What Can Meteorites Tell Us About the Formation of Jupiter?

Weiss, B. P.; Bottke, W. F.

doi:10.1029/2020av000376

Cited by 7 publications

(4 citation statements)

References 73 publications

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“…Our best-fit runs indicate that the giant planet instability probably occurred ∼20-30 Myr after the dissipation of the solar nebula, which in turn probably occurred a few megayears after CAIs (e.g., Weiss & Bottke 2021). This interval gives time for the PKB to experience some collisional evolution, but not so much to greatly steepen in the slope of 1 < D < 10 km bodies.…”

Section: Discussionmentioning

confidence: 74%

“…Stage 1 starts shortly after the giant planets form on nearly circular and coplanar orbits within the solar nebula. The likely time of solar nebular dispersion is 2-10 Myr after calciumaluminum-rich inclusion (CAI) formation (Kruijer et al 2017;Weiss & Bottke 2021). Gas-driven migration likely caused the giant planets to evolve into a resonant chain (i.e., the planets were trapped in mutual mean motion resonances with one another), but the stability of chains may have been limited after the gas disk went away (see review by Nesvorný 2018).…”

Section: Stage 1 Before the Giant Planet Instabilitymentioning

confidence: 99%

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The Collisional Evolution of the Primordial Kuiper Belt, Its Destabilized Population, and the Trojan Asteroids

Bottke,

Vokrouhlický,

Marschall

et al. 2023

Planet. Sci. J.

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The tumultuous early era of outer solar system evolution culminated when Neptune migrated across the primordial Kuiper Belt (PKB) and triggered a dynamical instability among the giant planets. This event led to the ejection of ∼99.9% of the PKB (here called the destabilized population), heavy bombardment of the giant planet satellites, and the capture of Jupiter’s Trojans. While this scenario has been widely tested using dynamical models, there have been fewer investigations into how the PKB, its destabilized population, and the Trojans experienced collisional evolution. Here we examined this issue for all three populations with the code Boulder. Our constraints included the size–frequency distributions (SFDs) of the Trojan asteroids and craters on the giant planet satellites. Using this combination, we solved for the unknown disruption law affecting bodies in these populations. The weakest ones, from an impact energy per mass perspective, were diameter D ∼ 20 m. Overall, collisional evolution produces a power-law-like shape for multikilometer Trojans and a wavy-shaped SFD in the PKB and destabilized populations. The latter can explain (i) the shapes of the ancient and younger crater SFDs observed on the giant planet satellites, (ii) the shapes of the Jupiter family and long-period comet SFDs, which experienced different degrees of collision evolution, and (iii) the present-day impact frequency of superbolides on Jupiter and smaller projectiles on Saturn’s rings. Our model results also indicate that many observed comets, the majority which are D < 10 km, are likely to be gravitational aggregates formed by large-scale collision events.

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Section: Discussionmentioning

confidence: 74%

Section: Stage 1 Before the Giant Planet Instabilitymentioning

confidence: 99%

The Collisional Evolution of the Primordial Kuiper Belt, Its Destabilized Population, and the Trojan Asteroids

Bottke,

Vokrouhlický,

Marschall

et al. 2023

Planet. Sci. J.

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“…Finally, the dissipation of the disk sets the limit for the accretion of gas to the gas giants (Weiss & Bottke, 2021). Thus, if we take the age of the CVs as the first evidence for the dissipation of the solar nebula in the outer solar system, that indicates that the gas giants stopped accreting mass sometime between 3.5 and 5 Myr after CAI formation.…”

Section: Solar Nebular Magnetic Fields and Implications For The Dissi...mentioning

confidence: 99%

Lifetime of the Outer Solar System Nebula From Carbonaceous Chondrites

et al. 2022

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The lifetimes of protoplanetary disks (PPDs) have important implications for the formation of planetary systems that emerge from them. Determining the lifetime of PPDs (i.e., the dissipation of the gas) constrains the formation time of gas giants and when gas-driven planetary migration can occur. The lifetimes of PPDs have been measured astronomically through observations of dust infrared spectral energy distributions (SEDs) (Haisch et al., 2001;Hernández et al., 2007). SED observations have provided evidence that disks pass through different stages during their evolution from that of protostars to transition disks (disks that have low or no near-infrared excess and high mid-to far-infrared excess) and to debris disks (no remaining gas) (Ercolano & Pascucci, 2017;Owen, 2016). With the exception of a few observed PPDs that are likely in the transition phase, the majority (∼90%) of observed PPDs are either in the PPD phase with a protostar or completely dissipated (Owen, 2016). This observation has been interpreted to suggest that PPDs have a two time-scale evolution during their lifetime: during

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“…These subsequent collisions occurred at a rapid pace in the first few million years of the solar system, and then more slowly as populations waned and the oligarchic stage of planetary formation commenced (Chambers 2008 ). The gas disk had likely locally dispersed between and after CAI-formation in the noncarbonaceous reservoir, and between and in the carbonaceous reservoir (95% confidence limits) (Weiss and Bottke 2021 ).…”

Section: The Fiducial Origin Scenario: a Differentiated Parent Body F...mentioning

confidence: 99%

Distinguishing the Origin of Asteroid (16) Psyche

et al. 2022

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The asteroid (16) Psyche may be the metal-rich remnant of a differentiated planetesimal, or it may be a highly reduced, metal-rich asteroidal material that never differentiated. The NASA Psyche mission aims to determine Psyche’s provenance. Here we describe the possible solar system regions of origin for Psyche, prior to its likely implantation into the asteroid belt, the physical and chemical processes that can enrich metal in an asteroid, and possible meteoritic analogs. The spacecraft payload is designed to be able to discriminate among possible formation theories. The project will determine Psyche’s origin and formation by measuring any strong remanent magnetic fields, which would imply it was the core of a differentiated body; the scale of metal to silicate mixing will be determined by both the neutron spectrometers and the filtered images; the degree of disruption between metal and rock may be determined by the correlation of gravity with composition; some mineralogy (e.g., modeled silicate/metal ratio, and inferred existence of low-calcium pyroxene or olivine, for example) will be detected using filtered images; and the nickel content of Psyche’s metal phase will be measured using the GRNS.

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What Can Meteorites Tell Us About the Formation of Jupiter?

Cited by 7 publications

References 73 publications

The Collisional Evolution of the Primordial Kuiper Belt, Its Destabilized Population, and the Trojan Asteroids

The Collisional Evolution of the Primordial Kuiper Belt, Its Destabilized Population, and the Trojan Asteroids

Lifetime of the Outer Solar System Nebula From Carbonaceous Chondrites

Distinguishing the Origin of Asteroid (16) Psyche

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