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REVIEW 3 major objections 5 minor 139 references

Very-wide-orbit planets from dynamical instabilities during the stellar birth cluster phase

T0 review · 3 major / 5 minor · reviewed 2026-08-07 · deepseek-v4-flash

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Pith's one-line read Wide-orbit planets are a natural byproduct of dynamical instabilities in stellar birth clusters.

desk verdict A large, honestly reported simulation campaign that turns a known flyby-trapping mechanism into quantitative demographics; the headline occurrence rate rests on a long-term stability assertion that isn't yet tested. read the letter →

arxiv 2505.24093 v1 pith:PQ5VK6QD submitted 2025-05-30 astro-ph.EP astro-ph.GAastro-ph.SR

André Izidoro , Sean N. Raymond , Nathan A. Kaib , Alessandro Morbidelli , Andrea Isella This is my paper
classification astro-ph.EPastro-ph.GAastro-ph.SR
keywords wide-orbitplanetsPlanetNinedynamicalinstabilitiesstellarbirthclustersplanet-planetscatteringflybystrappingefficiencysolarsystemformation
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

Planets on very wide, eccentric orbits are hard to explain with planet formation alone because most protoplanetary disks are far smaller than the orbits observed. This paper argues that such planets are a natural byproduct of dynamical instabilities happening while a planetary system is still embedded in its natal stellar cluster. In this picture, planet-planet scattering first flings a planet onto an eccentric orbit, and a stellar flyby or a change in the cluster potential raises its perihelion, detaching it from further scattering. The simulations give trapping efficiencies of 5-10 percent for Solar System-like instabilities, 1-5 percent for gas-giant exoplanet instabilities, and a resulting population of at least $10^{-3}$ wide-orbit planets per star. A sympathetic reader should care because this connects widely separated exoplanets and the hypothesized Planet Nine to a common early phase of every star's life.

What carries the argument

The load-bearing mechanism is two-step orbital trapping. First, planet-planet scattering during a dynamical instability drives a planet onto a highly eccentric orbit with an apoastron of several hundred au, too far to be circularized by the disk and vulnerable to ejection. Second, an external perturbation from a star passing within roughly 1000 au, a change in the cluster's gravitational potential near the cluster center, or an encounter with a dense gas filament kicks the planet so that its periastron rises; once the periastron is large enough, with $q>150$ au, $a<10^4$ au, and $e<0.9$, the planet is dynamically decoupled from the inner system and survives after cluster dispersal. The paper quantifies this with the trapping efficiency $\epsilon = N_{\rm wide}/(N_{\rm wide}+N_{\rm eject})$, which links the number of wide-orbit planets to the number of free-floating planets produced by the same instability.

What would settle it

Take the full set of simulated trapped orbits with perihelia between 150 and a few hundred au and eccentricities up to 0.9, then integrate them for 4.5 Gyr including Neptune's perturbations, galactic tides, and passing field stars; if the survival fraction is substantially below one, the quoted efficiencies and the $10^{-3}$ per star rate must be reduced by that factor. A survey measuring wide-orbit planet occurrence around metal-poor versus metal-rich gas-giant hosts would also test the predicted metallicity enhancement directly.

Watch

Extended reading notes

Core claim

The paper's central claim is that very wide-orbit planets with semimajor axes between roughly 100 and 10,000 au are not rare anomalies but a predictable outcome of planetary dynamical instabilities that occur before the natal cluster disperses. A planet scattered by other planets onto an eccentric orbit with a large apoastron can be trapped if a nearby stellar flyby or a rapid change in the cluster potential delivers a kick that raises its periastron, decoupling it from the inner planets. Using about 30,000 N-body simulations of five classes of systems, the authors find that Solar System-like configurations trap 5-10 percent of scattered planets, extrasolar gas-giant instabilities trap 1-5 percent, and ice-giant-only or circumbinary systems trap under 1 percent. Applied to the Solar System, the model gives a 5-10 percent chance that either the ice-giant growth phase or the final giant-planet instability produced a Planet Nine-like object, rising to roughly 40 percent if both happened during the cluster phase. Combining the efficiencies with the known frequency of giant-planet instabilities, the paper concludes that wide, eccentric planets occur at least $10^{-3}$ per star.

Load-bearing premise

The efficiencies assume that planets counted as trapped, with perihelia beyond 150 au and semimajor axes below 10,000 au, actually remain on those orbits for gigayears after the cluster disperses, even though the simulations only run 10-20 million years.

Editorial extensions

If this is right

  • If the mechanism is correct, the Solar System's two early instabilities together give a meaningful chance, up to about 40 percent, that a Planet Nine-like planet was trapped and still exists.
  • Wide-orbit, eccentric planets should be most common around stars that already host gas giants and are metal-rich, giving a concrete observational target for direct-imaging surveys.
  • The same instabilities that create free-floating planets should also create a comparable population of bound wide-orbit planets, with the ratio set by the trapping efficiency.
  • Current observational upper limits of a few percent at 100-5000 au are consistent with the predicted roughly $10^{-3}$ per star occurrence, so deeper surveys can test the prediction.
  • Trapping efficiency depends on cluster density and lifetime: compact or long-lived clusters trap more planets, while systems that eject planets too quickly, such as circumbinary gas giants, or too slowly, such as pure ice giants, trap almost none.

Reading between the lines

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

  • One testable extension is to search for wide-orbit planets in very young clusters a few million years old, before dispersal; if trapping is the main route, these clusters should already show a measurable population at 100-1000 au, possibly with randomized orbital inclinations.
  • If the metallicity correlation holds, wide-orbit planet searches around metal-rich, gas-giant-hosting stars could raise the detection rate by a factor of several relative to unbiased surveys, because the underlying instability rate is higher there.
  • The same trapping logic may apply to lower-mass ejected bodies: planetesimals scattered by giant planets could be parked at the inner edge of the Oort cloud by the cluster, which the paper notes as a byproduct consistent with Oort cloud formation.
  • A direct long-term stability check, using gigayear integrations of the trapped orbits with galactic tides and passing stars, would sharpen the quoted efficiencies; the paper does not perform those integrations, so the survival assumption remains the main uncertainty.
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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 proposes that very wide-orbit planets (semimajor axes of a few hundred to 10^4 au) can be produced when a planet scattered during a dynamical instability receives a gravitational kick from a passing star or from the cluster potential, raising its pericenter and decoupling it from the inner planetary system. The authors report N-body simulations of several classes of planetary systems embedded in model stellar clusters: the Solar System's ice-giant formation phase, the final giant-planet instability, extrasolar gas-giant and ice-giant instability systems, and circumbinary gas-giant systems. They define a trapping efficiency and measure values of about 5-10% for Solar System-like cases, 1-5% for extrasolar gas-giant systems, and lower values for ice-giant-only and circumbinary cases. From this they estimate that wide-orbit planets occur at least 10^-3 per star and discuss implications for Planet Nine and for the connection between wide-orbit and free-floating planets.

