| Full text | |
| Author(s): |
Ribeiro, Rafael de Sousa
[1, 2]
;
Morbidelli, Alessandro
[2]
;
Raymond, Sean N.
[3]
;
Izidoro, Andre
[1]
;
Gomes, Rodney
[4]
;
Vieira Neto, Ernesto
[1]
Total Authors: 6
|
| Affiliation: | [1] Sao Paulo State Univ, UNESP, Campus Guaratingueta, BR-12516410 Guaratingueta, SP - Brazil
[2] Univ Cote Azur, Observ Cote Azur, CNRS, Lab Lagrange, UMR7293, Blvd Observ, F-06304 Nice 4 - France
[3] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, B18N Geoffroy St Hilaire, F-33615 Pessac - France
[4] Observ Nacl, Rua Gen Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ - Brazil
Total Affiliations: 4
|
| Document type: | Journal article |
| Source: | ICARUS; v. 339, MAR 15 2020. |
| Web of Science Citations: | 0 |
| Abstract | |
The dynamical structure of the Solar System can be explained by a period of orbital instability experienced by the giant planets. While a late instability was originally proposed to explain the Late Heavy Bombardment, recent work favors an early instability. Here we model the early dynamical evolution of the outer Solar System to self-consistently constrain the most likely timing of the instability. We first simulate the dynamical sculpting of the primordial outer planetesimal disk during the accretion of Uranus and Neptune from migrating planetary embryos during the gas disk phase, and determine the separation between Neptune and the inner edge of the planetesimal disk. We performed simulations with a range of (inward and outward) migration histories for Jupiter. We find that, unless Jupiter migrated inwards by 10 AU or more, the instability almost certainly happened within 100 Myr of the start of Solar System formation. There are two distinct possible instability triggers. The first is an instability that is triggered by the planets themselves, with no appreciable influence from the planetesimal disk. About half of the planetary systems that we consider have a self-triggered instability. Of those, the median instability time is similar to 4Myr. Among self-stable systems - where the planets are locked in a resonant chain that remains stable in the absence of a planetesimal's disk- our self-consistently sculpted planetesimal disks nonetheless trigger a giant planet instability with a median instability time of 37-62 Myr for a reasonable range of migration histories of Jupiter. The simulations that give the latest instability times are those that invoked long-range inward migration of Jupiter from 15 AU or beyond; however these simulations over-excited the inclinations of Kuiper belt objects and are inconsistent with the present-day Solar System. We conclude on dynamical grounds that the giant planet instability is likely to have occurred early in Solar System history. (AU) | |
| FAPESP's process: | 16/24561-0 - On the relevance of small bodies in orbital dynamics |
| Grantee: | Othon Cabo Winter |
| Support Opportunities: | Research Projects - Thematic Grants |
| FAPESP's process: | 15/15588-9 - The stability of the solar system dynamical evolution via Nice Model |
| Grantee: | Rafael Ribeiro de Sousa |
| Support Opportunities: | Scholarships in Brazil - Doctorate |
| FAPESP's process: | 16/19556-7 - Planetary Formation and Dynamics: from the Solar System to Exoplanets |
| Grantee: | André Izidoro Ferreira da Costa |
| Support Opportunities: | Scholarships in Brazil - Young Researchers |
| FAPESP's process: | 17/09919-8 - A study of the self-gravitating planetesimal disk on Nice Model and the dynamical formation of the Kuiper Belt |
| Grantee: | Rafael Ribeiro de Sousa |
| Support Opportunities: | Scholarships abroad - Research Internship - Doctorate |
| FAPESP's process: | 16/12686-2 - Planetary formation and dynamics: from the Solar System to exoplanets |
| Grantee: | André Izidoro Ferreira da Costa |
| Support Opportunities: | Research Grants - Young Investigators Grants |