Pith. sign in

REVIEW 3 major objections 4 minor 157 references

Terrestrial Planet Formation from Two Source Reservoirs

T0 review · 3 major / 4 minor · reviewed 2026-08-06 · deepseek-v4-flash

Challenge this review Re-run · record.json Download PDF Read on arXiv ↗

Pith's one-line read Two separate planetesimal reservoirs — an inner ring near 0.5 au and an outer source at 1.5–2 au — can produce the terrestrial planets, with outward Type-I migration carrying Venus and Earth outward while Mars is the lone survivor of the…

desk verdict A serious and systematic simulation study with a genuinely new two-source architecture, but the Mars isotope claim is internally contradicted by the paper's own admitted composition numbers. read the letter →

arxiv 2507.14814 v1 pith:PR3DDYUW submitted 2025-07-20 astro-ph.EP

David Nesvorny , Alessandro Morbidelli , William F. Bottke , Rogerio Deienno , Max Goldberg This is my paper · ORCID
classification astro-ph.EP
keywords terrestrialplanetformationtwo-sourcereservoirmodelType-ImigrationmagneticallydrivenwindssilicatesublimationlineplanetesimalringsinnersolarsystemMars
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 claims that the terrestrial planets assembled from two distinct planetesimal reservoirs rather than a single radially extended disk. In the reference model (model203), an inner ring at about 0.6 au — where planetesimals would form near the silicate sublimation line — supplies Mercury, Venus, and Earth, while a second, broader source at 1.5–2 au supplies Mars and many Mars-sized bodies that mostly fall onto Earth. Outward Type-I migration driven by a magnetically-wind-like gas disk with a surface-density bump near 1 au carries Venus and Earth to their present orbits and leaves Mercury behind near the ring. The model matches all four terrestrial-planet criteria in 6.1% of 1,000 simulations, produces Earth with about 70% inner-ring (reduced) and 30% outer-source (oxidized) material, and gives Mars a distinct outer-source composition, explaining the Earth-Mars isotopic difference and suggesting Theia shared Earth's accretion history.

What carries the argument

The load-bearing mechanism is torque-driven migration in a gas disk with a surface-density bump: the paper writes the gas surface density as $\Sigma_g = \Sigma_0 (r/r_0)^{\beta(r)} e^{-t/\tau}$ with $\beta(r)=\beta_1 \ln(r/r_0)+\beta_2$, choosing $\beta_1=-1$, $\beta_2=0$, $\Sigma_0=3000$ g cm$^{-2}$, $r_0=0.9$ au. This makes the local slope $\partial \ln \Sigma/\partial \ln r$ positive inside about 1.2 au, so protoplanets of roughly 0.1–1 Earth mass experience an outward torque and drift toward the zero-torque radius near 1 au. The inner planetesimal ring at 0.5–0.6 au is the nursery: the most massive embryos grow, migrate out, and concentrate at 0.7–1 au, while lower-mass Mercury stays behind. A second reservoir at 1.5–2 au feeds Mars and, through inward migration, supplies about 30% of Earth's mass later. A giant-planet instability at about 11 Myr breaks the resonant chains formed in the disk and triggers the late giant-impact stage.

What would settle it

A concrete test is to measure or compute the radial gas-density profile of a protoplanetary disk inside 1.2 au and check whether its local slope $\partial \ln \Sigma/\partial \ln r$ is positive there. If observations or detailed disk models that include magnetic winds show a monotonically decreasing density with no inner bump, the outward-migration regime disappears; embryos formed near 0.5 au would migrate inward by Lindblad torques and would not end up at the Venus-Earth separation seen in the reference model.

Watch

Extended reading notes

Core claim

The central discovery is that a two-source initial condition, not a single annulus or an extended disk, best explains the modern terrestrial system. With an inner ring at $r_1 = 0.6$ au ($\sigma_1 = 0.05$ au), an outer reservoir at $r_2 = 1.7$ au ($\sigma_2 = 0.1$ au), total initial mass 2.1 Earth masses split 2:1 between inner and outer sources, and a gas disk whose surface density flattens or rises with radius inside about 1.2 au ($\Sigma_0 = 3000$ g cm$^{-2}$ at $r_0 = 0.9$ au, $\beta_1 = -1$, $\beta_2 = 0$), the simulations produce good Venus/Earth pairs in 50% of runs, good Mars in 35%, good Mercury in 32%, and tight Venus/Earth separation in 33%; 6.1% of runs satisfy all four criteria simultaneously. In those runs Earth accretes about 70% of its mass from the inner ring and about 30% from the outer source, while Mars accretes about 90% from the outer source. The paper argues that this accretion sequence matches the reduced-then-oxidized chemistry inferred for Earth's mantle, the distinct isotopic building blocks of Mars, and the Earth-like isotopic composition of the Moon, because Theia would have grown in the same inner reservoir and on a similar timescale as the proto-Earth.

Load-bearing premise

The load-bearing premise is that the protoplanetary gas disk had a density profile that pushed newborn planets outward inside about 1.2 au; if real disks instead pushed them inward, Venus and Earth would never move from the 0.5 au nursery out to 0.7–1 au and the inner-ring story fails.

Editorial extensions

If this is right

  • Mercury's small mass and orbit are a natural by-product: the inner ring is narrow and the most massive embryos migrate outward, leaving a low-mass planet behind near 0.5 au.
  • Earth's mantle composition and the Earth-Mars isotopic difference are explained by the same mass split: about 70% inner-ring (reduced) and 30% outer-source (oxidized) material for Earth, and about 90% outer-source material for Mars.
  • Theia, the Moon-forming impactor, plausibly grew from the same inner reservoir on a similar schedule as the proto-Earth, explaining the Earth-Moon isotopic similarity without special orbital or mixing assumptions.
  • Inner-ring planetesimals should be absent from the meteorite collection, because their implantation efficiency into the asteroid belt is estimated to be below about $3 \times 10^{-7}$.
  • The best-fit model implies a gas disk with an inner density bump, most naturally produced by magnetically driven winds, and an early giant-planet instability at about 11 Myr; both are testable predictions for disk and planet-formation models.

Reading between the lines

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

  • A testable extension, not made in the paper: the same disk profile that pushes terrestrial embryos outward near 1 au is also invoked for close-in super-Earth formation, so a unified disk evolution model could tie the terrestrial ring to the super-Earth population and predict their relative formation timescales.
  • If the inner-ring reservoir is truly unsampled in meteorites, future samples from Mercury or the near-Sun small-body population should carry the reduced, refractory-enriched signature of the inner ring rather than ordinary-chondrite-like material.
  • The model's rapid assembly of Mars from the 1.5–2 au source implies measurable consequences for Mars' volatile and siderophile budgets; Mars sample-return measurements of tungsten and noble gases could test whether the last large impactor came from that outer reservoir.
  • The 6.1% all-good success rate is based on N = 400 super-particles; repeating the reference model with several thousand bodies would show whether the stated success probability is stable or partly a resolution artifact.
Share X Bluesky LinkedIn Reddit HN

Editorial analysis

A structured set of objections, weighed in public.

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

Referee Report

3 major / 4 minor

Summary. The paper presents a large suite of N-body simulations of terrestrial planet formation starting from planetesimal disks with one or two radial reservoirs, a gas disk stage with Type-I migration and aerodynamic drag, a giant-planet instability, and a long late-stage integration. The authors explore roughly one hundred model configurations with one thousand simulations each and grade outcomes against objective criteria for Mercury, Venus/Earth, Mars, and the Venus-Earth separation. Their preferred two-source model (model203), with an inner ring at 0.6 au and an outer source at 1.7 au, yields success rates (V/E, Mars, Merc, V/E Sep) = (50%, 35%, 32%, 33%) and 6.1% of runs satisfying all four criteria. The paper claims that this model explains the masses and orbits of the terrestrial planets, the reduced/oxidized accretion history of Earth, and the isotopic differences between Earth and Mars, and that it provides a plausible accretion history for the Moon-forming impactor Theia.

Significance. If the central claims hold, this would be a substantial advance: the paper demonstrates that a two-reservoir initial condition plus outward Type-I migration in a wind-like disk can simultaneously match the radial mass concentration, the Mercury problem, the small-Mars problem, and the Earth's bimodal accretion chemistry. The statistical methodology is a clear strength: one thousand simulations per model, objective planet-matching criteria defined in Section 3.1, and systematic parameter variation with results tabulated in Tables 1 and 2. The fragmentation tests in Section 4.10 and the resolution checks with N=1000 and N=2000 are also valuable. However, the paper's third headline claim, that it explains the isotopic differences of Earth and Mars, is contradicted by the authors' own quantitative caveat in Section 5, and the Earth's 70/30 composition is largely built into the chosen mass split. The central mechanism also rests on a parameterized disk profile rather than a self-consistent disk model. These issues make the paper's central conclusion conditional rather than established.

