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REVIEW 3 major objections 5 minor 44 references

On the formation of super-Jupiters: Core Accretion or Gravitational Instability?

T0 review · 3 major / 5 minor · reviewed 2026-08-11 · deepseek-v4-flash

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Pith's one-line read Super-Jupiters can form by core accretion: their host disks carry at least as much total metal as Jupiter-forming disks.

desk verdict The paper's useful result is the robust directional claim that super-Jupiters do not form in metal-poor disks; the 'strong evidence' for core accretion is not supported by the paper's own Monte Carlo tests. read the letter →

arxiv 2412.06594 v1 pith:4L7MOSII submitted 2024-12-09 astro-ph.EP

M. Nguyen , V. Adibekyan This is my paper · ORCID
classification astro-ph.EP
keywords planetformationcoreaccretiongravitationalinstabilitysuper-Jupitershoststarmetallicitychemicalabundancesdiskmetalcontentexoplanet
verification ladder T0 review T1 audit T2 compute T3 formal

The pith

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

The reading

This paper asks whether super-Jupiters, planets roughly 4–13 times Jupiter's mass, can be built by the same core-accretion process that makes ordinary Jupiters, or whether their formation demands gravitational instability. The authors assemble 172 Jupiter-mass planets and 93 super-Jupiters, use the host stars' C, O, Mg, Si, and Fe abundances to estimate the total metal content of each protoplanetary disk, and compare the two groups. They find that super-Jupiter hosts have at least as much disk metal as Jupiter hosts and often slightly more, with mean total metal content above the proto-solar disk value. They take this as evidence that the metal budget does not rule out core accretion for the most massive giant planets, and they encourage modelers to test that conclusion.

What carries the argument

The central machinery is the stoichiometric model that turns stellar atmospheric abundances of C, O, Mg, Si, and Fe into Z, the mass fraction of heavy elements in planet-building solids, anchored to a modern solar composition reference. From Z the paper constructs Ztotal = Z × Mstar under a linear disk-mass–stellar-mass scaling, plus a conservative variant Z*_total = log(Z × Mstar) × σdisk that propagates the observed ~0.8 dex scatter in disk mass. The comparison between Jupiter and super-Jupiter groups is carried by two-sample t-tests, Kolmogorov–Smirnov and Anderson–Darling tests, and Monte Carlo draws that fold in abundance, stellar-mass, and disk-mass uncertainties.

What would settle it

Rebuild the analysis using only abundances from one homogeneous high-resolution survey for every host star and compare the mean Ztotal of the 4–13 Mjup group with the 1–4 Mjup group; if it is then lower, the paper's statistical claim is overturned. Separately, measure C, O, Mg, Si, and Fe in stars of fixed initial composition but different evolutionary states (for example, open-cluster stars of different masses); if the rock-forming element ratios change with evolution, the present-day-abundance premise fails.

Watch

Extended reading notes

Core claim

The paper's central claim is that stars hosting planets with masses above 4 Jupiter masses do not have metal-poor protoplanetary disks relative to stars hosting 1–4 Jupiter-mass planets. Using a stoichiometric model that converts atmospheric C, O, Mg, Si, and Fe abundances into Z, the metal mass fraction of planet-building material, and multiplying by stellar mass to approximate the disk's total metal content Ztotal, the authors report mean Z = 1.79 ± 0.58% for super-Jupiter hosts versus 1.63 ± 0.58% for Jupiter hosts, and mean Ztotal = 2.21 ± 0.84 versus 1.99 ± 0.69. A two-sample t-test on Ztotal gives p = 0.023, with Kolmogorov–Smirnov and Anderson–Darling tests also favoring distinct distributions, although Monte Carlo realizations that include the uncertainties do not always reach significance. The authors conclude that super-massive planets can plausibly form via core accretion; they note that 12 of 93 super-Jupiters have sub-solar disk metal content, where gravitational instability may still be needed.