Significance. If the result holds, the paper offers a concrete and physically plausible formation channel for a population that is otherwise hard to explain, and it makes falsifiable predictions: wide-orbit planets should be preferentially found around stars that host gas giants, hence around metal-rich, somewhat massive stars. The study is quantitatively transparent: it reports at least 100-1000 realizations per configuration, uses binomial error bars, explicitly states exclusion rules for orbits that may not be stable, and flags exploratory runs (ice-giant-only and circumbinary cases) as observationally unconstrained. The trapping efficiencies are measured rather than fitted to the target occurrence rate. The main weaknesses are the absence of long-term integrations supporting the claim that the counted orbits survive for Gyr, and the timing assumptions that underpin the combined Solar System probability.

major comments (3)
  1. [Main text, trapping-efficiency definition and final paragraph] The central claim that the counted wide-orbit planets are durable rests on the sentence "most trapped wide-orbit planets survive for tens of billions of years," but no simulation in the paper runs beyond 10-20 Myr. The efficiency epsilon = Nwide/(Nwide+Nejec) counts orbits at simulation end with q > 150 au, a < 10^4 au, and e < 0.9. Figure 3, panels b and c, shows large numbers of counted planets with q between 150 and roughly 550 au, many with a approaching 10^4 au and e near 0.9. These occupy the same dynamical regime as the excluded q = 35-150 au, e ~ 0.9-1 orbits that the paper itself says "may not maintain long-term stability." Galactic tides, passing field stars, and secular forcing from inner giants can alter q on Gyr timescales. Unless the authors supply long-term integrations of the trapped population (or an empirically calibrated stability boundary), the quoted efficiencies and the "at least 10^-3 per star" claim should be treated as upper-envelope estimates rather than established lower bounds. This is a load-bearing issue because it directly affects every quantitative result in the abstract.
  2. [Main text, Solar System probability paragraph] The combined 40% probability assumes that both Solar System scattering events—the ice-giant formation phase and the final giant-planet instability—occurred while the Sun was still in its natal embedded cluster (3-10 Myr). The paper itself cites constraints that the final instability happened within the first 10-100 Myr (refs. 33, 34), and only about 1% of clusters remain bound at ~100 Myr. If the final instability occurred after cluster dispersal, only the single-event 5-10% efficiency applies and the abstract's "rising to 40% if both were" is not supported. The manuscript should either quantify what fraction of allowed final-instability timings falls within the cluster phase or state explicitly that the 40% figure is conditional on both events occurring before cluster dispersal.
  3. [Main text, occurrence-rate estimate] The "at least 10^-3 per star" claim is built from a chain of literature and simulation factors: giant-planet occurrence of 1-10%, an instability fraction of 75-90%, an assumed lower limit of one ejected planet per instability, and a trapping efficiency of 1-10%. The text itself gives a plausible range of 7.5 x 10^-5 to 9 x 10^-3; the central value is near the geometric middle of this range, not obviously a lower bound. Each factor could be smaller, and the trapping-efficiency denominator Nwide+Nejec excludes planets that remain bound but not wide, so the status of "at least" should be justified or replaced by a central estimate with a stated uncertainty.
minor comments (5)
  1. [Extended Data Figure 1 caption] The caption reads "he eccentricity distribution of radial velocity exoplanets" and should read "The eccentricity distribution."
  2. [Methods, Circumbinary Star Systems] "Burlisch-Stoer" should be "Bulirsch-Stoer" in the two places where it appears.
  3. [Main text and Methods] The verb "refereed" is used in place of "referred" twice ("hereafter refereed to as" and "usually refereed to as open-clusters"); please correct these.
  4. [Figure 4] Some data points in Figure 4 appear to exceed 10% trapping efficiency, while the text summarizes the efficiency as 1-10%; please clarify in the caption or text whether these points correspond to the exploratory Solar-System-like (J-S-U) runs or to particular cluster configurations, and ensure the legend distinguishes the no-cluster crosses consistently.
  5. [Data availability] The Data availability statement says source data are "available at this link" but no URL appears in the manuscript text; please include the actual repository link.

Circularity Check

0 steps flagged · score 0.0 of 10

No significant circularity: efficiencies and occurrence rates are measured outputs, not fitted inputs.

full rationale

Derivation chain: (i) N-body cluster+planetary simulations are initialized using independent observables (RV giant-planet eccentricity distribution, Solar System architecture/Kuiper Belt constraints, observed cluster parameters); (ii) trapping efficiency epsilon = Nwide/(Nwide+Nejec) is measured as a simulation output over ~30,000 runs, with q>150 au, a<10^4 au, e<0.9 counting as trapped; (iii) the 10^-3 occurrence estimate is a multiplication of literature giant-planet occurrence (1-10%), literature instability fraction (75-90%), a literature lower limit of at least one ejected planet per instability, and the simulated epsilon (1-10%); (iv) the Solar System 5-10% and 40% figures are binomial conversions using the simulated epsilon and literature ejection counts. None of these steps fits or defines the target result: the wide-orbit count is the simulation output, not an input, and no equation reduces the predicted rate to the definition of the rate. Self-citations (Izidoro et al. 2015; Kaib et al. 2018; Raymond et al. 2023; etc.) are methodological, benchmark, or consistency checks such as the Oort-cloud analogy, and they are not the load-bearing proof of the trapping mechanism. The main concern is not circularity but robustness: the simulations run only 10-20 Myr while the paper asserts long-term survival over tens of Gyr, and the Solar System probability assumes both instabilities occurred during the embedded-cluster phase. These are extrapolation and timing uncertainties, not logical self-reference in the derivation.