major comments (3)
  1. [Section 5 and Section 3.2.3] There is an internal inconsistency between the abstract and the quantitative Mars composition. The abstract states that the model explains 'the isotopic differences of the Earth and Mars,' and Section 4.9 and Conclusion item 6 repeat this claim. However, Section 5 states that with the 2:1 mass split, 'Mars accretes ~90% of material from the outer source... This composition would not have enough EC material to explain observations.' Given the constraints quoted in Section 3.2.3 (Mars ~65% EC, Earth ~95% EC) and the tentative mapping of the inner ring to EC and outer source to OC, model203 predicts Mars to be ~90% OC and ~10% EC, which is the opposite of the inferred EC-dominated Mars. The model can produce two isotopically distinct planets, but it does not reproduce the specific EC/OC mixture inferred for Mars. This gap must be closed, either by an explicit treatment of an unsampled reservoir, by a different assignment of isotopic reservoirs to the two source rings, or by softening the claim in the abstract and conclusions.
  2. [Section 4.8, Eq. (2), and Table 2] The Earth's ~70% inner and ~30% outer composition is largely a consequence of the chosen 2:1 mass split (w2 = 1/3 in Eq. (2)), not an independent prediction of the model. The authors state in Section 3.2.1 that the 70/30 chemical split is itself one of the geochemical constraints motivating a two-source model, and Section 5 notes that the 2:1 split 'would represent the best match to the chemical composition of the BSE.' Since model203 was selected as the best among roughly one hundred tested configurations, at least partly with this compositional prior in mind, the claimed match to the Earth's chemistry is partially circular. The paper should quantify the Earth composition for the other mass splits reported in Table 2 (model211 with w2=1/2 and model212 with w2=1/4), and demonstrate that the 70/30 outcome is not simply read off from the initial mass ratio.
  3. [Section 2.2.2 and Eq. (9)] The central dynamical mechanism relies on a parameterized gas disk profile, Eq. (9) with beta1 = -1, beta2 = 0, and Sigma0 = 3000 g/cm^2, which produces outward Type-I migration inside ~1.2 au. The authors acknowledge that this is a simple parameterization 'that roughly approximated the results of MHD simulations,' but it is load-bearing: Section 4.6 shows that without this outward migration the inner-ring model does not place Venus and Earth at 0.7-1 au, and Section 4.8 uses the same profile for the reference model. The height of the density bump and the zero-torque radius are not derived from a self-consistent disk model, and the paper does not explore time-dependent beta1 and beta2 even though the cited MHD simulations show the profile evolving. The authors should either provide a more direct connection to published MDW disk calculations, including a range of plausible profiles and evolution histories, or explicitly frame the results as conditional on this assumed disk structure.
minor comments (4)
  1. [Section 6, Conclusion item 5] The sentence 'the best results were obtained with 1.4 MEarth in the inner ring and 0.7 MEarth in the inner ring' should read '0.7 MEarth in the outer ring;' otherwise it misstates the mass split that defines model203.
  2. [Table 1, model mmsn] The Notes column describes a gas disk with 'alpha0 = -1,' but the relevant parameter appears to be the power-law index beta in Eq. (8), not alpha0; the notation should be corrected for consistency with Section 4.4.
  3. [Title page and affiliations] The affiliation for the Nice group contains a typo: 'Bouldervard de l'Observatoire' should be 'Boulevard de l'Observatoire.'
  4. [Section 4.9] The claim that late accretion estimates are unreliable because each initial planetesimal has mass ~0.5% of Earth, comparable to the HSE-inferred late veneer, is clearly stated, but it would be helpful to also state whether the N=1000 and N=2000 resolution runs reported later in the section were used to assess this specific quantity, since those runs are said to give nearly identical results.

Circularity Check

2 steps flagged · score 6.0 of 10

The dynamical simulations are self-contained, but the Earth 70/30 chemical explanation reduces to the chosen 2:1 mass split, and the abstract's Mars-isotope claim is contradicted in Section 5.

  1. fitted input called prediction [Section 4.8 (model203 parameters) and Section 4.9 / Section 5 (Earth composition)]
    "The initial mass was partitioned between the two rings such that there is the mass m1 = 1.4 MEarth in the inner ring and the mass m2 = 0.7 MEarth in the outer source (w2 = 1/3 in Eq. 2). ... For the 2:1 mass split between the inner and outer sources (w2 = 1/3 in Eq. 2), we find that the Earth accretes ∼ 70% of material from the inner ring and ∼ 30% of material from the outer source (Fig. 13A). This case would represent the best match to the chemical composition of the BSE."

    Section 3.2.1 states the geochemical inference that the Earth accreted ~70% reduced then ~30% oxidized material and says 'This constraint supplies some justification for the two-source model.' The reference model then fixes the initial reservoir mass split at exactly the same 2:1 ratio (1.4 vs 0.7 MEarth). With mostly local accretion, the resulting Earth budget (~70/30) is the input mass ratio returned as output, so the headline chemical 'explanation' is partly self-definitional rather than an independent prediction.

  2. other [Abstract vs Section 5 (Discussion), third paragraph]
    "This model explains: ... (3) the isotopic differences of the Earth and Mars. ... On the other hand, a 2:1 mass split between the inner and outer sources would produce a Mars that accretes ∼ 90% of material from the outer source and ∼ 10% of material from the inner ring (on average; Fig. 13B). This composition would not have enough EC material to explain observations."

    This is an internal contradiction rather than a construction-circularity, but it removes the Mars-isotope support from the central claim. The reference model's predicted Mars budget (~90% outer / ~10% inner) is the opposite of the ~65% EC / ~33% OC mix inferred in Section 3.2.3, and the authors explicitly admit the model 'would not have enough EC material to explain observations.' The abstract nevertheless lists 'the isotopic differences of the Earth and Mars' as one of the model's explanations.

full rationale

The N-body derivation itself is not circular: the success rates (V/E, Mars, Merc, V/E Sep = 50%, 35%, 32%, 33%; 6.1% all-good) are genuine stochastic outcomes of the integrations, and the disk profile of Eq. (9) is an assumed parameterization rather than a disguised result. Self-citations (e.g., Morbidelli et al. 2022 for the silicate-line ring, NM12 for the instability) are not used as uniqueness theorems and do not by themselves force the conclusions. The principal circularity is the Earth-composition claim: the 70/30 reduced/oxidized geochemical constraint (Section 3.2.1) is used to justify the two-source model, the reference model sets the inner/outer mass split to the same 2:1 ratio, and Section 5 then reports the ~70/30 Earth budget as the 'best match.' That is a fitted input presented as a finding. The Mars-isotope claim is, by the authors' own admission in Section 5, not satisfied by the reference model (90% outer-source material), which contradicts the abstract's third claimed explanation. The 6.1% figure is a tuned maximum over ~100 tested models, which is model selection rather than circularity but should be read as a benchmark, not a blind prediction. On balance: partial circularity in one headline explanation and an admitted failure in another, with an otherwise self-contained dynamical study.

Assumptions & free parameters 9 free parameters · 8 assumptions · 2 invented entities

The central claim rests on several tuned initial conditions (ring locations, widths, mass split, disk density) and on domain assumptions about planetesimal formation at the silicate sublimation line, the existence of an outer reservoir, and the MDW disk profile. The most significant circularity is the mass split w2=1/3, which is chosen partly to match the Earth's 70/30 composition that the paper then presents as a success. The dynamical success rates provide some independent grounding, but the model selection over ~100 parameter sets means the reported 6.1% success is an optimized value. The two invented reservoirs are inferred, not directly observed, and their origins are deferred.

free parameters (9)
  • Inner ring location r1 = 0.6 au (model203); best range 0.4-0.6 au
    Varied from 0.3 to 0.7 au across models; r1 controls Mercury's location and Venus/Earth formation. Tuned to maximize success rates.
  • Inner ring width sigma1 = 0.05 au (model203)
    Tested 0.025 to 0.2 au; narrow rings work best, consistent with silicate sublimation line origin.
  • Outer source location r2 = 1.7 au (model203)
    Varied 1.5 to 2.1 au; Mars success rate drops for r2=1.5 au. Tuned to produce good Mars.
  • Outer source width sigma2 = 0.1 au (model203)
    Tested 0.1 to 0.4 au; wider outer sources improve Mars success.
  • Mass split w2 = 1/3 (2:1 inner:outer)
    Tested 1:1 and 3:1 splits; the 2:1 split produces the desired ~70/30 Earth composition, coupling this parameter to the geochemical constraint.
  • Gas disk normalization Sigma0 = 3000 g/cm2
    Varied 1500 to 6000 g/cm2; controls migration strength and Venus/Earth separation. Tuned as a compromise between Mars and Venus/Earth criteria.
  • Disk profile parameters beta1, beta2 = beta1=-1, beta2=0
    Chosen to mimic MDW disks; not systematically varied, but the profile is load-bearing for outward migration.
  • Turbulence amplitude kappa = 3e-6
    Chosen to improve Mercury success; a single test without turbulence (model220) lowers Mercury success from 32% to 16%.
  • Total mass Mtot = 2.1 Earth masses
    Taken from Hansen (2009) and Woo et al. (2024); not fitted to success, but affects final planet masses.
assumptions (8)
  • standard math The Symba symplectic integrator accurately models encounters between massive bodies over 300 Myr.
    Used in all simulations; the paper cites Wisdom & Holman (1991) and Duncan et al. (1998) for its accuracy.
  • domain assumption Type-I migration torque formulas from Paardekooper et al. (2010, 2011) and Ogihara et al. (2014) apply to growing protoplanets in the modeled disks.
    The migration and damping forces use these prescriptions (Section 2.2.1); deviations from these torque models would change migration directions and rates.
  • ad hoc to paper The parameterized MDW disk profile (Eq. 9) approximates the surface density of real magnetically driven wind disks.
    The paper states this is a simple parameterization that 'roughly approximated the results of MHD simulations' (Section 2.2.2); it is not a self-consistent disk model.
  • domain assumption Planetesimals formed in a narrow ring near the silicate sublimation line at ~0.5 au.
    Motivated by Morbidelli et al. (2022) and Marschall & Morbidelli (2023); the paper notes Carrera et al. (2025) challenges this in turbulent disks.
  • domain assumption An outer planetesimal reservoir existed at 1.5 to 2 au.
    Inferred from the need to form Mars with a distinct isotopic composition; the paper defers the origin of this source to future work.
  • domain assumption The giant planet instability occurred at ~11 Myr following the NM12 Case 1 five-planet model.
    The instability model is taken from Nesvorny & Morbidelli (2012); other instability timings and configurations are not tested for the two-source model.
  • domain assumption Perfect mergers in most simulations approximate real collisions.
    The bulk of simulations assume perfect mergers; tests with fragmentation (Section 4.10) show some differences, especially for Mercury's mass.
  • ad hoc to paper The collisional fragmentation algorithm's mass removal approximates real mass loss.
    The paper acknowledges the algorithm exaggerates mass wasting by removing all fragments smaller than 1e-4 Earth masses (Section 2.5).
invented entities (2)
  • Inner ring planetesimal reservoir at ~0.5 au
    purpose: Source of Mercury, Venus, and Earth; supplies reduced, enstatite-chondrite-like material that is unsampled in meteorite collections.
    Postulated to explain the inner planet formation and Earth's reduced component. The paper predicts an implantation efficiency below 3e-7, meaning the reservoir is effectively absent from the asteroid belt, so no direct falsifiable handle exists outside the paper.
  • Outer planetesimal reservoir at 1.5 to 2 au
    purpose: Source of Mars and roughly 30% of Earth's late-accreted oxidized material.
    Inferred dynamically to produce a small Mars with a distinct isotopic composition; the origin of this reservoir is left to future work (Goldberg et al., in preparation), so it lacks independent evidence.