Load-bearing premise

The load-bearing assumption is that the C, O, Mg, Si, and Fe measured in a host star's atmosphere today have the same relative amounts as the metals in its protoplanetary disk at the time the planets formed, so that present-day abundance ratios can stand in for the disk's primordial mix; if stellar evolution has changed those ratios, the estimated metal contents are unreliable and the comparison between the two planet groups collapses.

Editorial extensions

If this is right

  • The metal content of protoplanetary disks is not the bottleneck that rules out core accretion for planets above 4 Jupiter masses.
  • Earlier hints that super-Jupiter hosts are metal-poor likely came from using iron abundance alone; including C, O, Mg, and Si shifts the picture.
  • About 87% of super-Jupiter hosts in the sample have at least proto-solar total disk metal content, so core accretion can plausibly build most of these planets; the remaining sub-solar cases remain a separate puzzle.
  • Planet-formation models should treat super-Jupiters as a viable core-accretion outcome under these observed Ztotal values rather than assuming a sharp switch to gravitational instability at 4–10 Jupiter masses.

Reading between the lines

Editorial extensions of the paper, not claims the author makes directly.

  • A direct test of the paper's premise would be to compare present-day surface abundances with the compositions of intact protoplanetary disks around young stars; any systematic offset in C/O or Mg/Si ratios would propagate directly into Z.
  • If the constancy assumption holds, the paper implies that [Fe/H] alone systematically understates the metal content of low-metallicity, α-enhanced stars, which could explain why earlier work saw super-Jupiter hosts as metal-poor.
  • The p-values near 0.02–0.05 suggest the effect is real but small; a larger homogeneous abundance survey of super-Jupiter hosts would show whether the ~0.22 excess in mean Ztotal persists.
  • The 12 sub-solar super-Jupiters are a natural place to look for signs of gravitational instability, such as wide orbits or different companion populations, because core accretion is hardest to invoke there.
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Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, and a circularity audit.

Referee Report

3 major / 5 minor

Summary. The paper compares the total metal content available in protoplanetary disks around stars hosting 'Jupiters' (1–4 Mjup) and 'super-Jupiters' (4–13 Mjup). Using C, O, Mg, Si, and Fe abundances from the Hypatia Catalog and the stoichiometric model of Santos et al. (2017a), the authors compute a metal mass fraction Z and a total metal content Ztotal under the assumption that disk mass scales linearly with stellar mass. They report raw t-test, KS, and AD p-values of 0.023–0.042 suggesting a slightly higher Z and Ztotal for super-Jupiters, but their own Monte Carlo propagation shows that these differences are not robust: p<0.05 occurs in fewer than 50% of realizations for Ztotal and in only about 6% for Z*total. The paper nevertheless concludes in the abstract and discussion that the results are 'strong evidence' that super-Jupiters form via core accretion.

Significance. If the directional result were robust, it would be a useful observational constraint: the metal budget in protoplanetary disks would not appear to be the reason super-Jupiters are rare, which would mildly favor core accretion over gravitational instability. The paper's strength is that it moves beyond [Fe/H] alone by including rock-forming elements and it explicitly reports the unfavorable Monte Carlo result. However, because the headline significance collapses under the paper's own error propagation, the central claim as stated is not supported. The more defensible directional statement (super-Jupiters do not have less disk metal than Jupiters) could still be of interest to planet formation modelers.

