss mechanism. , keywords =. doi:10.1093/mnras/stz1230 , archivePrefix =. 1811.03202 , primaryClass =

    Pith/arXiv arXiv

  73. [73]

    , keywords =

    The mass-radius relation of exoplanets revisited. , keywords =. doi:10.1051/0004-6361/202348690 , archivePrefix =. 2311.12593 , primaryClass =

    Pith/arXiv arXiv

  74. [74]

    , keywords =

    Probabilistic Forecasting of the Masses and Radii of Other Worlds. , keywords =. doi:10.3847/1538-4357/834/1/17 , archivePrefix =. 1603.08614 , primaryClass =

    Pith/arXiv arXiv

  75. [75]

    , keywords =

    The Mass of KOI-94d and a Relation for Planet Radius, Mass, and Incident Flux. , keywords =. doi:10.1088/0004-637X/768/1/14 , archivePrefix =. 1303.2150 , primaryClass =

    Pith/arXiv arXiv

  76. [76]

    , keywords =

    Revisiting K2-233 spectroscopic time-series with multidimensional Gaussian processes. , keywords =. doi:10.1093/mnras/stad1139 , archivePrefix =. 2304.06406 , primaryClass =

    Pith/arXiv arXiv

  77. [77]

    The TESS-Keck Survey. XI. Mass Measurements for Four Transiting Sub-Neptunes Orbiting K Dwarf TOI-1246. , keywords =. doi:10.3847/1538-3881/ac69e5 , archivePrefix =. 2204.11895 , primaryClass =

    Pith/arXiv arXiv

  78. [78]

    , keywords =

    Two Terrestrial Planet Families with Different Origins. , keywords =. doi:10.3847/1538-4357/ab2714 , archivePrefix =. 1811.07919 , primaryClass =

    Pith/arXiv arXiv

  79. [79]

    , keywords =

    Long-period Giant Companions to Three Compact, Multiplanet Systems. , keywords =. doi:10.3847/1538-3881/ab0899 , archivePrefix =. 1903.07186 , primaryClass =

    Pith/arXiv arXiv 1903

  80. [80]

    , year = 1996, month = nov, volume =

    Formation of the Giant Planets by Concurrent Accretion of Solids and Gas. , year = 1996, month = nov, volume =. doi:10.1006/icar.1996.0190 , adsurl =

    arXiv 1996

Showing first 80 references.