how reviews work

0 comments
Cite this review

Pith. "Pith review of Terrestrial Planet Formation from Two Source Reservoirs." pith.science (2026). https://pith.science/paper/PR3DDYUW

@misc{pith2026250714814,
  author       = {Pith},
  title        = {Pith review of: Terrestrial Planet Formation from Two Source Reservoirs},
  year         = {2026},
  howpublished = {\url{https://pith.science/paper/PR3DDYUW}},
  note         = {Machine review of arXiv:2507.14814}
}
read the original abstract

This work describes new dynamical simulations of terrestrial planet formation. The simulations started at the protoplanetary disk stage, when planetesimals formed and accreted into protoplanets, and continued past the late stage of giant impacts. We explored the effect of different parameters, such as the initial radial distribution of planetesimals and Type-I migration of protoplanets, on the final results. In each case, a thousand simulations were completed to characterize the stochastic nature of the accretion process. In the model best able to satisfy various constraints, Mercury, Venus, and Earth accreted from planetesimals that formed early near the silicate sublimation line near 0.5 au and migrated by disk torques. For Venus and Earth to end up at 0.7-1 au, Type-I migration had to be directed outward, for example as the magnetically driven winds reduced the surface gas density in the inner part of the disk. Mercury was left behind near the original ring location. We suggest that Mars and multiple Mars-sized protoplanets grew from a distinct outer source of planetesimals at 1.5-2 au. While many migrated inwards to accrete onto the proto-Earth, our Mars was the lone survivor. This model explains: (1) the masses and orbits of the terrestrial planets, (2) the chemical composition of the Earth, where ~70% and ~30% come from reduced inner-ring and more-oxidized outer-ring materials, and (3) the isotopic differences of the Earth and Mars. It suggests that the Moon-forming impactor Theia plausibly shared a similar isotopic composition and accretion history with that of the proto-Earth.

Figures

Figures reproduced from arXiv: 2507.14814 by the authors.

Figure 1
Figure 1. — The initial surface densities of gas disks considered in this work and elsewhere. [PITH_FULL_IMAGE:figures/full_fig_p073_1.png] view at source ↗
Figure 2
Figure 2. — A migration map for the MDW disk given by Eq. (9) with Σ [PITH_FULL_IMAGE:figures/full_fig_p074_2.png] view at source ↗
Figure 3
Figure 3. — The orbital histories of outer planets in our instability model. The planets started [PITH_FULL_IMAGE:figures/full_fig_p075_3.png] view at source ↗
Figures from the paper (14 more)
Figure 4
Figure 4. Figure 4: — A comparison between the scaling laws of Leinhardt & Stewart (2012) and the SPH [PITH_FULL_IMAGE:figures/full_fig_p076_4.png]
Figure 5
Figure 5. Figure 5: — The result of 100 successful simulations of the [PITH_FULL_IMAGE:figures/full_fig_p077_5.png]
Figure 6
Figure 6. Figure 6: — The result of 100 successful simulations of the [PITH_FULL_IMAGE:figures/full_fig_p078_6.png]
Figure 7
Figure 7. Figure 7: — The accretion history of planets in one of the best cases from the simulation set [PITH_FULL_IMAGE:figures/full_fig_p079_7.png]
Figure 8
Figure 8. Figure 8: — The Venus/Earth separation, ∆a, and the average eccentricities/inclinations, ⟨e, i⟩, for 111 successful simulations from 0.01au (the narrow ring at 0.85 au with a 20% back￾ground) that produced good terrestrial planets (as defined in Section 3.1). The triangles show …
Figure 9
Figure 9. Figure 9: — The planet growth and migration in the [PITH_FULL_IMAGE:figures/full_fig_p081_9.png]
Figure 10
Figure 10. Figure 10: — The result of 61 simulations from model203 (r1 = 0.6 au and r2 = 1.7 au, no background, strong convergent migration) that simultaneously produced a good match to Mercury, Venus, Earth and Mars (as defined in Section 3.1). The black dots show the final results in eac…
Figure 11
Figure 11. Figure 11: — The result of 61 simulations from model203 (r1 = 0.6 au and r2 = 1.7 au, no background, strong convergent migration) that simultaneously produced a good match to Mercury, Venus, Earth and Mars (as defined in Section 3.1). The black dots show the final results in eac…
Figure 12
Figure 12. Figure 12: — The Venus/Earth separation, ∆a, and the average eccentricities/inclinations, ⟨e, i⟩, for 61 simulations from model203 (r1 = 0.6 au and r2 = 1.7 au, no background, strong convergent migration) that produced good terrestrial planets (as defined in Section 3.1). The tr…
Figure 13
Figure 13. Figure 13: — The fraction of Earth and Mars mass accreted from beyond the orbital radius [PITH_FULL_IMAGE:figures/full_fig_p085_13.png]
Figure 14
Figure 14. Figure 14: — Earth’s growth in the successful simulations from [PITH_FULL_IMAGE:figures/full_fig_p086_14.png]
Figure 15
Figure 15. Figure 15: — The growth of planets in the successful simulations from [PITH_FULL_IMAGE:figures/full_fig_p087_15.png]
Figure 16
Figure 16. Figure 16: — Panel A. The last giant impact on the Earth in our reference model (model203). We collected all successful simulations and determined the last giant impact on the proto￾Earth (as defined in the main text). The triangles show the time of the last giant impact, tgiant…
Figure 17
Figure 17. Figure 17: — The radial distribution of terrestrial planetesimals in the successful two-source [PITH_FULL_IMAGE:figures/full_fig_p089_17.png]

Discussion (0). Continue with ORCID to comment.

Reference graph

Works this paper leans on

157 extracted references · 37 canonical work pages

  1. [1]

    Agnor, C. B. & Lin, D. N. C.\ 2012, , On the Migration of Jupiter and Saturn: Constraints from Linear Models of Secular Resonant Coupling with the Terrestrial Planets, 745, 2, 143. doi:10.1088/0004-637X/745/2/143

    doi:10.1088/0004-637x/745/2/143 2012

  2. [2]

    B., Canup, R

    Agnor, C. B., Canup, R. M., & Levison, H. F.\ 1999, Icarus, 142, 1, 219. doi:10.1006/icar.1999.6201

    arXiv 1999

  3. [3]

    Andrews-Hanna, J. C. & Bottke, W. B.\ 2017, Fourth International Conference on Early Mars: Geologic, Hydrologic, and Climatic Evolution and the Implications for Life, Mars During the Pre-Noachian, 2014, 3078

    2017

  4. [4]

    J.\ 2011, , Dynamics of Protoplanetary Disks, 49, 1, 195

    Armitage, P. J.\ 2011, , Dynamics of Protoplanetary Disks, 49, 1, 195. doi:10.1146/annurev-astro-081710-102521

    doi:10.1146/annurev-astro-081710-102521 2011

  5. [5]

    & Reufer, A.\ 2014, Nature Geoscience, Mercury and other iron-rich planetary bodies as relics of inefficient accretion, 7, 8, 564

    Asphaug, E. & Reufer, A.\ 2014, Nature Geoscience, Mercury and other iron-rich planetary bodies as relics of inefficient accretion, 7, 8, 564. doi:10.1038/ngeo2189

    doi:10.1038/ngeo2189 2014

  6. [6]

    doi:10.1126/sciadv.1602365

    Barboni, M., Boehnke, P., Keller, B., et al.\ 2017, Science Advances, Early formation of the Moon 4.51 billion years ago, 3, 1, e1602365. doi:10.1126/sciadv.1602365

    doi:10.1126/sciadv.1602365 2017

  7. [7]

    E., & Betts, H.\ 2012, , Instability-driven Dynamical Evolution Model of a Primordially Five-planet Outer Solar System, 744, 1, L3

    Batygin, K., Brown, M. E., & Betts, H.\ 2012, , Instability-driven Dynamical Evolution Model of a Primordially Five-planet Outer Solar System, 744, 1, L3. doi:10.1088/2041-8205/744/1/L3

    work page doi:10.1088/2041-8205/744/1/l3 2012

  8. [8]

    & Kley, W.\ 2010, , Orbital evolution of eccentric planets in radiative discs, 523, A30