major comments (3)
  1. [Abstract; Section 4; Section 5] The headline claim is contradicted by the paper's own Monte Carlo test in Section 4. The raw t-test/KS/AD p-values (0.023–0.042) are reported as statistically significant, but the MC propagation over 10,000 realizations yields p<0.05 in fewer than 50% of cases for Ztotal and in only about 6% of cases for Z*total (over 94% with p>0.05). The text explicitly states that 'this test does not support the hypothesis that the two samples have statistically distinct distributions or mean values of Ztotal.' Nevertheless, the abstract and Section 5 describe the results as 'strong evidence' and 'consistently demonstrate' that super-Jupiters form in disks with at least as much metal content. Because the significance disappears once measurement uncertainties are propagated, the 'strong evidence' claim is not supported. The directional statement is more defensible (only 1 in 10,000 realizations gave a lower mean for super-Jupiters), but the paper must either provide a statistical argument for why the raw p-values are the relevant ones or substantially weaken the conclusion.
  2. [Section 3] The computation of Z and Ztotal relies on the assumption that present-day stellar atmospheric abundances reflect the primordial composition of the protoplanetary disk. The paper states that 'the abundance ratios of rock-forming elements remain relatively constant' over stellar evolution and supports this with Adibekyan et al. (2024, A&A, submitted), a self-cited manuscript that is not yet published and not available for verification. Since this assumption is load-bearing for the central claim, the authors should either provide the supporting analysis in the present paper or cite a published, independent source; at minimum, the results should be flagged as conditional on this assumption.
  3. [Section 3, Eq. (1)] The definition of Z*total is unclear and appears internally inconsistent. The text defines Z*total = log(Z × Mstar) × σdisk, where σdisk is a dispersion assumed to be 0.8 dex, but then states that 'σdisk was sampled from a log-normal distribution centered at 1 with a standard deviation of 0.8 dex.' Multiplying a log quantity by a dispersion does not generate scatter; it rescales the values. Please provide the exact error model used, justify the factor of 0.8, and ensure the text matches the analysis. This matters because Figure 3 and the corresponding MC results for Z*total are used to argue that the two samples have similar distributions.
minor comments (5)
  1. [Section 5] The paragraph beginning 'The observational evidence that Jupiter-mass planets tend to form around stars with high metallicity...' is duplicated verbatim and should be removed in one place.
  2. [Section 3] The 'proto-solar disk level' is used in the text and in Figure 2 but is never quantitatively defined; please state explicitly that it corresponds to Z = 1.25% and Ztotal = 1.25 under the adopted solar reference.
  3. [Section 2] The paper reports 428 massive planets orbiting 396 stars after the SWEET-Cat cross-match and 265 planets in the final sample, but it does not state how many targets remained after the Hypatia cross-match; please provide the intermediate sample size.
  4. [Section 4] The statement that excluding the 10 systems with planets in both the Jupiter and super-Jupiter groups 'does not affect the outcomes of the tests' would be more convincing if the resulting p-values were reported.
  5. [Section 2] The [X/H] < 0.6 cutoff is justified only as excluding 'potentially inaccurate abundances' and removes four targets; please add a sensitivity test showing that the conclusions are unchanged if these targets are retained or if a different threshold is used.

Circularity Check

1 steps flagged · score 4.0 of 10

No construction-level circularity in the empirical comparison; one load-bearing assumption is justified only by an unpublished self-cited manuscript.

  1. self citation load bearing [Section 3, "Metals in the protoplanetary disk"]
    "However, as we recently demonstrated in Adibekyan et al. (2024, A&A, submitted), while the individual abundances of elements can change significantly over the evolution of FGK stars, the abundance ratios of rock-forming elements remain relatively constant. This consistency supports the validity of using present-day stellar abundances to infer the composition of protoplanetary disks."

    The central quantity Z, and therefore Ztotal, is computed from present-day stellar abundances of C, O, Mg, Si, and Fe. The paper's claim that these ratios faithfully represent the primordial protoplanetary disk composition is not derived or independently tested here; it is supported solely by 'Adibekyan et al. (2024, A&A, submitted)', an unpublished manuscript with overlapping authorship. This is load-bearing because if rock-forming element ratios do change with stellar evolution, the derived Z values and the subsequent Jupiter versus super-Jupiter comparison would be unreliable. The citation is not machine-checked, code-reproduced, or externally falsified within the paper, so it does not qualify as independent evidence under the usual standards.