Assumptions & free parameters 4 free parameters · 7 assumptions · 0 invented entities

The central claims rest on: (1) hand-chosen outcome thresholds defining 'trapped wide-orbit planets' (q>150 au, a<10^4 au, e<0.9), which set all efficiencies; (2) scenario inputs selected from literature or deliberately varied (cluster lifetime 3/5 Myr nominal and 50 Myr exploratory, gas disk rescaling fgas=0.5/0.7, ejected-planet count N=5 versus 3); (3) domain assumptions about cluster-bound lifetimes, the timing of Solar System instabilities during the cluster phase, the adequacy of a fixed Plummer gas potential, the Gyr stability of counted orbits, and literature rates for giant planet occurrence and instability ubiquity. No new physical entities are introduced; Planet Nine is adopted from prior work, not postulated here.

free parameters (4)
  • Trapped-orbit thresholds (q > 150 au, a < 10^4 au, e < 0.9) = q_min = 150 au, a_max = 10^4 au, e_max = 0.9
    Hand-chosen definitions of a successful trapping; planets with q < 35 au, and planets with q between 35 and 150 au at e near 0.9-1, are excluded as possibly coupled to the inner system. These boundaries set every quoted efficiency and the occurrence estimate derived from them.
  • Cluster lifetime tc = 3 and 5 Myr nominal; 50 Myr exploratory
    Gas cluster dissipation time. The 50 Myr cases are deliberately ad hoc to demonstrate that longer cluster lifetimes raise ice-giant trapping efficiency about five-fold.
  • Gas disk surface density rescaling fgas = 0.5 and 0.7
    Multiplicative rescaling of the base 1D gas disk profile in the ice-giant formation simulations to test lower-mass disks.
  • Number of ejected planets in the Solar System binomial estimate = 5 for the headline 40%; 3 for the conservative 14%
    Input to the binomial calculation giving the probability of capturing a wide-orbit planet that could represent Planet Nine; values are literature-informed choices, and the headline 40% requires the larger ejected count.
assumptions (7)
  • domain assumption Stars form in embedded clusters and most stars remain bound for about 3-10 Myr
    Invoked to justify the cluster-phase perturbation environment (Main text, paragraph 2; Methods, Stellar Cluster), with observational support from Lada & Lada and related references.
  • domain assumption Both Solar System instability events (ice-giant formation and the final giant planet instability) happened while the Sun was still in its birth cluster
    The 5-10% and 40% probabilities are conditional on this timing; the final instability is independently constrained to 10-100 Myr, which may post-date cluster dispersal at 3-10 Myr. The paper does not quantify the probability that the timing overlaps the cluster phase.
  • domain assumption A fixed Plummer gas potential plus point-mass stars adequately captures cluster perturbations
    Methods: the gas is a fixed background potential that does not react to stars, and substructure and filaments are neglected; the authors acknowledge the approximation and lean on prior usage (Brasser et al. 2006).
  • domain assumption Trapped orbits (q > 150 au, a < 10^4 au, e < 0.9) are long-term stable after cluster dispersal
    The efficiency metric assumes Gyr survival based on literature (galactic tides, Zink et al. 2020), not on long integrations in this paper, since runs end at 10-20 Myr.
  • domain assumption Giant planet systems undergo dynamical instabilities in 75-95% of cases, ejecting at least one planet
    From cited literature (Juric & Tremaine 2008; Chatterjee et al. 2008; Raymond et al. 2010); underpins the 10^-3 occurrence estimate.
  • domain assumption Giant planet occurrence integrated over stellar types is about 1-10%
    From Fulton et al. 2021 and related surveys; used in the occurrence estimate chain.
  • domain assumption The modified MERCURY integrator, including the circumbinary scheme, is accurate enough for the claimed statistics
    Methods: the circumbinary algorithm is validated by Jacobi constant conservation at 10^-4 to 10^-3 and by comparing final eccentricity distributions with a Bulirsch-Stoer integrator; the single-star scheme is inherited from Kaib et al. 2018.

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Pith. "Pith review of Very-wide-orbit planets from dynamical instabilities during the stellar birth cluster phase." pith.science (2026). https://pith.science/paper/PQ5VK6QD

@misc{pith2026250524093,
  author       = {Pith},
  title        = {Pith review of: Very-wide-orbit planets from dynamical instabilities during the stellar birth cluster phase},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/PQ5VK6QD}},
  note         = {Machine review of arXiv:2505.24093}
}
abstract

Gas giant planets have been detected on eccentric orbits several hundreds of astronomical units in size around other stars. It has been proposed that even the Sun hosts a wide-orbit planet of 5-10 Earth masses, often called Planet Nine, which influences the dynamics of distant Trans-Neptunian objects. However, the formation mechanism of such planets remains uncertain. Here we use numerical simulations to show that very wide-orbit planets are a natural byproduct of dynamical instabilities that occur in planetary systems while their host stars are still embedded in natal stellar clusters. A planet is first brought to an eccentric orbit with an apoastron of several hundred au by repeated gravitational scattering by other planets, then perturbations from nearby stellar flybys stabilise the orbit by decoupling the planet from the interaction with the inner system. In our Solar System, the two main events likely conducive to planetary scattering were the growth of Uranus and Neptune, and the giant planets instability. We estimate a 5-10% likelihood of creating a very wide-orbit planet if either happened while the Sun was still in its birth cluster, rising to 40% if both were. In our simulated exoplanetary systems, the trapping efficiency is 1-5\%. Our results imply that planets on wide, eccentric orbits occur at least $10^{-3}$ per star.

Figures

Figures reproduced from arXiv: 2505.24093 by the authors.

Figure 1
Figure 1. Snapshots of the dynamical evolution of a stellar cluster with 200 stars. Panels show the top view projection of the cluster at different times. Color-coded circles represent individual stars and the size of the circle scales with M0.5 (for presentation purposes only), where M is the star mass. In this nominal simulation, a solar-mass star is at the center of the reference frame. We refer to this star as the host st… view at source ↗
Figure 2
Figure 2. Trapping of wide-orbit planets in a extrasolar gas-giant instability simulation and a Solar System early dynamical instability simulation. Both simulations of panels A and B start with fully formed planets. The cluster contains 200 stars and Rc = 40, 000 au. The host star is a solar-mass star in both simulations. A): Trapping of a wide-orbit exoplanet. The top panel shows the distance of two specific star members of… view at source ↗
Figure 3
Figure 3. Final orbital distribution of planets produced in early dynamical planetary instabilities taking place in different planetary systems embedded in stellar clusters with different configurations. Nstar represents the number of stars in the cluster. Rc is the cluster Plummer radius, tc is the timing of cluster dispersal. Panels a, b, c, and d show the orbital distribution of planets in simulations modeling the accretio… view at source ↗
Figures from the paper (2 more)
Figure 4
Figure 4. Figure 4: Exoplanet surveys have shown that ∼1-10% of all main sequence stars host giant exo￾planets, integrated over all stellar types84–86. To match the observed eccentricity distribution,28,29 roughly 75-90% of giant exoplanet systems must be the survivors of dynamical instab…
Figure 4
Figure 4. Figure 4: Wide-orbit planet trapping efficiency in different planetary systems embedded in star clusters with different configurations. The point shape gives the star cluster configuration as shown at the very top of the panel. Crosses are used to represent cases with no star cl…