    Bitsch, B. & Kley, W.\ 2010, , Orbital evolution of eccentric planets in radiative discs, 523, A30. doi:10.1051/0004-6361/201014414

    doi:10.1051/0004-6361/201014414 2010

Show all 157 references
  1. [9]

    doi:10.1051/0004-6361/201424964

    Bitsch, B., Johansen, A., Lambrechts, M., et al.\ 2015, , The structure of protoplanetary discs around evolving young stars, 575, A28. doi:10.1051/0004-6361/201424964

    2015 doi

  2. [10]

    F., Nesvorn \'y , D., Grimm, R

    Bottke, W. F., Nesvorn \'y , D., Grimm, R. E., et al.\ 2006, , Iron meteorites as remnants of planetesimals formed in the terrestrial planet region, 439, 7078, 821. doi:10.1038/nature04536

    2006 doi

  3. [11]

    F., Walker, R

    Bottke, W. F., Walker, R. J., Day, J. M. D., et al.\ 2010, Science, Stochastic Late Accretion to Earth, the Moon, and Mars, 330, 6010, 1527. doi:10.1126/science.1196874

    2010 doi

  4. [12]

    F., Vokrouhlick \'y , D., Minton, D., et al.\ 2012, , An Archaean heavy bombardment from a destabilized extension of the asteroid belt, 485, 7396, 78

    Bottke, W. F., Vokrouhlick \'y , D., Minton, D., et al.\ 2012, , An Archaean heavy bombardment from a destabilized extension of the asteroid belt, 485, 7396, 78. doi:10.1038/nature10967

    2012 doi

  5. [13]

    E., Gaffney, A

    Borg, L. E., Gaffney, A. M., & Shearer, C. K.\ 2015, MAPS, A review of lunar chronology revealing a preponderance of 4.34-4.37 Ga ages, 50, 4, 715. doi:10.1111/maps.12373

    2015 doi

  6. [14]

    E., Gaffney, A

    Borg, L. E., Gaffney, A. M., Kruijer, T. S., et al.\ 2019, Earth and Planetary Science Letters, Isotopic evidence for a young lunar magma ocean, 523, 115706. doi:10.1016/j.epsl.2019.07.008

    2019 doi

  7. [15]

    J., & Levison, H

    Brasser, R., Duncan, M. J., & Levison, H. F.\ 2007, Icarus, Embedded star clusters and the formation of the Oort cloud. II. The effect of the primordial solar nebula, 191, 2, 413. doi:10.1016/j.icarus.2007.05.003

    2007 doi

  8. [16]

    doi:10.1051/0004-6361/200912878

    Brasser, R., Morbidelli, A., Gomes, R., et al.\ 2009, , Constructing the secular architecture of the solar system II: the terrestrial planets, 507, 2, 1053. doi:10.1051/0004-6361/200912878

    2009 doi

  9. [17]

    doi:10.1038/s41550-021-01383-3

    Bro z , M., Chrenko, O., Nesvorn \'y , D., et al.\ 2021, Nature Astronomy, Early terrestrial planet formation by torque-driven convergent migration of planetary embryos, 5, 898. doi:10.1038/s41550-021-01383-3

    2021 doi

  10. [18]

    S., & Kleine, T.\ 2018, , Hf-W chronology of CR chondrites: Implications for the timescales of chondrule formation and the distribution of ^ 26 Al in the solar nebula, 222, 284

    Budde, G., Kruijer, T. S., & Kleine, T.\ 2018, , Hf-W chronology of CR chondrites: Implications for the timescales of chondrule formation and the distribution of ^ 26 Al in the solar nebula, 222, 284. doi:10.1016/j.gca.2017.10.014

    2018 doi

  11. [19]

    doi:10.1126/sciadv.abj7601

    Burkhardt, C., Spitzer, F., Morbidelli, A., et al.\ 2021, Science Advances, Terrestrial planet formation from lost inner solar system material, 7, 52, eabj7601. doi:10.1126/sciadv.abj7601

    2021 doi

  12. [20]

    J., et al.\ 2019, Icarus, Constraining the thermal properties of planetary surfaces using machine learning: Application to airless bodies, 325, 16

    Cambioni, S., Delbo, M., Ryan, A. J., et al.\ 2019, Icarus, Constraining the thermal properties of planetary surfaces using machine learning: Application to airless bodies, 325, 16. doi:10.1016/j.icarus.2019.01.017

    2019 doi

  13. [21]

    M.\ 2012, Science, Forming a Moon with an Earth-like Composition via a Giant Impact, 338, 6110, 1052

    Canup, R. M.\ 2012, Science, Forming a Moon with an Earth-like Composition via a Giant Impact, 338, 6110, 1052. doi:10.1126/science.1226073

    2012 doi

  14. [22]

    M., Righter, K., Dauphas, N., et al.\ 2023, Reviews in Mineralogy and Geochemistry, Origin of the Moon, 89, 1, 53

    Canup, R. M., Righter, K., Dauphas, N., et al.\ 2023, Reviews in Mineralogy and Geochemistry, Origin of the Moon, 89, 1, 53. doi:10.2138/rmg.2023.89.02

    2023 doi

  15. [23]

    B., Li, R., et al.\ 2021, , Protoplanetary Disk Rings as Sites for Planetesimal Formation, 161, 2, 96

    Carrera, D., Simon, J. B., Li, R., et al.\ 2021, , Protoplanetary Disk Rings as Sites for Planetesimal Formation, 161, 2, 96. doi:10.3847/1538-3881/abd4d9

    2021 doi

  16. [24]

    B., et al.\ 2025, Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall, arXiv:2504.13246

    Carrera, D., Davenport, A., Simon, J. B., et al.\ 2025, Turbulence Inhibits Planetesimal Formation in Class 0/I Disks Subject to Infall, arXiv:2504.13246. doi:10.48550/arXiv.2504.13246

    2025 doi arXiv

  17. [25]

    E.\ 2001, Icarus, Making More Terrestrial Planets, 152, 2, 205

    Chambers, J. E.\ 2001, Icarus, Making More Terrestrial Planets, 152, 2, 205. doi:10.1006/icar.2001.6639

    2001

  18. [26]

    E.\ 2013, Icarus, Late-stage planetary accretion including hit-and-run collisions and fragmentation, 224, 1, 43

    Chambers, J. E.\ 2013, Icarus, Late-stage planetary accretion including hit-and-run collisions and fragmentation, 224, 1, 43. doi:10.1016/j.icarus.2013.02.015

    2013 doi

  19. [27]

    Chambers, J. E. & Wetherill, G. W.\ 1998, Icarus, Making the Terrestrial Planets: N-Body Integrations of Planetary Embryos in Three Dimensions, 136, 2, 304. doi:10.1006/icar.1998.6007

    1998

  20. [28]

    Chambers, J. E. & Cassen, P.\ 2002, MAPS, 37, 11, 1523. doi:10.1111/j.1945-5100.2002.tb00808.x

    2002

  21. [29]

    O., D'Angelo, G., Reyes-Ruiz, M., et al.\ 2020, , Capture and migration of Jupiter and Saturn in mean motion resonance in a gaseous protoplanetary disc, 492, 4, 6007

    Chametla, R. O., D'Angelo, G., Reyes-Ruiz, M., et al.\ 2020, , Capture and migration of Jupiter and Saturn in mean motion resonance in a gaseous protoplanetary disc, 492, 4, 6007. doi:10.1093/mnras/staa260

    2020 doi

  22. [30]

    Chou, C.-L.\ 1978, Lunar and Planetary Science Conference Proceedings, Fractionation of Siderophile Elements in the Earth's Upper Mantle, 1, 219

    1978

  23. [31]

    M., & Crocket, J

    Chou, C.-L., Shaw, D. M., & Crocket, J. H.\ 1983, Lunar and Planetary Science Conference Proceedings, Siderophile trace elements in the Earth's oceanic crust and upper mantle, 88, 507. doi:10.1029/JB088iS02p0A507

    1983 doi

  24. [32]

    S., Kaib, N

    Clement, M. S., Kaib, N. A., Raymond, S. N., et al.\ 2018, Icarus, Mars' growth stunted by an early giant planet instability, 311, 340. doi:10.1016/j.icarus.2018.04.008

    2018 doi

  25. [33]

    S., Kaib, N

    Clement, M. S., Kaib, N. A., & Chambers, J. E.\ 2019, , Dynamical Constraints on Mercury s Collisional Origin, 157, 5, 208. doi:10.3847/1538-3881/ab164f

    2019 doi

  26. [34]

    S., Kaib, N

    Clement, M. S., Kaib, N. A., Raymond, S. N., et al.\ 2021a, Icarus, The early instability scenario: Mars' mass explained by Jupiter's orbit, 367, 114585. doi:10.1016/j.icarus.2021.114585

    2021

  27. [35]

    S., Raymond, S

    Clement, M. S., Raymond, S. N., & Chambers, J. E.\ 2021b, , 923, 1, L16. doi:10.3847/2041-8213/ac3e6d

    doi

  28. [36]

    S., Chambers, J

    Clement, M. S., Chambers, J. E., Kaib, N. A., et al.\ 2023, Icarus, Mercury's formation within the early instability scenario, 394, 115445. doi:10.1016/j.icarus.2023.115445

    2023

  29. [37]

    N., Bizzarro, M., Krot, A

    Connelly, J. N., Bizzarro, M., Krot, A. N., et al.\ 2012, Science, The Absolute Chronology and Thermal Processing of Solids in the Solar Protoplanetary Disk, 338, 6107, 651. doi:10.1126/science.1226919

    2012 doi

  30. [38]