full rationale

The paper is primarily an empirical comparison of host-star metal content for Jupiter-mass versus super-Jupiter-mass planets, using public catalogs (NEA, SWEET-Cat, Hypatia) and a stated stoichiometric model. The main conclusion that super-Jupiters form in disks with at least as much metal content as Jupiters is not derived from a fitted parameter or defined into existence; it is a statistical comparison with real data. The Monte Carlo test in Section 4 actually shows that the p-values are below 0.05 in fewer than half of realizations, which is an internal consistency problem for the 'strong evidence' language, but it is not circularity. The only genuine circularity concern is the load-bearing self-citation: the assumption that present-day rock-forming element abundance ratios remain constant over stellar evolution is justified exclusively by an unpublished, same-author manuscript (Adibekyan et al. 2024, A&A, submitted). Because this assumption underpins the calculation of Z and Ztotal, it introduces a moderate circularity burden, though the central empirical comparison retains independent content from external catalogs and standard statistical tests. Score 4 reflects this partial self-citation dependence without overstating it as a construction-level equivalence.

Assumptions & free parameters 2 free parameters · 5 assumptions · 0 invented entities

The central claim rests on a chain of assumptions: stellar abundances trace disk composition, the stoichiometric model converts them to Z, disk mass scales with stellar mass, and the abundance ratios are unchanged over time. The most fragile is the abundance-ratio invariance, supported by a self-cited submitted paper. The sigma_disk parameter is adopted from literature to broaden uncertainties, which weakens the significance of the difference.

free parameters (2)
  • sigma_disk = 0.8 dex
    Dispersion in disk mass at fixed stellar mass, adopted from literature (Manara et al. 2023) and used to compute Z*_total; not fitted to this sample but added as a conservative broadening.
  • superlinear_scaling_power = 1.5
    Power-law index for the alternative disk mass-stellar mass relation tested in the robustness check; not a primary parameter but used to show results are unchanged.
assumptions (5)
  • domain assumption Stellar atmospheric C, O, Mg, Si, Fe abundances represent the composition of the protoplanetary disk.
    Central to converting stellar abundances into disk metal content; explicitly assumed in Section 3.
  • domain assumption The stoichiometric model of Santos et al. (2017a) correctly converts stellar abundances into Z.
    Used without re-derivation to calculate Z from the abundances of five elements.
  • domain assumption Disk mass scales linearly with stellar mass.
    Used to compute Ztotal = Z × Mstar; the paper acknowledges other scalings but adopts linear as primary.
  • domain assumption Abundance ratios of rock-forming elements remain constant over FGK stellar evolution.
    Invoked to justify present-day abundances as primordial; supported only by a submitted, self-cited paper (Adibekyan et al. 2024).
  • ad hoc to paper The [X/H] < 0.6 dex cutoff excludes only inaccurate abundance determinations.
    Applied to remove four targets with extreme abundances; the paper argues the Galaxy has not enriched beyond 0.6 dex, but this is a post-hoc selection.

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Cite this review

Pith. "Pith review of On the formation of super-Jupiters: Core Accretion or Gravitational Instability?." pith.science (2026). https://pith.science/paper/4L7MOSII

@misc{pith2026241206594,
  author       = {Pith},
  title        = {Pith review of: On the formation of super-Jupiters: Core Accretion or Gravitational Instability?},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/4L7MOSII}},
  note         = {Machine review of arXiv:2412.06594}
}
read the original abstract

The Core Accretion model is widely accepted as the primary mechanism for forming planets up to a few Jupiter masses. However, the formation of super-massive planets remains a subject of debate, as their formation via the Core Accretion model requires super-solar metallicities. Assuming stellar atmospheric abundances reflect the composition of protoplanetary disks, and that disk mass scales linearly with stellar mass, we calculated the total amount of metals in planet-building materials that could contribute to the formation of massive planets. In this work, we studied a sample of 172 Jupiter-mass planets and 93 planets with masses exceeding 4 Mjup. Our results consistently demonstrate that planets with masses above 4 Mjup form in disks with at least as much metal content as those hosting planets with masses between 1 and 4 Mjup, often with slightly higher metallicity, typically exceeding that of the proto-solar disk. We interpret this as strong evidence that the formation of very massive Jupiters is feasible through Core Accretion and encourage planet formation modelers to test our observational conclusions.