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Works this paper leans on

139 extracted references · 80 canonical work pages

  1. [1]

    The distribution of comets around stars

    Tremaine, S. The distribution of comets around stars. In Phillips, J. A., Thorsett, S. E. & Kulkarni, S. R. (eds.) Planets Around Pulsars, vol. 36 of ASP Conf. Ser ., 335–344 (1993)

    1993

  2. [2]

    C., Bonsor, A., Jackson, A

    Wyatt, M. C., Bonsor, A., Jackson, A. P., Marino, S. & Shannon, A. How to design a planetary system for different scattering outcomes: giant impact sweet spot, maximizing exocomets, scattered discs. Mon. Not. R. Astron. Soc. 464, 3385–3407 (2017)

    2017

  3. [3]

    Bae, J. et al. Structured Distributions of Gas and Solids in Protoplanetary Disks. In Inutsuka, S., Aikawa, Y ., Muto, T., Tomida, K. & Tamura, M. (eds.)Protostars and Planets VII , vol. 534 of ASP Conf. Ser ., 423 (2023)

    2023

  4. [4]

    A., Levison, H

    Kretke, K. A., Levison, H. F., Buie, M. W. & Morbidelli, A. A Method to Constrain the Size of the Protosolar Nebula. Astron. J. 143, 91 (2012)

    2012

  5. [5]

    Bohn, A. J. et al. Two Directly Imaged, Wide-orbit Giant Planets around the Young, Solar Analog TYC 8998-760-1. Astrophys. J. 898, L16 (2020)

    2020

  6. [6]

    Zhang, Z. et al. The Second Discovery from the COCONUTS Program: A Cold Wide-orbit Exoplanet around a Young Field M Dwarf at 10.9 pc. Astrophys. J. 916, L11 (2021)

    2021

  7. [7]

    Janson, M. et al. A wide-orbit giant planet in the high-mass b Centauri binary system. Nature 600, 231–234 (2021)

    2021

  8. [8]

    Bohn, A. J. et al. Discovery of a directly imaged planet to the young solar analog YSES 2. Astron. Astrophys. 648, A73 (2021)

    2021

Show all 139 references
  1. [9]

    Gaidos, E. et al. Zodiacal exoplanets in time (ZEIT) XII: a directly imaged planetary-mass companion to a young Taurus M dwarf star.Mon. Not. R. Astron. Soc. 512, 583–601 (2022). 34

    2022

  2. [10]

    Currie, T. et al. Direct Imaging and Spectroscopy of Extrasolar Planets. In Inutsuka, S., Aikawa, Y ., Muto, T., Tomida, K. & Tamura, M. (eds.)Protostars and Planets VII, vol. 534 of ASP Conf. Ser ., 799 (2023)

    2023

  3. [11]

    M., Macintosh, B

    Marois, C., Zuckerman, B., Konopacky, Q. M., Macintosh, B. & Barman, T. Images of a fourth planet orbiting HR 8799. Nature 468, 1080–1083 (2010)

    2010

  4. [12]

    M., De Rosa, R

    Nguyen, M. M., De Rosa, R. J. & Kalas, P. First Detection of Orbital Motion for HD 106906 b: A Wide-separation Exoplanet on a Planet Nine-like Orbit. Astron. J. 161, 22 (2021)

    2021

  5. [13]

    Faherty, J. K. et al. A Wide Planetary Mass Companion Discovered through the Citizen Science Project Backyard Worlds: Planet 9. Astrophys. J. 923, 48 (2021)

    2021

  6. [14]

    Mróz, P. et al. No large population of unbound or wide-orbit Jupiter-mass planets. Nature 548, 183–186 (2017)

    2017

  7. [15]

    Miret-Roig, N. et al. A rich population of free-floating planets in the Upper Scorpius young stellar association. Nat. Astron. 6, 89–97 (2022)

    2022

  8. [16]

    & Brown, M

    Batygin, K. & Brown, M. E. Evidence for a Distant Giant Planet in the Solar System. Astron. J. 151, 22 (2016)

    2016

  9. [17]

    Brown, M. E. & Batygin, K. Observational Constraints on the Orbit and Location of Planet Nine in the Outer Solar System. Astrophys. J. 824, L23 (2016)

    2016

  10. [18]

    Trujillo, C. A. & Sheppard, S. S. A Sedna-like body with a perihelion of 80 astronomical units. Nature 507, 471–474 (2014)

    2014

  11. [19]

    Brown, M. E. & Batygin, K. The Orbit of Planet Nine. Astron. J. 162, 219 (2021)

    2021

  12. [20]

    & Brown, M

    Batygin, K. & Brown, M. E. Evidence for a Distant Giant Planet in the Solar System. Astron. J. 151, 22 (2016). 35

    2016

  13. [21]

    & Morbidelli, A

    Batygin, K. & Morbidelli, A. Dynamical Evolution Induced by Planet Nine. Astron. J. 154, 229 (2017)

    2017

  14. [22]

    C., Brown, M

    Batygin, K., Adams, F. C., Brown, M. E. & Becker, J. C. The planet nine hypothesis. Phys. Rep. 805, 1–53 (2019)

    2019

  15. [23]

    Shankman, C. et al. OSSOS. VI. Striking Biases in the Detection of Large Semimajor Axis Trans-Neptunian Objects. Astron. J. 154, 50 (2017)

    2017

  16. [24]

    N., Izidoro, A

    Raymond, S. N., Izidoro, A. & Morbidelli, A. Solar System Formation in the Context of Extrasolar Planets. In Meadows, V . S., Arney, G. N., Schmidt, B. E. & Des Marais, D. J. (eds.) Planet. Astrobiol., 287 (Univ. Arizona Press, 2020)

    2020

  17. [25]

    N., Hersant, F

    Izidoro, A., Morbidelli, A., Raymond, S. N., Hersant, F. & Pierens, A. Accretion of Uranus and Neptune from inward-migrating planetary embryos blocked by Jupiter and Saturn. As- tron. Astrophys. 582, A99 (2015)

    2015

  18. [26]

    & Guillot, T

    Helled, R., Nettelmann, N. & Guillot, T. Uranus and Neptune: Origin, Evolution and Internal Structure. Space Sci. Rev. 216, 38 (2020)

    2020

  19. [27]