    & Nelson, R

    Cresswell, P. & Nelson, R. P.\ 2008, , Three-dimensional simulations of multiple protoplanets embedded in a protostellar disc, 482, 2, 677. doi:10.1051/0004-6361:20079178

    2008 doi

  31. [39]

    I., Morbidelli, A., Rubie, D

    Dale, K. I., Morbidelli, A., Rubie, D. C., et al.\ 2025, Earth and Planetary Science Letters, Compositional outcomes of Earth formation from a narrow ring, 658, 119334. doi:10.1016/j.epsl.2025.119334

    2025

  32. [40]

    doi:10.1038/nature20830

    Dauphas, N.\ 2017, , The isotopic nature of the Earth s accreting material through time, 541, 7638, 521. doi:10.1038/nature20830

    2017 doi

  33. [41]

    & Marty, B.\ 2002, Journal of Geophysical Research (Planets), Inference on the nature and the mass of Earth's late veneer from noble metals and gases, 107, E12, 5129

    Dauphas, N. & Marty, B.\ 2002, Journal of Geophysical Research (Planets), Inference on the nature and the mass of Earth's late veneer from noble metals and gases, 107, E12, 5129. doi:10.1029/2001JE001617

    2002 doi

  34. [42]

    & Pourmand, A.\ 2011, , Hf-W-Th evidence for rapid growth of Mars and its status as a planetary embryo, 473, 7348, 489

    Dauphas, N. & Pourmand, A.\ 2011, , Hf-W-Th evidence for rapid growth of Mars and its status as a planetary embryo, 473, 7348, 489. doi:10.1038/nature10077

    2011 doi

  35. [43]

    & Schauble, E

    Dauphas, N. & Schauble, E. A.\ 2016, Annual Review of Earth and Planetary Sciences, Mass Fractionation Laws, Mass-Independent Effects, and Isotopic Anomalies, 44, 709. doi:10.1146/annurev-earth-060115-012157

    2016 doi

  36. [44]

    doi:10.1016/j.icarus.2023.115805

    Dauphas, N., Hopp, T., & Nesvorn \'y , D.\ 2024, Icarus, Bayesian inference on the isotopic building blocks of Mars and Earth, 408, 115805. doi:10.1016/j.icarus.2023.115805

    2024

  37. [45]

    Day, J. M. D. & Walker, R. J.\ 2015, Earth and Planetary Science Letters, Highly siderophile element depletion in the Moon, 423, 114. doi:10.1016/j.epsl.2015.05.001

    2015 doi

  38. [46]

    doi:10.1088/0004-6256/148/2/25

    Deienno, R., Nesvorn \'y , D., Vokrouhlick \'y , D., et al.\ 2014, , Orbital Perturbations of the Galilean Satellites during Planetary Encounters, 148, 2, 25. doi:10.1088/0004-6256/148/2/25

    2014 doi

  39. [47]

    S., et al.\ 2017, , Constraining the Giant Planets' Initial Configuration from Their Evolution: Implications for the Timing of the Planetary Instability, 153, 4, 153

    Deienno, R., Morbidelli, A., Gomes, R. S., et al.\ 2017, , Constraining the Giant Planets' Initial Configuration from Their Evolution: Implications for the Timing of the Planetary Instability, 153, 4, 153. doi:10.3847/1538-3881/aa5eaa

    2017 doi

  40. [48]

    J., Kretke, K

    Deienno, R., Walsh, K. J., Kretke, K. A., et al.\ 2019, , Energy Dissipation in Large Collisions No Change in Planet Formation Outcomes, 876, 2, 103. doi:10.3847/1538-4357/ab16e1

    2019 doi

  41. [49]

    P., Birnstiel, T., Huang, J., et al.\ 2018, , The Disk Substructures at High Angular Resolution Project (DSHARP)

    Dullemond, C. P., Birnstiel, T., Huang, J., et al.\ 2018, , The Disk Substructures at High Angular Resolution Project (DSHARP). VI. Dust Trapping in Thin-ringed Protoplanetary Disks, 869, 2, L46. doi:10.3847/2041-8213/aaf742

    2018 doi

  42. [50]

    J., Levison, H

    Duncan, M. J., Levison, H. F., & Lee, M. H.\ 1998, , A Multiple Time Step Symplectic Algorithm for Integrating Close Encounters, 116, 4, 2067. doi:10.1086/300541

    1998 doi

  43. [51]

    & Alibert, Y.\ 2017, , Planetesimal formation starts at the snow line, 608, A92

    Dra \.z kowska, J. & Alibert, Y.\ 2017, , Planetesimal formation starts at the snow line, 608, A92. doi:10.1051/0004-6361/201731491

    2017 doi

  44. [52]

    Emsenhuber, A., Cambioni, S., Asphaug, E., et al.\ 2020, , Realistic On-the-fly Outcomes of Planetary Collisions. II. Bringing Machine Learning to N-body Simulations, 891, 1, 6. doi:10.3847/1538-4357/ab6de5

    2020 doi

  45. [53]

    doi:10.3847/PSJ/ad2178

    Emsenhuber, A., Asphaug, E., Cambioni, S., et al.\ 2024, PSJ, A New Database of Giant Impacts over a Wide Range of Masses and with Material Strength: A First Analysis of Outcomes, 5, 3, 59. doi:10.3847/PSJ/ad2178

    2024 doi

  46. [54]

    Eriksson, L. E. J., Ronnet, T., & Johansen, A.\ 2021, , 648, A112. doi:10.1051/0004-6361/202039889

    2021 doi

  47. [55]

    Fischer, R. A. & Nimmo, F.\ 2018, Earth and Planetary Science Letters, Effects of core formation on the Hf-W isotopic composition of the Earth and dating of the Moon-forming impact, 499, 257. doi:10.1016/j.epsl.2018.07.03

    2018 doi

  48. [56]

    M., Hughes, A

    Flaherty, K. M., Hughes, A. M., Rose, S. C., et al.\ 2017, , A Three-dimensional View of Turbulence: Constraints on Turbulent Motions in the HD 163296 Protoplanetary Disk Using DCO ^ + , 843, 2, 150. doi:10.3847/1538-4357/aa79f9

    2017 doi

  49. [57]

    J., et al.\ 2017, , 3D Radiation Nonideal Magnetohydrodynamical Simulations of the Inner Rim in Protoplanetary Disks, 835, 2, 230

    Flock, M., Fromang, S., Turner, N. J., et al.\ 2017, , 3D Radiation Nonideal Magnetohydrodynamical Simulations of the Inner Rim in Protoplanetary Disks, 835, 2, 230. doi:10.3847/1538-4357/835/2/230

    2017 doi

  50. [58]

    C., et al.\ 2025, Forming Mercury by a grazing giant collision involving similar mass bodies, arXiv:2503.02826

    Franco, P., Roig, F., Winter, O. C., et al.\ 2025, Forming Mercury by a grazing giant collision involving similar mass bodies, arXiv:2503.02826. doi:10.48550/arXiv.2503.02826

    2025 doi arXiv

  51. [59]

    M., Gross, J., Borg, L

    Gaffney, A. M., Gross, J., Borg, L. E., et al.\ 2023, Reviews in Mineralogy and Geochemistry, Magmatic Evolution I: Initial Differentiation of the Moon, 89, 1, 103. doi:10.2138/rmg.2023.89.03

    2023 doi

  52. [60]

    & Tedesco, E.\ 1982, Science, Compositional Structure of the Asteroid Belt, 216, 4553, 1405

    Gradie, J. & Tedesco, E.\ 1982, Science, Compositional Structure of the Asteroid Belt, 216, 4553, 1405. doi:10.1126/science.216.4553.1405

    1982

  53. [61]

    S., Bhattacharjee, S., Mardaru, G.-D., et al.\ 2025, , Tracing the origin of volatiles on Earth using nitrogen isotope ratios in iron meteorites, 388, 34

    Grewal, D. S., Bhattacharjee, S., Mardaru, G.-D., et al.\ 2025, , Tracing the origin of volatiles on Earth using nitrogen isotope ratios in iron meteorites, 388, 34. doi:10.1016/j.gca.2024.11.011

    2025 doi

  54. [62]

    Grimm, S. L. & Stadel, J. G.\ 2014, , The GENGA Code: Gravitational Encounters in N-body Simulations with GPU Acceleration, 796, 1, 23. doi:10.1088/0004-637X/796/1/23

    2014 doi

  55. [63]

    C., et al.\ 2024, , The Solar System could have formed in a low-viscosity disc: A dynamical study from giant planet migration to the Nice model, 688, A202

    Griveaud, P., Crida, A., Petit, A. C., et al.\ 2024, , The Solar System could have formed in a low-viscosity disc: A dynamical study from giant planet migration to the Nice model, 688, A202. doi:10.1051/0004-6361/202450340

    2024 doi

  56. [64]

    doi:10.1143/PTPS.70.35

    Hayashi, C.\ 1981, Progress of Theoretical Physics Supplement, Structure of the Solar Nebula, Growth and Decay of Magnetic Fields and Effects of Magnetic and Turbulent Viscosities on the Nebula, 70, 35. doi:10.1143/PTPS.70.35

    1981 doi

  57. [65]

    E., Lada, E

    Haisch, K. E., Lada, E. A., & Lada, C. J.\ 2001, , Disk Frequencies and Lifetimes in Young Clusters, 553, 2, L153. doi:10.1086/320685

    2001 doi

  58. [66]

    Hansen, B. M. S.\ 2009, , Formation of the Terrestrial Planets from a Narrow Annulus, 703, 1, 1131. doi:10.1088/0004-637X/703/1/1131

