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(Reference retrieved automatically from Web of Science through information on FAPESP grant and its corresponding number as mentioned in the publication by the authors.)

Excitation of a Primordial Cold Asteroid Belt as an Outcome of Planetary Instability

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Author(s):
Deienno, Rogerio [1, 2] ; Izidoro, Andre [3] ; Morbidelli, Alessandro [4] ; Gomes, Rodney S. [5] ; Nesvorny, David [2] ; Raymond, Sean N. [6]
Total Authors: 6
Affiliation:
[1] Inst Nacl Pesquisas Espaciais, Ave Astronautas 1758, BR-12227010 Sao Jose Dos Campos, SP - Brazil
[2] Southwest Res Inst, Dept Space Studies, 1050 Walnut St, Boulder, CO 80302 - USA
[3] Univ Estadual Paulista, Grp Dinam Orbital & Planetol, Av Dr Ariberto Pereira da Cunha 333, BR-12516410 Guaratingueta, SP - Brazil
[4] Univ Cote Azur, UMR7293, Lab Lagrange, Observ Cote Azur, CNRS, Blvd Observ, F-06304 Nice 4 - France
[5] Observ Nacl, Rua Gen Jose Cristino 77, BR-20921400 Rio De Janeiro, RJ - Brazil
[6] Univ Bordeaux, Lab Astrophys Bordeaux, CNRS, B18N, Allee Geoffroy St Hilaire, F-33615 Pessac - France
Total Affiliations: 6
Document type: Journal article
Source: ASTROPHYSICAL JOURNAL; v. 864, n. 1 SEP 1 2018.
Web of Science Citations: 3
Abstract

The main asteroid belt (MB) is low in mass but dynamically excited. Here we propose a new mechanism to excite the MB during the giant planet (the ``Nice model{''}) instability, which is expected to feature repeated close encounters between Jupiter and one or more ice giants ({''}jumping Jupiter{''} or JJ). We show that, when Jupiter temporarily reaches a high-enough level of excitation, both in eccentricity and inclination, it induces strong forced vectors of eccentricity and inclination across the MB region. Because during the JJ instability Jupiter's orbit ``jumps{''} around, the forced vectors keep changing both in magnitude and phase throughout the whole MB region. The entire cold primordial MB is thus excited as a natural outcome of the JJ instability. The level of such an excitation, however, is typically larger than the current orbital excitation observed in the MB. We show that the subsequent evolution of the solar system is capable of reshaping the resultant overexcited MB to its present-day orbital state, and that a strong mass depletion (similar to 90%) is associated with the JJ instability phase and its subsequent evolution throughout the age of the solar system. (AU)

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: 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
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