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

44 extracted references · 9 canonical work pages

  1. [1]

    Adibekyan V (2019) Heavy Metal Rules. I. Exoplanet Incidence and Metallicity . Geosciences 9(3):105. doi:10.3390/geosciences9030105, https://arxiv.org/abs/1902.04493 arXiv:1902.04493 [astro-ph.EP]

    arXiv 2019

  2. [2]

    The Kepler and HARPS samples

    Adibekyan VZ, Delgado Mena E, Sousa SG, et al (2012 a ) Exploring the -enhancement of metal-poor planet-hosting stars. The Kepler and HARPS samples . 547:A36. doi:10.1051/0004-6361/201220167, https://arxiv.org/abs/1209.6272 arXiv:1209.6272 [astro-ph.EP]

    arXiv 2012

  3. [3]

    Adibekyan VZ, Santos NC, Sousa SG, et al (2012 b ) Overabundance of -elements in exoplanet-hosting stars . 543:A89. doi:10.1051/0004-6361/201219564, https://arxiv.org/abs/1205.6670 arXiv:1205.6670 [astro-ph.EP]

    arXiv 2012

  4. [4]

    Galactic stellar populations and planets

    Adibekyan VZ, Sousa SG, Santos NC, et al (2012 c ) Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program. Galactic stellar populations and planets . 545:A32. doi:10.1051/0004-6361/201219401, https://arxiv.org/abs/1207.2388 arXiv:1207.2388 [astro-ph.EP]

    arXiv 2012

  5. [5]

    Adibekyan VZ, Figueira P, Santos NC, et al (2013) Orbital and physical properties of planets and their hosts: new insights on planet formation and evolution . 560:A51. doi:10.1051/0004-6361/201322551, https://arxiv.org/abs/1311.2417 arXiv:1311.2417 [astro-ph.EP]

    work page Pith review arXiv 2013

  6. [6]

    771(2):129

    Andrews SM, Rosenfeld KA, Kraus AL, et al (2013) The Mass Dependence between Protoplanetary Disks and their Stellar Hosts . 771(2):129. doi:10.1088/0004-637X/771/2/129, https://arxiv.org/abs/1305.5262 arXiv:1305.5262 [astro-ph.SR]

    arXiv 2013

  7. [7]

    Ansdell M, Williams JP, van der Marel N, et al (2016) ALMA Survey of Lupus Protoplanetary Disks. I. Dust and Gas Masses . 828(1):46. doi:10.3847/0004-637X/828/1/46, https://arxiv.org/abs/1604.05719 arXiv:1604.05719 [astro-ph.EP]

    arXiv 2016

  8. [8]

    653:A141

    Asplund M, Amarsi AM, Grevesse N (2021) The chemical make-up of the Sun: A 2020 vision . 653:A141. doi:10.1051/0004-6361/202140445, https://arxiv.org/abs/2105.01661 arXiv:2105.01661 [astro-ph.SR]

    arXiv 2021

Show all 44 references
  1. [9]

    A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood

    Bensby T, Feltzing S, Oey MS (2014) Exploring the Milky Way stellar disk. A detailed elemental abundance study of 714 F and G dwarf stars in the solar neighbourhood . 562:A71. doi:10.1051/0004-6361/201322631, https://arxiv.org/abs/1309.2631 arXiv:1309.2631 [astro-ph.GA]

    2014 arXiv

  2. [10]

    Science 276:1836--1839

    Boss AP (1997) Giant planet formation by gravitational instability. Science 276:1836--1839. doi:10.1126/science.276.5320.1836

    1997

  3. [11]