    & Morbidelli, A

    Nesvorný, D. & Morbidelli, A. Statistical Study of the Early Solar System’s Instability with Four, Five, and Six Giant Planets. Astron. J. 144, 117 (2012)

    2012

  20. [28]

    Butler, R. P. et al. Catalog of Nearby Exoplanets. Astrophys. J. 646, 505–522 (2006)

    2006

  21. [29]

    & Santos, N

    Udry, S. & Santos, N. C. Statistical Properties of Exoplanets. Annu. Rev. Astron. Astrophys. 45, 397–439 (2007)

    2007

  22. [30]

    & Tremaine, S

    Juri ´c, M. & Tremaine, S. Dynamical Origin of Extrasolar Planet Eccentricity Distribution. Astrophys. J. 686, 603–620 (2008). 36

    2008

  23. [31]

    B., Matsumura, S

    Chatterjee, S., Ford, E. B., Matsumura, S. & Rasio, F. A. Dynamical Outcomes of Planet- Planet Scattering. Astrophys. J. 686, 580–602 (2008)

    2008

  24. [33]

    Nesvorný, D., V okrouhlický, D., Bottke, W. F. & Levison, H. F. Evidence for very early migration of the Solar System planets from the Patroclus-Menoetius binary Jupiter Trojan. Nat. Astron. 2, 878–882 (2018)

    2018

  25. [34]

    Liu, B., Raymond, S. N. & Jacobson, S. A. Early Solar System instability triggered by dispersal of the gaseous disk. Nature 604, 643–646 (2022)

    2022

  26. [35]

    Lada, C. J. & Lada, E. A. Embedded Clusters in Molecular Clouds. Annu. Rev. Astron. As- trophys. 41, 57–115 (2003)

    2003

  27. [36]

    Adams, F. C. The Birth Environment of the Solar System. Annu. Rev. Astron. Astrophys. 48, 47–85 (2010)

    2010

  28. [37]

    Early evolution of the birth cluster of the solar system

    Pfalzner, S. Early evolution of the birth cluster of the solar system. Astron. Astrophys. 549, A82 (2013)

    2013

  29. [38]

    E., Ercolano, B

    Dale, J. E., Ercolano, B. & Bonnell, I. A. Early evolution of embedded clusters. Mon. Not. R. Astron. Soc. 451, 987–1003 (2015)

    2015

  30. [39]

    Adamo, A. et al. Star Clusters Near and Far; Tracing Star Formation Across Cosmic Time. Space Sci. Rev. 216, 69 (2020)

    2020

  31. [40]

    Adams, F. C. & Laughlin, G. Constraints on the Birth Aggregate of the Solar System.Icarus 150, 151–162 (2001). 37

    2001

  32. [41]

    F., McMillan, S

    Portegies Zwart, S. F., McMillan, S. L. W. & Gieles, M. Young Massive Star Clusters. Annu. Rev. Astron. Astrophys. 48, 431–493 (2010)

    2010

  33. [42]

    Malmberg, D., Davies, M. B. & Heggie, D. C. The effects of fly-bys on planetary systems. Mon. Not. R. Astron. Soc. 411, 859–877 (2011)

    2011

  34. [43]

    Parker, R. J. & Quanz, S. P. The effects of dynamical interactions on planets in young substructured star clusters. Mon. Not. R. Astron. Soc. 419, 2448–2458 (2012)

    2012

  35. [44]

    & Adams, F

    Laughlin, G. & Adams, F. C. The Modification of Planetary Orbits in Dense Open Clusters. Astrophys. J. 508, L171–L174 (1998)

    1998

  36. [45]

    Perets, H. B. & Kouwenhoven, M. B. N. On the Origin of Planets at Very Wide Orbits from the Recapture of Free Floating Planets. Astrophys. J. 750, 83 (2012)

    2012

  37. [46]

    & Adams, F

    Li, G. & Adams, F. C. Interaction Cross Sections and Survival Rates for Proposed Solar System Member Planet Nine. Astrophys. J. 823, L3 (2016)

    2016

  38. [47]

    J., Raymond, S

    Mustill, A. J., Raymond, S. N. & Davies, M. B. Is there an exoplanet in the Solar system? Mon. Not. R. Astron. Soc. 460, L109–L113 (2016)

    2016

  39. [48]

    J., Lichtenberg, T

    Parker, R. J., Lichtenberg, T. & Quanz, S. P. Was Planet 9 captured in the Sun’s natal star-forming region? Mon. Not. R. Astron. Soc. 472, L75–L79 (2017)

    2017

  40. [49]

    van Elteren, A., Portegies Zwart, S., Pelupessy, I., Cai, M. X. & McMillan, S. L. W. Surviv- ability of planetary systems in young and dense star clusters. Astron. Astrophys. 624, A120 (2019)

    2019

  41. [50]

    C., Parker, R

    Daffern-Powell, E. C., Parker, R. J. & Quanz, S. P. The Great Planetary Heist: theft and capture in star-forming regions. Mon. Not. R. Astron. Soc. 514, 920–934 (2022). 38

    2022

  42. [51]

    Boss, A. P. Giant planet formation by gravitational instability. Science 276, 1836–1839 (1997)

    1997

  43. [52]

    Kenyon, S. J. & Bromley, B. C. Formation of Super-Earth Mass Planets at 125-250 AU from a Solar-type Star. Astrophys. J. 806, 42 (2015)

    2015

  44. [53]

    Eriksson, L. E. J., Mustill, A. J. & Johansen, A. Circularizing Planet Nine through dy- namical friction with an extended, cold planetesimal belt. Mon. Not. R. Astron. Soc. 475, 4609–4616 (2018)

    2018

  45. [54]

    Bromley, B. C. & Kenyon, S. J. Making Planet Nine: A Scattered Giant in the Outer Solar System. Astrophys. J. 826, 64 (2016)

    2016

  46. [55]

    Esposito, T. M. et al. Debris Disk Results from the Gemini Planet Imager Exoplanet Sur- vey’s Polarimetric Imaging Campaign. Astron. J. 160, 24 (2020)

    2020

  47. [56]

    Beuzit, J. L. et al. SPHERE: the exoplanet imager for the Very Large Telescope.Astron. As- trophys. 631, A155 (2019)

    2019

  48. [57]

    Welsh, W. F. & Orosz, J. A. Two Suns in the Sky: The Kepler Circumbinary Planets. In Deeg, H. J. & Belmonte, J. A. (eds.) Handbook of Exoplanets, 34 (Springer Cham, 2018)

    2018

  49. [58]