    2009 doi

  59. [67]

    A., Margot, J.-L., Solomon, S

    Hauck, S. A., Margot, J.-L., Solomon, S. C., et al.\ 2013, Journal of Geophysical Research (Planets), The curious case of Mercury's internal structure, 118, 6, 1204. doi:10.1002/jgre.20091

    2013 doi

  60. [68]

    N., et al.\ 2022, Nature Astronomy, Planetesimal rings as the cause of the Solar System's planetary architecture, 6, 357

    Izidoro, A., Dasgupta, R., Raymond, S. N., et al.\ 2022, Nature Astronomy, Planetesimal rings as the cause of the Solar System's planetary architecture, 6, 357. doi:10.1038/s41550-021-01557-z

    2022 doi

  61. [69]

    Jacobson, S. A. & Dobson, C.\ 2022, Ancient Venus Conference, What Does It Mean to Have No Moon? Evidence for an Early or No Giant Impact on Venus, 2680, 2030

    2022

  62. [70]

    A., Morbidelli, A., Raymond, S

    Jacobson, S. A., Morbidelli, A., Raymond, S. N., et al.\ 2014, , Highly siderophile elements in Earth's mantle as a clock for the Moon-forming impact, 508, 7494, 84. doi:10.1038/nature13172

    2014 doi

  63. [71]

    A., Rubie, D

    Jacobson, S. A., Rubie, D. C., Hernlund, J., et al.\ 2017, Earth and Planetary Science Letters, Formation, stratification, and mixing of the cores of Earth and Venus, 474, 375. doi:10.1016/j.epsl.2017.06.023

    2017 doi

  64. [72]

    R., Owen, J

    Jankovic, M. R., Owen, J. E., Mohanty, S., et al.\ 2021, , MRI-active inner regions of protoplanetary discs. I. A detailed model of disc structure, 504, 1, 280. doi:10.1093/mnras/stab920

    2021 doi

  65. [73]

    doi:10.1126/sciadv.abc0444

    Johansen, A., Ronnet, T., Bizzarro, M., et al.\ 2021, Science Advances, A pebble accretion model for the formation of the terrestrial planets in the Solar System, 7, 8, eabc0444. doi:10.1126/sciadv.abc0444

    2021 doi

  66. [74]

    & Dorn, C.\ 2022, , 662, A19

    Johansen, A. & Dorn, C.\ 2022, , 662, A19. doi:10.1051/0004-6361/202243480

    2022 doi

  67. [75]

    Leinhardt, Z. M. & Stewart, S. T.\ 2012, , Collisions between Gravity-dominated Bodies. I. Outcome Regimes and Scaling Laws, 745, 1, 79. doi:10.1088/0004-637X/745/1/79

    2012 doi

  68. [76]

    doi:10.1016/j.chemer.2010.02.002

    Keil, K.\ 2010, Chemie der Erde / Geochemistry, Enstatite achondrite meteorites (aubrites) and the histories of their asteroidal parent bodies, 70, 4, 295. doi:10.1016/j.chemer.2010.02.002

    2010 doi

  69. [77]

    Kimura, K., Lewis, R. S., & Anders, E.\ 1974, , Distribution of gold and rhenium between nickel-iron and silicate melts: implications for the abundance of siderophile elements on the Earth and Moon, 38, 5, 683. doi:10.1016/0016-7037(74)90144-6

    1974 doi

  70. [78]

    & Schreiber, A.\ 2020, , Turbulence Sets the Length Scale for Planetesimal Formation: Local 2D Simulations of Streaming Instability and Planetesimal Formation, 901, 1, 54

    Klahr, H. & Schreiber, A.\ 2020, , Turbulence Sets the Length Scale for Planetesimal Formation: Local 2D Simulations of Streaming Instability and Planetesimal Formation, 901, 1, 54. doi:10.3847/1538-4357/abac58

    2020 doi

  71. [79]

    & Walker, R

    Kleine, T. & Walker, R. J.\ 2017, Annual Review of Earth and Planetary Sciences, Tungsten Isotopes in Planets, 45, 1, 389. doi:10.1146/annurev-earth-063016-020037

    2017 doi

  72. [80]

    & Dauphas, N.\ 2013, Icarus, Small planetesimals in a massive disk formed Mars, 225, 1, 122

    Kobayashi, H. & Dauphas, N.\ 2013, Icarus, Small planetesimals in a massive disk formed Mars, 225, 1, 122. doi:10.1016/j.icarus.2013.03.006

    2013 doi

  73. [81]

    Korenaga, J. & Marchi, S.\ 2023, Proceedings of the National Academy of Science, Vestiges of impact-driven three-phase mixing in the chemistry and structure of Earth's mantle, 120, 43, e2309181120. doi:10.1073/pnas.2309181120

    2023 doi

  74. [82]

    Kretke, K. A. & Lin, D. N. C.\ 2012, , The Importance of Disk Structure in Stalling Type I Migration, 755, 1, 74. doi:10.1088/0004-637X/755/1/74

    2012 doi

  75. [83]

    N., Yurimoto, H., Hutcheon, I

    Krot, A. N., Yurimoto, H., Hutcheon, I. D., et al.\ 2005, , Chronology of the early Solar System from chondrule-bearing calcium-aluminium-rich inclusions, 434, 7036, 998. doi:10.1038/nature03470

    2005 doi

  76. [84]

    Kruijer, T. S., Burkhardt, C., Budde, G., et al.\ 2017, Proceedings of the National Academy of Science, Age of Jupiter inferred from the distinct genetics and formation times of meteorites, 114, 26, 6712. doi:10.1073/pnas.1704461114

    2017 doi

  77. [85]

    K., & Inutsuka, S.\ 2020, , Dispersal of protoplanetary discs by the combination of magnetically driven and photoevaporative winds, 492, 3, 3849

    Kunitomo, M., Suzuki, T. K., & Inutsuka, S.\ 2020, , Dispersal of protoplanetary discs by the combination of magnetically driven and photoevaporative winds, 492, 3, 3849. doi:10.1093/mnras/staa087

    2020 doi

  78. [86]

    & Petit, A

    Laskar, J. & Petit, A. C.\ 2017, , AMD-stability and the classification of planetary systems, 605, A72. doi:10.1051/0004-6361/201630022

    2017 doi

  79. [87]

    F., Duncan, M

    Levison, H. F., Duncan, M. J., & Thommes, E.\ 2012, , A Lagrangian Integrator for Planetary Accretion and Dynamics (LIPAD), 144, 4, 119. doi:10.1088/0004-6256/144/4/119

    2012 doi

  80. [88]

    N., & Jacobson, S

    Liu, B., Raymond, S. N., & Jacobson, S. A.\ 2022, , Early Solar System instability triggered by dispersal of the gaseous disk, 604, 7907, 643. doi:10.1038/s41586-022-04535-1

    2022 doi

  81. [89]

    Lykawka, P. S. & Ito, T.\ 2017, , 838, 2, 106. doi:10.3847/1538-4357/aa6544

    2017 doi

  82. [90]

    J., & Canup, R

    Marchi, S., Walker, R. J., & Canup, R. M.\ 2020, Science Advances, A compositionally heterogeneous martian mantle due to late accretion, 6, 7, eaay2338. doi:10.1126/sciadv.aay2338

    2020 doi

  83. [91]

    M., Aharonson, O., & Asphaug, E.\ 2008, , Mega-impact formation of the Mars hemispheric dichotomy, 453, 7199, 1216

    Marinova, M. M., Aharonson, O., & Asphaug, E.\ 2008, , Mega-impact formation of the Mars hemispheric dichotomy, 453, 7199, 1216. doi:10.1038/nature07070

    2008 doi

  84. [92]

    & Morbidelli, A.\ 2023, , An inflationary disk phase to explain extended protoplanetary dust disks, 677, A136

    Marschall, R. & Morbidelli, A.\ 2023, , An inflationary disk phase to explain extended protoplanetary dust disks, 677, A136. doi:10.1051/0004-6361/202346616

    2023 doi

  85. [93]

    doi:10.1007/s11214-020-00649-y

    Mezger, K., Sch \"o nb \"a chler, M., & Bouvier, A.\ 2020, , Accretion of the Earth Missing Components?, 216, 2, 27. doi:10.1007/s11214-020-00649-y

    2020 doi

  86. [94]

    & Crida, A.\ 2007, Icarus, The dynamics of Jupiter and Saturn in the gaseous protoplanetary disk, 191, 1, 158

    Morbidelli, A. & Crida, A.\ 2007, Icarus, The dynamics of Jupiter and Saturn in the gaseous protoplanetary disk, 191, 1, 158. doi:10.1016/j.icarus.2007.04.001

    2007 doi

  87. [95]

    & Wood, B

    Morbidelli, A. & Wood, B. J.\ 2015, Geophysical Monograph Series, Late Accretion and the Late Veneer, 212, 71. doi:10.1002/9781118860359.ch4

    2015 doi

  88. [96]

    doi:10.1088/0004-6256/140/5/1391

    Morbidelli, A., Brasser, R., Gomes, R., et al.\ 2010, , Evidence from the Asteroid Belt for a Violent Past Evolution of Jupiter's Orbit, 140, 5, 1391. doi:10.1088/0004-6256/140/5/1391

    2010 doi

  89. [97]

    doi:10.1016/j.epsl.2020.116220

    Morbidelli, A., Libourel, G., Palme, H., et al.\ 2020, Earth and Planetary Science Letters, Subsolar Al/Si and Mg/Si ratios of non-carbonaceous chondrites reveal planetesimal formation during early condensation in the protoplanetary disk, 538, 116220. doi:10.1016/j.epsl.2020.116220