    Deal M, Alecian G, Lebreton Y, et al (2018) Impacts of radiative accelerations on solar-like oscillating main-sequence stars . 618:A10. doi:10.1051/0004-6361/201833361, https://arxiv.org/abs/1806.10533 arXiv:1806.10533 [astro-ph.SR]

    2018 arXiv

  4. [12]

    Delgado Mena E, Adibekyan V, Santos NC, et al (2021) Chemical abundances of 1111 FGK stars from the HARPS GTO planet search program. IV. Carbon and C/O ratios for Galactic stellar populations and planet hosts . 655:A99. doi:10.1051/0004-6361/202141588, https://arxiv.org/abs/21...

    2021 arXiv

  5. [13]

    944(2):135

    Fiorellino E, Tychoniec , Cruz-S \'a enz de Miera F, et al (2023) The Mass Accretion Rate and Stellar Properties in Class I Protostars . 944(2):135. doi:10.3847/1538-4357/aca320, https://arxiv.org/abs/2211.07653 arXiv:2211.07653 [astro-ph.SR]

    2023 arXiv

  6. [14]

    622(2):1102--1117

    Fischer DA, Valenti J (2005) The Planet-Metallicity Correlation . 622(2):1102--1117. doi:10.1086/428383

    2005 doi

  7. [15]

    Gaia Collaboration , Prusti T, de Bruijne JHJ, et al (2016) The Gaia mission . 595:A1. doi:10.1051/0004-6361/201629272, https://arxiv.org/abs/1609.04153 arXiv:1609.04153 [astro-ph.IM]

    2016 arXiv

  8. [16]

    399(1):L103--L107

    Gonzalez G (2009) Stars with planets and the thick disc . 399(1):L103--L107. doi:10.1111/j.1745-3933.2009.00734.x

    2009

  9. [17]

    A potential link with planet formation

    Guzm \'a n-D \' az J, Montesinos B, Mendigut \' a I, et al (2023) Relation between metallicities and spectral energy distributions of Herbig Ae/Be stars. A potential link with planet formation . 671:A140. doi:10.1051/0004-6361/202245427, https://arxiv.org/abs/2212.14022 arXiv:...

    2023 arXiv

  10. [18]

    148(3):54

    Hinkel NR, Timmes FX, Young PA, et al (2014) Stellar Abundances in the Solar Neighborhood: The Hypatia Catalog . 148(3):54. doi:10.1088/0004-6256/148/3/54, https://arxiv.org/abs/1405.6719 arXiv:1405.6719 [astro-ph.SR]

    2014 arXiv

  11. [19]

    Computing in Science & Engineering 9(3):90--95

    Hunter JD (2007) Matplotlib: A 2d graphics environment. Computing in Science & Engineering 9(3):90--95. doi:10.1109/MCSE.2007.55

    2007 doi

  12. [20]

    Ida S, Lin DNC (2004) Toward a Deterministic Model of Planetary Formation. I. A Desert in the Mass and Semimajor Axis Distributions of Extrasolar Planets . 604(1):388--413. doi:10.1086/381724, https://arxiv.org/abs/astro-ph/0312144 arXiv:astro-ph/0312144 [astro-ph]

    2004 arXiv

  13. [21]

    arXiv e-prints arXiv:2411.00277

    Liu Y, Roussel H, Linz H, et al (2024) Dust mass in protoplanetary disks with porous dust opacities . arXiv e-prints arXiv:2411.00277. https://arxiv.org/abs/2411.00277 arXiv:2411.00277 [astro-ph.EP]

    2024 arXiv

  14. [22]

    Maldonado J, Villaver E, Eiroa C, et al (2019) Connecting substellar and stellar formation: the role of the host star's metallicity . 624:A94. doi:10.1051/0004-6361/201833827, https://arxiv.org/abs/1903.01141 arXiv:1903.01141 [astro-ph.SR]

    2019 arXiv

  15. [23]

    In: Inutsuka S, Aikawa Y, Muto T, et al (eds) Protostars and Planets VII, p 539, doi:10.48550/arXiv.2203.09930, 2203.09930

    Manara CF, Ansdell M, Rosotti GP, et al (2023) Demographics of Young Stars and their Protoplanetary Disks: Lessons Learned on Disk Evolution and its Connection to Planet Formation . In: Inutsuka S, Aikawa Y, Muto T, et al (eds) Protostars and Planets VII, p 539, doi:10.48550/a...

