Coagulation Calculations of Icy Planet Formation at 15-150 Au: A Correlation Between the Maximum Radius and the Slope of the Size Distribution for Trans-Neptunian Objects

Kenyon, Scott J.; Bromley, Benjamin C.

doi:10.1088/0004-6256/143/3/63

Cited by 60 publications

(25 citation statements)

References 133 publications

(222 reference statements)

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“…In this case, the mass distribution of KBOs is a superposition of those from different regions. Such a scenario was examined by Kenyon and Bromley (2012). Their results still imply that the steep slope and the bump at 10 21 g are difficult to be reproduced if m 0 is lower than m 0,crit (see their Fig.…”

Section: Kuiper Beltmentioning

confidence: 95%

Onset of oligarchic growth and implication for accretion histories of dwarf planets

Morishima

2017

Icarus

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We investigate planetary accretion that starts from equal-mass planetesimals using an analytic theory and numerical simulations. We particularly focus on how the planetary mass M oli at the onset of oligarchic growth depends on the initial mass m 0 of a planetesimal. Oligarchic growth commences when the velocity dispersion relative to the Hill velocity of the protoplanet takes its minimum. We find that if m 0 is small enough, this normalized velocity dispersion becomes as low as unity during the intermediate stage between the runaway and oligarchic growth stages. In this case, M oli is independent of m 0 . If m 0 is large, on the other hand, oligarchic growth commences directly after runaway growth, and M oli ∝ m 3/7 0 . The planetary mass M oli for the solid surface density of the Minimum Mass Solar Nebula is close to the masses of the dwarf planets in a reasonable range of m 0 . This indicates that they are likely to be the largest remnant planetesimals that failed to become planets. The power-law exponent q of the differential mass distribution of remnant planetesimals is typically −2.0 and −2.7 to −2.5 for small and large m 0 . The slope, q ≃ −2.7, and the bump at 10 21 g (or 50 km in radius) for the mass distribution of hot Kuiper belt objects are reproduced if m 0 is the bump mass. On the other hand, small initial planetesimals with m 0 ∼ 10 13 g or less are favored to explain the slope of large asteroids, q ≃ −2.0, while the bump at 10 21 g can be reproduced by introducing a small number of asteroid seeds each with mass of 10 19 g.

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Section: Kuiper Beltmentioning

confidence: 95%

Onset of oligarchic growth and implication for accretion histories of dwarf planets

Morishima

2017

Icarus

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“…Relatively little work has been done on collisional coagulation since (e.g. Schlichting and Sari, 2011;Kenyon and Bromley, 2012;Schlichting et al, 2013;Shannon et al 2016).…”

Section: Accretion Of Kbosmentioning

confidence: 99%

Kuiper belt: Formation and evolution

Morbidelli

Nesvorný

2020

The Trans-Neptunian Solar System

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This chapter reviews accretion models for Kuiper belt objects (KBOs), discussing in particular the compatibility of the observed properties of the KBO population with the streaming instability paradigm. Then it discusses how the dynamical structure of the KBO population, including the formation of its 5 subcomponents (cold, hot, resonant, scattered and fossilized), can be quantitatively understood in the framewok of the giant planet instability. We also establish the connections between the KBO population and the Trojans of Jupiter and Neptune, the irregular satellites of all giant planets, the Oort cloud and the Dtype main belt asteroids. Finally, we discuss the collisional evolution of the KBO population, arguing that the current size-frequency distribution below 100 km in size has been achieved as a collisional equilibrium in a few tens of My inside the original massive trans-Neptunain disk, possibly with the exception of the cold population sub-component.

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“…X 0 is the initial (anhydrous rock) mass fraction. Short-lived radionuclides can be neglected, since the accretion time of Charon is expected to be much longer than in the inner solar system (Kenyon & Bromley 2012), on the order of tens of Myr. ̺ u 3.5 + 2.15 · 10 −12 P g cm −3 Rock specific density (p) ̺ p 2.9 + 3.41 · 10 −12 P g cm −3 Water thermal conductivity K ℓ 5.5 · 10 4 erg cm −1 s −1 K −1 Ice thermal conductivity (c) K c 5.67 · 10 7 /T erg cm −1 s −1 K −1 Ice thermal conductivity (a) K a 2.348 · 10 2 T + 2.82 · 10 3 erg cm −1 s −1 K −1 Rock thermal conductivity (u) (2015).…”

Section: Model Configuration and Parametersmentioning

confidence: 99%

The contraction/expansion history of Charon with implications for its planetary-scale tectonic belt

Malamud

Perets

Schubert

2017

Monthly Notices of the Royal Astronomical Society

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The New Horizons mission to the Kuiper Belt has recently revealed intriguing features on the surface of Charon, including a network of chasmata, cutting across or around a series of high topography features, conjoining to form a belt. It is proposed that this tectonic belt is a consequence of contraction/expansion episodes in the moon's evolution associated particularly with compaction, differentiation and geochemical reactions of the interior. The proposed scenario involves no need for solidification of a vast subsurface ocean and/or a warm initial state. This scenario is based on a new, detailed thermo-physical evolution model of Charon that includes multiple processes. According to the model, Charon experiences two contraction/expansion episodes in its history that may provide the proper environment for the formation of the tectonic belt. This outcome remains qualitatively the same, for several different initial conditions and parameter variations. The precise orientation of Charon's tectonic belt, and the cryovolcanic features observed south of the tectonic belt may have involved a planetary-scale impact, that occurred only after the belt had already formed.

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Coagulation Calculations of Icy Planet Formation at 15-150 Au: A Correlation Between the Maximum Radius and the Slope of the Size Distribution for Trans-Neptunian Objects

Cited by 60 publications

References 133 publications

Onset of oligarchic growth and implication for accretion histories of dwarf planets

Onset of oligarchic growth and implication for accretion histories of dwarf planets

Kuiper belt: Formation and evolution

The contraction/expansion history of Charon with implications for its planetary-scale tectonic belt

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