    2020

  90. [98]

    doi:10.1038/s41550-021-01517-7

    Morbidelli, A., Bailli \'e , K., Batygin, K., et al.\ 2022, Nature Astronomy, Contemporary formation of early Solar System planetesimals at two distinct radial locations, 6, 72. doi:10.1038/s41550-021-01517-7

    2022 doi

  91. [99]

    doi:10.1016/j.epsl.2024.119120

    Morbidelli, A., Kleine, T., & Nimmo, F.\ 2025, Earth and Planetary Science Letters, Did the terrestrial planets of the solar system form by pebble accretion?, 650, 119120. doi:10.1016/j.epsl.2024.119120

    2025

  92. [100]

    doi:10.1146/annurev-astro-081817-052028

    Nesvorn \'y , D.\ 2018, , Dynamical Evolution of the Early Solar System, 56, 137. doi:10.1146/annurev-astro-081817-052028

    2018 doi

  93. [101]

    doi:10.1088/2041-8205/742/2/L22

    Nesvorn \'y , D.\ 2011, , Young Solar System's Fifth Giant Planet?, 742, 2, L22. doi:10.1088/2041-8205/742/2/L22

    2011 doi

  94. [102]

    & Morbidelli, A.\ 2012 (NM12), , Statistical Study of the Early Solar System's Instability with Four, Five, and Six Giant Planets, 144, 4, 117

    Nesvorn \'y , D. & Morbidelli, A.\ 2012 (NM12), , Statistical Study of the Early Solar System's Instability with Four, Five, and Six Giant Planets, 144, 4, 117. doi:10.1088/0004-6256/144/4/117

    2012 doi

  95. [103]

    doi:10.1088/0004-637X/768/1/45

    Nesvorn \'y , D., Vokrouhlick \'y , D., & Morbidelli, A.\ 2013, , Capture of Trojans by Jumping Jupiter, 768, 1, 45. doi:10.1088/0004-637X/768/1/45

    2013 doi

  96. [104]

    F., et al.\ 2018, Nature Astronomy, Evidence for very early migration of the Solar System planets from the Patroclus-Menoetius binary Jupiter Trojan, 2, 878

    Nesvorn \'y , D., Vokrouhlick \'y , D., Bottke, W. F., et al.\ 2018, Nature Astronomy, Evidence for very early migration of the Solar System planets from the Patroclus-Menoetius binary Jupiter Trojan, 2, 878. doi:10.1038/s41550-018-0564-3

    2018 doi

  97. [105]

    N., Marschall, R., et al.\ 2020, , Superparticle Method for Simulating Collisions, 895, 1, 63

    Nesvorn \'y , D., Youdin, A. N., Marschall, R., et al.\ 2020, , Superparticle Method for Simulating Collisions, 895, 1, 63. doi:10.3847/1538-4357/ab89a1

    2020 doi

  98. [106]

    V., & Deienno, R.\ 2021, , The Role of Early Giant-planet Instability in Terrestrial Planet Formation, 161, 2, 50

    Nesvorn \'y , D., Roig, F. V., & Deienno, R.\ 2021, , The Role of Early Giant-planet Instability in Terrestrial Planet Formation, 161, 2, 50. doi:10.3847/1538-3881/abc8ef

    2021 doi

  99. [107]

    V., Vokrouhlick \'y , D., et al.\ 2023, Icarus, Early bombardment of the moon: Connecting the lunar crater record to the terrestrial planet formation, 399, 115545

    Nesvorn \'y , D., Roig, F. V., Vokrouhlick \'y , D., et al.\ 2023, Icarus, Early bombardment of the moon: Connecting the lunar crater record to the terrestrial planet formation, 399, 115545. doi:10.1016/j.icarus.2023.115545

    2023

  100. [108]

    D., Korycansky, D

    Nimmo, F., Hart, S. D., Korycansky, D. G., et al.\ 2008, , Implications of an impact origin for the martian hemispheric dichotomy, 453, 7199, 1220. doi:10.1038/nature07025

    2008 doi

  101. [109]

    doi:10.1038/s41586-024-08231-0

    Nimmo, F., Kleine, T., & Morbidelli, A.\ 2024, , Tidally driven remelting around 4.35 billion years ago indicates the Moon is old, 636, 8043, 598. doi:10.1038/s41586-024-08231-0

    2024 doi

  102. [110]

    P., Morbidelli, A., & Levison, H

    O'Brien, D. P., Morbidelli, A., & Levison, H. F.\ 2006, Icarus, Terrestrial planet formation with strong dynamical friction, 184, 1, 39. doi:10.1016/j.icarus.2006.04.005

    2006 doi

  103. [111]

    ichiro .\ 2014, , N-body Simulations of Terrestrial Planet Formation under the Influence of a Hot Jupiter, 787, 2, 172

    Ogihara, M., Kobayashi, H., & Inutsuka, S.-. ichiro .\ 2014, , N-body Simulations of Terrestrial Planet Formation under the Influence of a Hot Jupiter, 787, 2, 172. doi:10.1088/0004-637X/787/2/172

    2014 doi

  104. [112]

    K., et al.\ 2018a, , Formation of the terrestrial planets in the solar system around 1 au via radial concentration of planetesimals, 612, L5

    Ogihara, M., Kokubo, E., Suzuki, T. K., et al.\ 2018a, , Formation of the terrestrial planets in the solar system around 1 au via radial concentration of planetesimals, 612, L5. doi:10.1051/0004-6361/201832654

    doi

  105. [113]

    K., et al.\ 2018b, , Formation of close-in super-Earths in evolving protoplanetary disks due to disk winds, 615, A63

    Ogihara, M., Kokubo, E., Suzuki, T. K., et al.\ 2018b, , Formation of close-in super-Earths in evolving protoplanetary disks due to disk winds, 615, A63. doi:10.1051/0004-6361/201832720

    doi

  106. [114]

    doi:10.3847/1538-4357/ad65d5

    Ogihara, M., Morbidelli, A., & Kunitomo, M.\ 2024, , Super-Earth Formation with Slow Migration from a Ring in an Evolving Peaked Disk Compatible with Terrestrial Planet Formation, 972, 2, 181. doi:10.3847/1538-4357/ad65d5

    2024 doi

  107. [115]

    S., Mac Low, M.-M., & Menou, K.\ 2007, , Turbulent Torques on Protoplanets in a Dead Zone, 670, 1, 805

    Oishi, J. S., Mac Low, M.-M., & Menou, K.\ 2007, , Turbulent Torques on Protoplanets in a Dead Zone, 670, 1, 805. doi:10.1086/521781

    2007 doi

  108. [116]

    & Ormel, C

    Okuzumi, S. & Ormel, C. W.\ 2013, , The Fate of Planetesimals in Turbulent Disks with Dead Zones. I. The Turbulent Stirring Recipe, 771, 1, 43. doi:10.1088/0004-637X/771/1/43

    2013 doi

  109. [117]

    & Mellema, G.\ 2006, , 459, 1, L17

    Paardekooper, S.-J. & Mellema, G.\ 2006, , 459, 1, L17. doi:10.1051/0004-6361:20066304

    2006 doi

  110. [119]

    Unsaturated horseshoe drag, 401, 3, 1950

    Paardekooper, S.-J., Baruteau, C., Crida, A., et al.\ 2010, , A torque formula for non-isothermal type I planetary migration - I. Unsaturated horseshoe drag, 401, 3, 1950. doi:10.1111/j.1365-2966.2009.15782.x

    2010

  111. [120]

    Effects of diffusion, 410, 1, 293

    Paardekooper, S.-J., Baruteau, C., & Kley, W.\ 2011, , A torque formula for non-isothermal Type I planetary migration - II. Effects of diffusion, 410, 1, 293. doi:10.1111/j.1365-2966.2010.17442.x

    2011

  112. [121]

    & Stevenson, D

    Pahlevan, K. & Stevenson, D. J.\ 2007, Earth and Planetary Science Letters, Equilibration in the aftermath of the lunar-forming giant impact, 262, 3-4, 438. doi:10.1016/j.epsl.2007.07.055

    2007 doi

  113. [122]

    Papaloizou, J. C. B. & Larwood, J. D.\ 2000, , On the orbital evolution and growth of protoplanets embedded in a gaseous disc, 315, 4, 823. doi:10.1046/j.1365-8711.2000.03466.x

    2000

  114. [123]

    doi:10.1016/j.gca.2018.10.017

    Pape, J., Mezger, K., Bouvier, A.-S., et al.\ 2019, , Time and duration of chondrule formation: Constraints from ^ 26 Al- ^ 26 Mg ages of individual chondrules, 244, 416. doi:10.1016/j.gca.2018.10.017

    2019 doi

  115. [124]

    P \'e ron, S. & Mukhopadhyay, S.\ 2022, Earth and Planetary Science Letters, Pre-subduction mantle noble gas elemental pattern reveals larger missing xenon in the deep interior compared to the atmosphere, 593, 117655. doi:10.1016/j.epsl.2022.117655

    2022

  116. [125]

    C., Laskar, J., & Bou \'e , G.\ 2018, , Hill stability in the AMD framework, 617, A93

    Petit, A. C., Laskar, J., & Bou \'e , G.\ 2018, , Hill stability in the AMD framework, 617, A93. doi:10.1051/0004-6361/201833088

    2018 doi

  117. [126]

    doi:10.1016/j.icarus.2023.115427

    Piralla, M., Villeneuve, J., Schnuriger, N., et al.\ 2023, Icarus, A unified chronology of dust formation in the early solar system, 394, 115427. doi:10.1016/j.icarus.2023.115427

