Dynamical origin of the Dwarf Planet Ceres

@article{RibeirodeSousa2022DynamicalOO,
  title={Dynamical origin of the Dwarf Planet Ceres},
  author={Rafael Ribeiro de Sousa and Alessandro Morbidelli and Rodney Gomes and Ernesto Vieira Neto and Andr{\'e} Izidoro and A. A. Alves},
  journal={Icarus},
  year={2022}
}

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

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

References

SHOWING 1-10 OF 44 REFERENCES

CAPTURE OF TRANS-NEPTUNIAN PLANETESIMALS IN THE MAIN ASTEROID BELT

The orbital evolution of the giant planets after nebular gas was eliminated from the Solar System but before the planets reached their final configuration was driven by interactions with a vast sea

LATE ORBITAL INSTABILITIES IN THE OUTER PLANETS INDUCED BY INTERACTION WITH A SELF-GRAVITATING PLANETESIMAL DISK

We revisit the issue of the cause of the dynamical instability during the so-called Nice model, which describes the early dynamical evolution of the giant planets. In particular, we address the

Modeling the Historical Flux of Planetary Impactors

The impact cratering record of the Moon and the terrestrial planets provides important clues about the formation and evolution of the solar system. Especially intriguing is the epoch ≃3.8–3.9 Gyr ago

STATISTICAL STUDY OF THE EARLY SOLAR SYSTEM'S INSTABILITY WITH FOUR, FIVE, AND SIX GIANT PLANETS

Several properties of the solar system, including the wide radial spacing and orbital eccentricities of giant planets, can be explained if the early solar system evolved through a dynamical

Differentiation of the asteroid Ceres as revealed by its shape

C Ceres has a shape and smoothness indicative of a gravitationally relaxed object that is significantly less flattened than that expected for a homogeneous object, but is consistent with a central mass concentration indicative of differentiation.

Origin of the orbital architecture of the giant planets of the Solar System

This model reproduces all the important characteristics of the giant planets' orbits, namely their final semimajor axes, eccentricities and mutual inclinations, provided that Jupiter and Saturn crossed their 1:2 orbital resonance.

The empty primordial asteroid belt

It is shown that the present-day asteroid belt is consistent with having formed empty, without any planetesimals between Mars and Jupiter’s present- day orbits.

Instabilities in the Early Solar System Due to a Self-gravitating Disk

These simulations indicate that the self-stirring of the primordial Kuiper belt is very important to the dynamics of the giant planet instability, and interactions between planetesimals dynamically heat the disk and typically prevent the outer solar system instability from being delayed by more than a few tens of million years after giant planet formation.