| Full text | |
| Author(s): |
Deienno, Rogerio
[1]
;
Gomes, Rodney S.
[2]
;
Walsh, Kevin J.
[3]
;
Morbidelli, Alessandro
[4]
;
Nesvorny, David
[3]
Total Authors: 5
|
| Affiliation: | [1] Inst Nacl Pesquisas Espaciais, Ave Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP - Brazil
[2] Observ Nacl, Rua Gen Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ - Brazil
[3] Southwest Space Res Inst, Dept Space Studies, 1050 Walnut St, Boulder, CO 80302 - USA
[4] Univ Cote Azur, Lab Lagrange, CNRS, UMR7293, Observ Cote Azur, Blvd Observ, F-06304 Nice 4 - France
Total Affiliations: 4
|
| Document type: | Journal article |
| Source: | ICARUS; v. 272, p. 114-124, JUL 1 2016. |
| Web of Science Citations: | 17 |
| Abstract | |
The Asteroid Belt is characterized by the radial mixing of bodies with different physical properties, a very low mass compared to Minimum Mass Solar Nebula expectations and has an excited orbital distribution, with eccentricities and inclinations covering the entire range of values allowed by the constraints of dynamical stability. Models of the evolution of the Asteroid Belt show that the origin of its structure is strongly linked to the process of terrestrial planet formation. The Grand Tack model presents a possible solution to the conundrum of reconciling the small mass of Mars with the properties of the Asteroid Belt, including the mass depletion, radial mixing and orbital excitation. However, while the inclination distribution produced in the Grand Tack model is in good agreement with the one observed, the eccentricity distribution is skewed towards values larger than those found today. Here, we evaluate the evolution of the orbital properties of the Asteroid Belt from the end of the Grand Tack model (at the end of the gas nebula phase when planets emerge from the dispersing gas disk), throughout the subsequent evolution of the Solar System including an instability of the Giant Planets approximately 400 Myr later. Before the instability, the terrestrial planets were modeled on dynamically cold orbits with Jupiter and Saturn locked in a 3:2 mean motion resonance. The model continues for an additional 4.1 Gyr after the giant planet instability. Our results show that the eccentricity distribution obtained in the Grand Tack model evolves towards one very similar to that currently observed, and the semimajor axis distribution does the same. The inclination distribution remains nearly unchanged with a slight preference for depletion at low inclination; this leads to the conclusion that the inclination distribution at the end of the Grand Tack is a bit over-excited. Also, we constrain the primordial eccentricities of Jupiter and Saturn, which have a major influence on the dynamical evolution of the Asteroid Belt and its final orbital structure. (C) 2016 Elsevier Inc. All rights reserved. (AU) | |
| FAPESP's process: | 15/18682-6 - Late instability in the solar system |
| Grantee: | Rogerio Deienno |
| Support Opportunities: | Scholarships abroad - Research Internship - Post-doctor |
| FAPESP's process: | 14/02013-5 - Orbital evolution of the asteroids in the first 700 MY of the solar system |
| Grantee: | Rogerio Deienno |
| Support Opportunities: | Scholarships in Brazil - Post-Doctoral |