    & Adams, F

    Proszkow, E.-M. & Adams, F. C. Dynamical Evolution of Young Embedded Clusters: A Parameter Space Survey. Astrophys. J. Suppl. 185, 486–510 (2009)

    2009

  50. [59]

    Allen, L. et al. The Structure and Evolution of Young Stellar Clusters. In Reipurth, B., Jewitt, D. & Keil, K. (eds.) Protostars and Planets V, 361 (2007)

    2007

  51. [60]

    M., Chandar, R

    Fall, S. M., Chandar, R. & Whitmore, B. C. New Tests for Disruption Mechanisms of Star Clusters: Methods and Application to the Antennae Galaxies. Astrophys. J. 704, 453–468 (2009). 39

    2009

  52. [61]

    Wijnen, T. P. G., Pols, O. R., Pelupessy, F. I. & Portegies Zwart, S. Disc truncation in embedded star clusters: Dynamical encounters versus face-on accretion. Astron. Astrophys. 604, A91 (2017)

    2017

  53. [62]

    & Price, D

    Cuello, N., Ménard, F. & Price, D. J. Close encounters: How stellar flybys shape planet- forming discs. European Physical Journal Plus 138, 11 (2023)

    2023

  54. [63]

    Winter, A. J. et al. Protoplanetary disc truncation mechanisms in stellar clusters: comparing external photoevaporation and tidal encounters. Mon. Not. R. Astron. Soc. 478, 2700–2722 (2018)

    2018

  55. [64]

    Fressin, F. et al. The False Positive Rate of Kepler and the Occurrence of Planets. Astro- phys. J. 766, 81 (2013)

    2013

  56. [65]

    Haisch Jr., K. et al. Disk Frequencies and Lifetimes in Young Clusters. Astrophys. J. 553, L153 (2001)

    2001

  57. [66]

    Brasser, R., Duncan, M. J. & Levison, H. F. Embedded star clusters and the formation of the Oort Cloud. Icarus 184, 59–82 (2006)

    2006

  58. [67]

    Rasio, F. A. & Ford, E. B. Dynamical instabilities and the formation of extrasolar planetary systems. Science 274, 954–956 (1996)

    1996

  59. [68]

    & Nesvorný, D

    Beaugé, C. & Nesvorný, D. Multiple-planet Scattering and the Origin of Hot Jupiters. Astrophys. J. 751, 119 (2012)

    2012

  60. [69]

    F., Morbidelli, A., Tsiganis, K., Nesvorný, D

    Levison, H. F., Morbidelli, A., Tsiganis, K., Nesvorný, D. & Gomes, R. Late Orbital In- stabilities in the Outer Planets Induced By Interaction With a Self-Gravitating Planetesimal Disk. Astron. J. 142, 152 (2011)

    2011

  61. [70]

    Deienno, R. et al. Excitation of a Primordial Cold Asteroid Belt as an Outcome of Planetary Instability. Astrophys. J. 864, 50 (2018). 40

    2018

  62. [71]

    & Mukai, T

    Higuchi, A., Kokubo, E., Kinoshita, H. & Mukai, T. Orbital Evolution of Planetesimals due to the Galactic Tide: Formation of the Comet Cloud. Astron. J. 134, 1693–1706 (2007)

    2007

  63. [72]

    Kaib, N. A. & Quinn, T. The formation of the Oort cloud in open cluster environments. Icarus 197, 221–238 (2008)

    2008

  64. [73]

    & Fabrycky, D

    Bailey, N. & Fabrycky, D. Stellar Flybys Interrupting Planet-Planet Scattering Generates Oort Planets. Astron. J. 158, 94 (2019)

    2019

  65. [74]

    N., Izidoro, A

    Raymond, S. N., Izidoro, A. & Kaib, N. A. Oort cloud (exo)planets. Mon. Not. R. As- tron. Soc. 524, L72–L77 (2023)

    2023

  66. [75]

    S., Kaib, N

    Clement, M. S., Kaib, N. A., Raymond, S. N. & Walsh, K. J. Mars’ growth stunted by an early giant planet instability. Icarus 311, 340–356 (2018)

    2018

  67. [76]

    de Sousa, R. R. et al. Dynamical evidence for an early giant planet instability. Icarus 339, 113605 (2020)

    2020

  68. [77]

    N., Armitage, P

    Raymond, S. N., Armitage, P. J. & Gorelick, N. Planet-Planet Scattering in Planetesimal Disks. II. Predictions for Outer Extrasolar Planetary Systems. Astrophys. J. 711, 772–795 (2010)

    2010

  69. [78]

    Izidoro, A. et al. Breaking the chains: hot super-Earth systems from migration and disrup- tion of compact resonant chains. Mon. Not. R. Astron. Soc. 470, 1750–1770 (2017)

    2017

  70. [79]

    Carter, E. J. & Stamatellos, D. On the survivability of a population of gas giant planets on wide orbits. Mon. Not. R. Astron. Soc. 525, 1912–1921 (2023)

    2023

  71. [80]

    & Nogueira, E

    Gomes, R., Nesvorný, D., Morbidelli, A., Deienno, R. & Nogueira, E. Checking the com- patibility of the cold Kuiper belt with a planetary instability migration model. Icarus 306, 319–327 (2018). 41

    2018

  72. [81]

    Mróz, P. et al. A Terrestrial-mass Rogue Planet Candidate Detected in the Shortest-timescale Microlensing Event. Astrophys. J. 903, L11 (2020)

    2020

  73. [82]

    & Gaudi, B

    Clanton, C. & Gaudi, B. S. Constraining the Frequency of Free-floating Planets from a Syn- thesis of Microlensing, Radial Velocity, and Direct Imaging Survey Results. Astrophys. J. 834, 46 (2017)

    2017

  74. [83]

    & Raymond, S

    Veras, D. & Raymond, S. N. Planet-planet scattering alone cannot explain the free-floating planet population. Mon. Not. R. Astron. Soc. 421, L117–L121 (2012)

    2012

  75. [84]

    Fulton, B. J. et al. California Legacy Survey. II. Occurrence of Giant Planets beyond the Ice Line. Astrophys. J. Suppl. 255, 14 (2021)

    2021

  76. [85]

    Bowler, B. P. Imaging Extrasolar Giant Planets. Publ. Astron. Soc. Pac.128, 102001 (2016)

    2016

  77. [86]

    Suzuki, D. et al. The Exoplanet Mass-ratio Function from the MOA-II Survey: Discovery of a Break and Likely Peak at a Neptune Mass. Astrophys. J. 833, 145 (2016)