    2023 doi arXiv

  16. [24]

    526(3):3933--3943

    Matsukoba R, Vorobyov EI, Hosokawa T, et al (2023) Formation of a wide-orbit giant planet in a gravitationally unstable subsolar-metallicity protoplanetary disc . 526(3):3933--3943. doi:10.1093/mnras/stad3003, https://arxiv.org/abs/2307.13722 arXiv:2307.13722 [astro-ph.EP]

    2023 arXiv

  17. [25]

    In: Proceedings of the 9th Python in Science Conference, Austin, TX, pp 51--56

    McKinney W, et al (2010) Data structures for statistical computing in python. In: Proceedings of the 9th Python in Science Conference, Austin, TX, pp 51--56

    2010

  18. [26]

    773(2):168

    Mohanty S, Greaves J, Mortlock D, et al (2013) Protoplanetary Disk Masses from Stars to Brown Dwarfs . 773(2):168. doi:10.1088/0004-637X/773/2/168, https://arxiv.org/abs/1305.6896 arXiv:1305.6896 [astro-ph.SR]

    2013 arXiv

  19. [27]

    Mordasini C, Alibert Y, Benz W, et al (2012) Extrasolar planet population synthesis . IV. Correlations with disk metallicity, mass, and lifetime . 541:A97. doi:10.1051/0004-6361/201117350, https://arxiv.org/abs/1201.1036 arXiv:1201.1036 [astro-ph.EP]

    2012 arXiv

  20. [28]

    156(5):221

    Narang M, Manoj P, Furlan E, et al (2018) Properties and Occurrence Rates for Kepler Exoplanet Candidates as a Function of Host Star Metallicity from the DR25 Catalog . 156(5):221. doi:10.3847/1538-3881/aae391, https://arxiv.org/abs/1809.08385 arXiv:1809.08385 [astro-ph.EP]

    2018 arXiv

  21. [29]

    831(2):125

    Pascucci I, Testi L, Herczeg GJ, et al (2016) A Steeper than Linear Disk Mass-Stellar Mass Scaling Relation . 831(2):125. doi:10.3847/0004-637X/831/2/125, https://arxiv.org/abs/1608.03621 arXiv:1608.03621 [astro-ph.EP]

    2016 arXiv

  22. [30]

    124(1):62--85

    Pollack JB, Hubickyj O, Bodenheimer P, et al (1996) Formation of the Giant Planets by Concurrent Accretion of Solids and Gas . 124(1):62--85. doi:10.1006/icar.1996.0190

    1996

  23. [31]

    525(2):2208--2228

    Ratcliffe B, Minchev I, Anders F, et al (2023) Unveiling the time evolution of chemical abundances across the Milky Way disc with APOGEE . 525(2):2208--2228. doi:10.1093/mnras/stad1573, https://arxiv.org/abs/2305.13378 arXiv:2305.13378 [astro-ph.GA]

    2023 arXiv

  24. [32]

    arXiv e-prints arXiv:2406.05447

    Rauer H, Aerts C, Cabrera J, et al (2024) The PLATO Mission . arXiv e-prints arXiv:2406.05447. doi:10.48550/arXiv.2406.05447, https://arxiv.org/abs/2406.05447 arXiv:2406.05447 [astro-ph.IM]

    2024 doi arXiv

  25. [33]

