Dynamical origin of the Dwarf Planet Ceres

Sousa, Rafael Ribeiro de; Morbidelli, Alessandro; Gomes, R. S.; Neto, E. Vieira; Izidoro, André; Alves, Abreuçon Atanasio

doi:10.1016/j.icarus.2022.114933

Cited by 9 publications

(9 citation statements)

References 56 publications

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“…Lastly, we should point out that our analysis relies on the fact that absolutely no mass existed in the MAB before implantation (Raymond & Izidoro 2017b;Izidoro et al 2021b). We are also not accounting for additional implantation from planetesimals originally beyond Jupiter, e.g., the Jupiter-Saturn zone (Raymond & Izidoro 2017a) or farther out (Ribeiro de Sousa et al 2022). Therefore, the values reported in Figure 3 should be interpreted as an upper limit on mass implantation.…”

Section: Modelmentioning

confidence: 99%

Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System

Deienno¹,

Izidoro²,

Morbidelli³

et al. 2022

ApJL

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The migration history of Jupiter in the Sun’s natal disk remains poorly constrained. Here we consider how Jupiter’s migration affects small-body reservoirs and how this constrains its original orbital distance from the Sun. We study the implications of large-scale and inward radial migration of Jupiter for the inner solar system while considering the effects of collisional evolution of planetesimals. We use analytical prescriptions to simulate the growth and migration of Jupiter in the gas disk. We assume the existence of a planetesimal disk inside Jupiter’s initial orbit. This planetesimal disk received an initial total mass and size–frequency distribution (SFD). Planetesimals feel the effects of aerodynamic gas drag and collide with one another, mostly while shepherded by the migrating Jupiter. Our main goal is to measure the amount of mass in planetesimals implanted into the main asteroid belt (MAB) and the SFD of the implanted population. We also monitor the amount of dust produced during planetesimal collisions. We find that the SFD of the planetesimal population implanted into the MAB tends to resemble that of the original planetesimal population interior to Jupiter. We also find that unless very little or no mass existed between 5 au and Jupiter’s original orbit, it would be difficult to reconcile the current low mass of the MAB with the possibility that Jupiter migrated from distances beyond 15 au. This is because the fraction of the original disk mass that gets implanted into the MAB is very large. Finally, we discuss the implications of our results in terms of dust production to the so-called NC–CC isotopic dichotomy.

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Section: Modelmentioning

confidence: 99%

Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System

Deienno¹,

Izidoro²,

Morbidelli³

et al. 2022

ApJL

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“…3. The ice giants' accretion -from the inward migration and collisional growth of a population of ~5 Earth-mass cores (21) -scattered planetesimals inward, implanting a fraction in the asteroid belt due to gas drag (22).…”

Section: Ceres-like Asteroids' Thermal Evolutionmentioning

confidence: 99%

“…Accounting for the gas giants' migration and the ice giants' growth, the source region of dark asteroids would have extended from a few to ~20 AU, yet with a strong preference for objects originating between ~5 and 10 AU (18,20,28). The ice giants' growth implanted planetesimals from ~10 AU to at least 20-30 AU (22). Finally, the dynamical instability implanted planetesimals that accreted at ~20-40 AU (25).…”

Section: Ceres-like Asteroids' Thermal Evolutionmentioning

confidence: 99%

“…Gas-driven capture (mechanisms 1, 2, and 3) produces a broader distribution of implanted asteroids in which it is statistically unlikely not to have captured any objects interior to Ceres' present-day orbit (18,19,22). For both mechanisms 1 and 3, the peak in the distribution of implanted Ceres-sized planetesimals is close to Ceres' actual orbit (18,22). However, suppose we assume that Ceres and the large dark asteroids are part of the same population and that no large dark asteroids exist closer to the Sun than Ceres.…”

Section: Ceres-like Asteroids' Thermal Evolutionmentioning

confidence: 99%

“…The migration of the gas-and ice giants caused the source region of implanted planetesimals to expand outward (18,19). The ice giants' growth implanted additional planetesimals (22). The giant planet's instability then implanted some asteroids from the outer planetesimal disk (25,26) -this is the likely source of the large dark asteroids.…”

Section: Ceres-like Asteroids' Thermal Evolutionmentioning

confidence: 99%

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Late accretion of Ceres-like asteroids and their implantation into the outer main belt

et al. 2023

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Surface Compositions of Trojan Asteroids

Emery,

Binzel,

Britt

et al. 2024

Space Sci Rev

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The Jupiter Trojan asteroids are a key population for understanding the chemical and dynamical evolution of the Solar System. Surface compositions of Trojans, in turn, provide crucial information for reconstructing their histories. NASA’s Lucy mission will soon complete the first spacecraft reconnaissance of this population. This review summarizes the current state of knowledge of Trojan surface compositions and looks ahead to expected advances in that knowledge from Lucy. Surface compositions of Trojans remain uncertain due to a relative lack of diagnostic absorption features, though dedicated observations have begun to provide some clues to compositions. Trojans have uniformly low albedos, with a population average of ∼5.3%, and red spectral slopes at ultraviolet, visible, and near-infrared wavelengths. A bimodality of spectral slopes has been detected and confirmed across all these wavelengths, and the ratio of “less-red” to “red” Trojans increases with decreasing size. A broad absorption at ∼3.1 μm in some less-red Trojans may indicate the presence of N-H bearing material. Mid-infrared emissivity spectra reveal the presence of fine-grained anhydrous silicates on the surfaces. The meteorite collection contains no identifiable analogs to Trojan asteroids. Among small body populations, some Main Belt asteroids, comets, irregular satellites, and Centaurs provide reasonable spectral matches, supporting some genetic relationships among some members of these groups. The cause of the observed spectral properties remains uncertain, but recent suggestions include a combination of volatile ice sublimation and space weathering or a combination of impact gardening and space weathering. The Lucy mission will provide detailed compositional analysis of (3548) Eurybates, (15094) Polymele, (11351) Leucus, (21900) Orus, and (617) Patroclus-Menoetius, a suite of targets that sample the diversity among the Trojan population along several dimensions. With these flybys, the Lucy mission is poised to resolve many of the outstanding questions regarding Trojan surface compositions, thereby revealing how the Trojans formed and evolved and providing a clearer view of Solar System history.

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Dynamical origin of the Dwarf Planet Ceres

Cited by 9 publications

References 56 publications

Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System

Implications of Jupiter Inward Gas-driven Migration for the Inner Solar System

Late accretion of Ceres-like asteroids and their implantation into the outer main belt

Surface Compositions of Trojan Asteroids

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