    2016

  78. [87]

    Raymond, S. N. et al. Debris disks as signposts of terrestrial planet formation. Astron. As- trophys. 530, A62 (2011)

    2011

  79. [88]

    & Carson, J

    Durkan, S., Janson, M. & Carson, J. C. High Contrast Imaging with Spitzer: Constraining the Frequency of Giant Planets out to 1000 au Separations. Astrophys. J. 824, 58 (2016)

    2016

  80. [89]

    Baron, F. et al. WEIRD: Wide-orbit Exoplanet Search with InfraRed Direct Imaging. As- tron. J. 156, 137 (2018)

    2018

  81. [90]

    Fischer, D. A. & Valenti, J. The Planet-Metallicity Correlation. Astrophys. J. 622, 1102– 1117 (2005)

    2005

  82. [91]

    Dawson, R. I. & Murray-Clay, R. A. Giant Planets Orbiting Metal-rich Stars Show Signa- tures of Planet-Planet Interactions. Astrophys. J. 767, L24 (2013). 42

    2013

  83. [92]

    A., Aller, K

    Johnson, J. A., Aller, K. M., Howard, A. W. & Crepp, J. R. Giant Planet Occurrence in the Stellar Mass-Metallicity Plane. Publ. Astron. Soc. Pac. 122, 905 (2010)

    2010

  84. [93]

    K., Batygin, K

    Zink, J. K., Batygin, K. & Adams, F. C. The Great Inequality and the Dynamical Disinte- gration of the Outer Solar System. Astron. J. 160, 232 (2020)

    2020

  85. [94]

    Post-main-sequence planetary system evolution

    Veras, D. Post-main-sequence planetary system evolution. Royal Society Open Science 3, 150571 (2016)

    2016

  86. [95]

    N., Kaib, N

    Raymond, S. N., Kaib, N. A., Selsis, F. & Bouy, H. Future trajectories of the Solar System: dynamical simulations of stellar encounters within 100 au. Mon. Not. R. Astron. Soc. 527, 6126–6138 (2024)

    2024

  87. [96]

    Chambers, J. E. A hybrid symplectic integrator that permits close encounters between mas- sive bodies. Mon. Not. R. Astron. Soc. 304, 793–799 (1999)

    1999

  88. [97]

    E., Quintana, E

    Chambers, J. E., Quintana, E. V ., Duncan, M. J. & Lissauer, J. J. Symplectic Integrator Algorithms for Modeling Planetary Accretion in Binary Star Systems.Astron. J. 123, 2884– 2894 (2002)

    2002

  89. [98]

    A., White, E

    Kaib, N. A., White, E. B. & Izidoro, A. Simulations of the Fomalhaut system within its local galactic environment. Mon. Not. R. Astron. Soc. 473, 470–491 (2018)

    2018

  90. [99]

    J., Levison, H

    Duncan, M. J., Levison, H. F. & Lee, M. H. A Multiple Time Step Symplectic Algorithm for Integrating Close Encounters. Astron. J. 116, 2067–2077 (1998)

    1998

  91. [100]

    Plummer, H. C. On the problem of distribution in globular star clusters. Mon. Not. R. As- tron. Soc. 71, 460–470 (1911)

    1911

  92. [101]

    Ellithorpe, E. A. & Kaib, N. A. Dynamical fates of S-type planetary systems in embedded cluster environments. Mon. Not. R. Astron. Soc. 515, 2914–2927 (2022). 43

    2022

  93. [102]

    J., Henon, M

    Aarseth, S. J., Henon, M. & Wielen, R. A Comparison of Numerical Methods for the Study of Star Cluster Dynamics. Astron. Astrophys. 37, 183–187 (1974)

    1974

  94. [103]

    J., Levison, H

    Brasser, R., Duncan, M. J., Levison, H. F., Schwamb, M. E. & Brown, M. E. Reassessing the formation of the inner Oort cloud in an embedded star cluster. Icarus 217, 1–19 (2012)

    2012

  95. [104]

    Carpenter, J. M. 2MASS Observations of the Perseus, Orion A, Orion B, and Monoceros R2 Molecular Clouds. Astron. J. 120, 3139–3161 (2000)

    2000

  96. [105]

    C., Proszkow, E

    Adams, F. C., Proszkow, E. M., Fatuzzo, M. & Myers, P. C. Early Evolution of Stellar Groups and Clusters: Environmental Effects on Forming Planetary Systems. Astrophys. J. 641, 504–525 (2006)

    2006

  97. [106]

    & Kroupa, P

    Marks, M. & Kroupa, P. Inverse dynamical population synthesis. Constraining the initial conditions of young stellar clusters by studying their binary populations. Astron. Astrophys. 543, A8 (2012)

    2012

  98. [107]

    The Initial Mass Function of Stars: Evidence for Uniformity in Variable Systems

    Kroupa, P. The Initial Mass Function of Stars: Evidence for Uniformity in Variable Systems. Science 295, 82–91 (2002)

    2002

  99. [108]

    & Carlstrom, J

    Bally, J., Testi, L., Sargent, A. & Carlstrom, J. Disk Mass Limits and Lifetimes of Externally Irradiated Young Stellar Objects Embedded in the Orion Nebula. Astron. J. 116, 854–859 (1998)

    1998

  100. [109]

    Morales, E. F. E., Wyrowski, F., Schuller, F. & Menten, K. M. Stellar clusters in the inner Galaxy and their correlation with cold dust emission. Astron. Astrophys. 560, A76 (2013)

    2013

  101. [110]

    Embedded clusters

    Ascenso, J. Embedded clusters. In Stahler, S. (ed.) The Birth of Star Clusters , vol. 424 of Astrophys. Space Sci. Libr ., 1 (Springer, 2018). Provided by the SAO/NASA Astrophysics Data System. 44

    2018

  102. [111]

    & Kiyaeva, O

    Tokovinin, A. & Kiyaeva, O. Eccentricity distribution of wide binaries. Mon. Not. R. As- tron. Soc. 456, 2070–2079 (2016)

    2016

  103. [112]

    Young Solar System’s Fifth Giant Planet? Astrophys

    Nesvorny, D. Young Solar System’s Fifth Giant Planet? Astrophys. J. 742, L22 (2011)

    2011

  104. [113]

    F., Tsiganis, K

    Morbidelli, a., Levison, H. F., Tsiganis, K. & Gomes, R. Chaotic capture of Jupiter’s Trojan asteroids in the early Solar System. Nature 435, 462–465 (2005)

    2005

  105. [114]