    373:1019--1031

    Santos NC, Israelian G, Mayor M (2001) The metal-rich nature of stars with planets . 373:1019--1031. doi:10.1051/0004-6361:20010648, https://arxiv.org/abs/astro-ph/0105216 arXiv:astro-ph/0105216 [astro-ph]

    2001 arXiv

  26. [34]

    Santos NC, Sousa SG, Mortier A, et al (2013) SWEET-Cat: A catalogue of parameters for Stars With ExoplanETs. I. New atmospheric parameters and masses for 48 stars with planets . 556:A150. doi:10.1051/0004-6361/201321286, https://arxiv.org/abs/1307.0354 arXiv:1307.0354 [astro-ph.SR]

    2013 arXiv

  27. [35]

    Santos NC, Adibekyan V, Dorn C, et al (2017 a ) Constraining planet structure and composition from stellar chemistry: trends in different stellar populations . 608:A94. doi:10.1051/0004-6361/201731359, https://arxiv.org/abs/1711.00777 arXiv:1711.00777 [astro-ph.EP]

    2017 arXiv

  28. [36]

    Santos NC, Adibekyan V, Figueira P, et al (2017 b ) Observational evidence for two distinct giant planet populations . 603:A30. doi:10.1051/0004-6361/201730761, https://arxiv.org/abs/1705.06090 arXiv:1705.06090 [astro-ph.EP]

    2017 arXiv

  29. [37]

    853(1):37

    Schlaufman KC (2018) Evidence of an Upper Bound on the Masses of Planets and Its Implications for Giant Planet Formation . 853(1):37. doi:10.3847/1538-4357/aa961c, https://arxiv.org/abs/1801.06185 arXiv:1801.06185 [astro-ph.EP]

    2018 arXiv

  30. [38]

    In: 9th Python in Science Conference

    Seabold S, Perktold J (2010) statsmodels: Econometric and statistical modeling with python. In: 9th Python in Science Conference

    2010

  31. [39]

    arXiv e-prints arXiv:2409.11965

    Sousa SG, Adibekyan V, Delgado-Mena E, et al (2024) SWEET-Cat: A view on the planetary mass-radius relation . arXiv e-prints arXiv:2409.11965. doi:10.48550/arXiv.2409.11965, https://arxiv.org/abs/2409.11965 arXiv:2409.11965 [astro-ph.EP]

    2024 doi

  32. [40]

    727(1):57

    Spiegel DS, Burrows A, Milsom JA (2011) The Deuterium-burning Mass Limit for Brown Dwarfs and Giant Planets . 727(1):57. doi:10.1088/0004-637X/727/1/57, https://arxiv.org/abs/1008.5150 arXiv:1008.5150 [astro-ph.EP]

    2011 arXiv

  33. [41]

    Nature Methods 17:261--272

    Virtanen P, Gommers R, Oliphant TE, et al (2020) SciPy 1.0: Fundamental Algorithms for Scientific Computing in Python . Nature Methods 17:261--272. doi:10.1038/s41592-019-0686-2

    2020 doi

  34. [42]

    Journal of Open Source Software 6(60):3021

    Waskom ML (2021) seaborn: statistical data visualization. Journal of Open Source Software 6(60):3021. doi:10.21105/joss.03021, ://doi.org/10.21105/joss.03021

    2021 doi

  35. [43]

    , " * write output.state after.block = add.period write newline

    ENTRY address archive author booktitle chapter doi edition editor eid eprint howpublished institution journal key keywords month note number organization pages publisher school series title type url volume year archivePrefix primaryClass adsurl adsnote version label extra.labe...

  36. [44]

    write newline

    " write newline "" before.all 'output.state := FUNCTION add.period duplicate empty 'skip "." * add.blank if FUNCTION if.digit duplicate "0" = swap duplicate "1" = swap duplicate "2" = swap duplicate "3" = swap duplicate "4" = swap duplicate "5" = swap duplicate "6" = swap dupl...

Pith tools

Reviewed August 11, 2026 · model on record in the stance chip above.