    2023

  118. [127]

    Poirier, J.-P.\ 2000, Introduction to the Physics of the Earth's Interior, 326

    2000

  119. [128]

    doi:10.1111/j.1745-3933.2012.01337.x

    Rein, H.\ 2012, , Period ratios in multiplanetary systems discovered by Kepler are consistent with planet migration, 427, 1, L21. doi:10.1111/j.1745-3933.2012.01337.x

    2012

  120. [129]

    & Papaloizou, J

    Rein, H. & Papaloizou, J. C. B.\ 2009, , On the evolution of mean motion resonances through stochastic forcing: fast and slow libration modes and the origin of HD 128311, 497, 2, 595. doi:10.1051/0004-6361/200811330

    2009 doi

  121. [130]

    & Choksi, N.\ 2022, Research Notes of the American Astronomical Society, An Implementation of Stochastic Forces for the N-body Code REBOUND, 6, 5, 95

    Rein, H. & Choksi, N.\ 2022, Research Notes of the American Astronomical Society, An Implementation of Stochastic Forces for the N-body Code REBOUND, 6, 5, 95. doi:10.3847/2515-5172/ac6e41

    2022 doi

  122. [131]

    & Nesvorn \'y , D.\ 2015, , The Evolution of Asteroids in the Jumping-Jupiter Migration Model, 150, 6, 186

    Roig, F. & Nesvorn \'y , D.\ 2015, , The Evolution of Asteroids in the Jumping-Jupiter Migration Model, 150, 6, 186. doi:10.1088/0004-6256/150/6/186

    2015 doi

  123. [132]

    R.\ 2016, , Jumping Jupiter Can Explain Mercury s Orbit, 820, 2, L30

    Roig, F., Nesvorn \'y , D., & DeSouza, S. R.\ 2016, , Jumping Jupiter Can Explain Mercury s Orbit, 820, 2, L30. doi:10.3847/2041-8205/820/2/L30

    2016 doi

  124. [133]

    doi:10.1093/mnras/stab2874

    Roig, F., Nesvorn \'y , D., Deienno, R., et al.\ 2021, , ISYMBA: a symplectic massive nbodies integrator with planets interpolation, 508, 4, 4858. doi:10.1093/mnras/stab2874

    2021 doi

  125. [134]

    C., Frost, D

    Rubie, D. C., Frost, D. J., Mann, U., et al.\ 2011, Earth and Planetary Science Letters, Heterogeneous accretion, composition and core-mantle differentiation of the Earth, 301, 1-2, 31. doi:10.1016/j.epsl.2010.11.030

    2011 doi

  126. [135]

    C., Laurenz, V., Jacobson, S

    Rubie, D. C., Laurenz, V., Jacobson, S. A., et al.\ 2016, Science, Highly siderophile elements were stripped from Earth s mantle by iron sulfide segregation, 353, 6304, 1141. doi:10.1126/science.aaf6919

    2016 doi

  127. [136]

    doi:10.3847/1538-4357/ad39e6

    Scora, J., Valencia, D., Morbidelli, A., et al.\ 2024, , Forming Mercury from Excited Initial Conditions, 967, 1, 1. doi:10.3847/1538-4357/ad39e6

    2024 doi

  128. [137]

    Scott, E. R. D. & Krot, A. N.\ 2014, Meteorites and Cosmochemical Processes, Chondrites and Their Components, 1, 65

    2014

  129. [138]

    Shakura, N. I. & Sunyaev, R. A.\ 1973, , Black holes in binary systems. Observational appearance., 24, 337

    1973

  130. [139]

    doi:10.1016/j.epsl.2021.117211

    Spitzer, F., Burkhardt, C., Nimmo, F., et al.\ 2021, Earth and Planetary Science Letters, Nucleosynthetic Pt isotope anomalies and the Hf-W chronology of core formation in inner and outer solar system planetesimals, 576, 117211. doi:10.1016/j.epsl.2021.117211

    2021

  131. [140]

    Stewart, S. T. & \'C uk, M.\ 2012, DPS, A New Model for the Origin of the Moon, 44, 503.04

    2012

  132. [141]

    K., Ogihara, M., Morbidelli, A., et al.\ 2016, , Evolution of protoplanetary discs with magnetically driven disc winds, 596, A74

    Suzuki, T. K., Ogihara, M., Morbidelli, A., et al.\ 2016, , Evolution of protoplanetary discs with magnetically driven disc winds, 596, A74. doi:10.1051/0004-6361/201628955

    2016 doi

  133. [142]

    & Dauphas, N.\ 2012, Earth and Planetary Science Letters, Abundance, distribution, and origin of ^ 60 Fe in the solar protoplanetary disk, 359, 248

    Tang, H. & Dauphas, N.\ 2012, Earth and Planetary Science Letters, Abundance, distribution, and origin of ^ 60 Fe in the solar protoplanetary disk, 359, 248. doi:10.1016/j.epsl.2012.10.011

    2012 doi

  134. [143]

    Thiemens, M., Sprung, P., Fonseca, R., et al.\ 2018, European Planetary Science Congress, Hf/W insights into the primeval Moon, EPSC2018-968

    2018

  135. [144]

    doi:10.1038/nature03539

    Tsiganis, K., Gomes, R., Morbidelli, A., et al.\ 2005, , Origin of the orbital architecture of the giant planets of the Solar System, 435, 7041, 459. doi:10.1038/nature03539

    2005 doi

  136. [145]

    Turekian, K. K. & Clark, S. P.\ 1969, Earth and Planetary Science Letters, Inhomogeneous accumulation of the earth from the primitive solar nebula, 6, 5, 346. doi:10.1016/0012-821X(69)90183-6

    1969 doi

  137. [146]

    J., Morbidelli, A., Raymond, S

    Walsh, K. J., Morbidelli, A., Raymond, S. N., et al.\ 2011, , A low mass for Mars from Jupiter's early gas-driven migration, 475, 7355, 206. doi:10.1038/nature10201

    2011 doi

  138. [147]

    Walsh, K. J. & Levison, H. F.\ 2016, , Terrestrial Planet Formation from an Annulus, 152, 3, 68. doi:10.3847/0004-6256/152/3/68

    2016 doi

  139. [148]

    D., Harris, A

    Warner, B. D., Harris, A. W., Vokrouhlick \'y , D., et al.\ 2009, Icarus, Analysis of the Hungaria asteroid population, 204, 1, 172. doi:10.1016/j.icarus.2009.06.004

    2009 doi

  140. [149]

    Warren, P. H.\ 2011, Earth and Planetary Science Letters, Stable-isotopic anomalies and the accretionary assemblage of the Earth and Mars: A subordinate role for carbonaceous chondrites, 311, 1, 93. doi:10.1016/j.epsl.2011.08.047

    2011 doi

  141. [150]

    J.\ 1977, , The Distribution of Mass in the Planetary System and Solar Nebula, 51, 1, 153

    Weidenschilling, S. J.\ 1977, , The Distribution of Mass in the Planetary System and Solar Nebula, 51, 1, 153. doi:10.1007/BF00642464

    1977 doi

  142. [151]

    P., Bai, X.-N., & Fu, R

    Weiss, B. P., Bai, X.-N., & Fu, R. R.\ 2021, Science Advances, History of the solar nebula from meteorite paleomagnetism, 7, 1, eaba5967. doi:10.1126/sciadv.aba5967

    2021 doi

  143. [152]

    Williams, J. P. & Cieza, L. A.\ 2011, , Protoplanetary Disks and Their Evolution, 49, 1, 67. doi:10.1146/annurev-astro-081710-102548

    2011 doi

  144. [153]

    & Holman, M.\ 1991, , Symplectic maps for the N-body problem., 102, 1528

    Wisdom, J. & Holman, M.\ 1991, , Symplectic maps for the N-body problem., 102, 1528. doi:10.1086/115978

    1991 doi

  145. [154]

    Woo, J. M. Y., Morbidelli, A., Grimm, S. L., et al.\ 2023, Icarus, Terrestrial planet formation from a ring, 396, 115497. doi:10.1016/j.icarus.2023.115497

    2023

  146. [155]

    Woo, J. M. Y., Nesvorn \'y , D., Scora, J., et al.\ 2024, Icarus, Terrestrial planet formation from a ring: Long-term simulations accounting for the giant planet instability, 417, 116109. doi:10.1016/j.icarus.2024.116109

    2024

  147. [156]

    @esa ( ) , n @biblabelnum##1 ##1

    \@ifclassloaded aguplus natbib The aguplus class already includes natbib coding, so you should not add it explicitly Type <Return> for now, but then later remove the command natbib from the document \@ifclassloaded nlinproc natbib The nlinproc class already includes natbib cod...

  148. [157]

    @stdbsttrue NAT@ctr \@lbibitem[ NAT@ctr ] \@lbibitem[#1]#2 \@extra@b@citeb \@ifundefined br@#2\@extra@b@citeb \@namedef br@#2 \@nameuse br@#2\@extra@b@citeb \@ifundefined b@#2\@extra@b@citeb @num @parse #2 [ @natanchorstart #2\@extra@b@citeb \@biblabel @num @natanchorend] @ifc...

  149. [158]

    @open @close @open @close and [1] URL: #1 \@ifundefined chapter * \@mkboth \@ifundefined NAT@sectionbib * \@mkboth * \@mkboth\@gobbletwo \@ifclassloaded amsart * \@ifclassloaded amsbook * \@ifundefined bib@heading @heading NAT@ctr thebibliography [1] @ \@biblabel NAT@ctr \@bib...

Pith tools

Reviewed August 6, 2026 · model on record in the stance chip above.