    & Ida, S

    Kokubo, E. & Ida, S. Formation of Protoplanets from Planetesimals in the Solar Nebula. Icarus 143, 15 (2000)

    2000

  106. [115]

    & Morbidelli, A

    Lega, E., Crida, A., Bitsch, B. & Morbidelli, A. Migration of Earth-sized planets in 3D radiative discs. Mon. Not. R. Astron. Soc. 440, 683–695 (2014)

    2014

  107. [116]

    & Izidoro, A

    Bitsch, B. & Izidoro, A. Giants are bullies: How their growth influences systems of inner sub-Neptunes and super-Earths. Astron. Astrophys. 674, A178 (2023)

    2023

  108. [117]

    Wang, J. J. et al. Dynamical Constraints on the HR 8799 Planets with GPI. Astron. J. 156, 192 (2018)

    2018

  109. [118]

    & Crida, A

    Morbidelli, A. & Crida, A. The dynamics of Jupiter and Saturn in the gaseous protoplanetary disk. Icarus 191, 158–171 (2007)

    2007

  110. [119]

    N., Morbidelli, A., Hersant, F

    Izidoro, A., Raymond, S. N., Morbidelli, A., Hersant, F. & Pierens, A. Gas Giant Planets As Dynamical Barriers To Inward-Migrating Super-Earths. Astrophys. J. 800, L22 (2015)

    2015

  111. [120]

    Structure of the Solar Nebula, Growth and Decay of Magnetic Fields and Effects of Magnetic and Turbulent Viscosities on the Nebula

    Hayashi, C. Structure of the Solar Nebula, Growth and Decay of Magnetic Fields and Effects of Magnetic and Turbulent Viscosities on the Nebula. Prog. Theor . Phys. Suppl.70, 35–53 (1981)

    1981

  112. [121]

    Shakura, N. I. & Sunyaev, R. A. Black holes in binary systems. Observational appearance. Astron. Astrophys. 24 (1973). 45

    1973

  113. [122]

    Cresswell & Nelson, R. P. Three-dimensional simulations of multiple protoplanets embed- ded in a protostellar disc. Astron. Astrophys. 482, 677 (2008)

    2008

  114. [123]

    Coleman, G. A. L. & Nelson, R. P. On the formation of planetary systems via oligarchic growth in thermally evolving viscous discs. Mon. Not. R. Astron. Soc. 445, 479–499 (2014)

    2014

  115. [124]

    & Kley, W

    Paardekooper, S.-J., Baruteau, C., Crida, A. & Kley, W. A torque formula for non- isothermal type I planetary migration - I. Unsaturated horseshoe drag. Mon. Not. R. As- tron. Soc. 401, 1950–1964 (2010)

    2010

  116. [125]

    & Kley, W

    Paardekooper, S.-J., Baruteau, C. & Kley, W. A torque formula for non-isothermal Type I planetary migration - II. Effects of diffusion. Mon. Not. R. Astron. Soc. 410, 293–303 (2011)

    2011

  117. [126]

    & Brasser, R

    Ida, S., Muto, T., Matsumura, S. & Brasser, R. A new and simple prescription for planet orbital migration and eccentricity damping by planet-disc interactions based on dynamical friction. Mon. Not. R. Astron. Soc. 494, 5666–5674 (2020)

    2020

  118. [127]

    Papaloizou, J. C. B. & Larwood, J. D. On the orbital evolution and growth of protoplanets embedded in a gaseous disc. Mon. Not. R. Astron. Soc. 315, 823–833 (2000)

    2000

  119. [128]

    Brasser, R., Duncan, M. J. & Levison, H. F. Embedded star clusters and the formation of the Oort cloud. II. The effect of the primordial solar nebula. Icarus 191, 413–433 (2007)

    2007

  120. [129]

    Johansen, A. et al. Rapid planetesimal formation in turbulent circumstellar disks. Nature 448, 1022–1025 (2007)

    2007

  121. [130]

    B., Armitage, P

    Simon, J. B., Armitage, P. J., Li, R. & Youdin, A. N. The Mass and Size Distribution of Planetesimals Formed by the Streaming Instability. I. The Role of Self-gravity.Astrophys. J. 822, 55 (2016). 46

    2016

  122. [131]

    The Origin of Pluto’s Orbit: Implications for the Solar System Beyond Nep- tune

    Malhotra, R. The Origin of Pluto’s Orbit: Implications for the Solar System Beyond Nep- tune. Astron. J. 110, 420 (1995)

    1995

  123. [132]

    Fernandez, J. A. & Ip, W. H. Some dynamical aspects of the accretion of Uranus and Neptune: The exchange of orbital angular momentum with planetesimals. Icarus 58, 109– 120 (1984)

    1984

  124. [133]

    F., Tsiganis, K

    Gomes, R., Levison, H. F., Tsiganis, K. & Morbidelli, A. Origin of the cataclysmic Late Heavy Bombardment period of the terrestrial planets. Nature 435, 466–9 (2005)

    2005

  125. [134]

    Batygin, K., Brown, M. E. & Betts, H. Instability-Driven Dynamical Evolution Model of a Primordially Five-Planet Outer Solar System. Astrophys. J. 744, L3 (2012)

    2012

  126. [135]

    Dynamical Evolution of the Early Solar System.Annu

    Nesvorný, D. Dynamical Evolution of the Early Solar System.Annu. Rev. Astron. Astrophys. 56, 137–174 (2018)

    2018

  127. [136]

    & Gustafsson, B

    Nordlander, T., Rickman, H. & Gustafsson, B. The destruction of an Oort Cloud in a rich stellar cluster. Astron. Astrophys. 603, A112 (2017)

    2017

  128. [137]

    & Morbidelli, A

    Brasser, R. & Morbidelli, A. Oort cloud and Scattered Disc formation during a late dynam- ical instability in the Solar System. Icarus 225, 40–49 (2013)

    2013

  129. [138]

    Nesvorný, D. et al. Origin and Evolution of Short-period Comets. Astrophys. J. 845, 27 (2017)

    2017

  130. [139]

    & Rickman, H

    Dones, L., Brasser, R., Kaib, N. & Rickman, H. Origin and Evolution of the Cometary Reservoirs. Space Sci. Rev. 197, 191–269 (2015)

    2015

  131. [140]

    scattered

    Weidenschilling, S. J. Aerodynamics of solid bodies in the solar nebula. Mon. Not. R. As- tron. Soc. 180, 57–70 (1977). 47 This Supplementary Information presents additional simulation results that support and ex- tend the findings discussed in the main text. It includes simul...

    1977

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