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Dynamical evolution of asteroid families

Grant number: 14/24071-7
Support Opportunities:Scholarships abroad - Research
Effective date (Start): August 24, 2015
Effective date (End): February 20, 2016
Field of knowledge:Physical Sciences and Mathematics - Astronomy - Solar System Astronomy
Principal Investigator:Valerio Carruba
Grantee:Valerio Carruba
Host Investigator: David Nesvorny
Host Institution: Faculdade de Engenharia (FEG). Universidade Estadual Paulista (UNESP). Campus de Guaratinguetá. Guaratinguetá , SP, Brazil
Research place: Southwest Research Institute, Boulder (SwRI), United States  


The current structure of the Solar System was deeply shaped by the effects of planetary migration. The most recent models of planetary migration suggest that the current orbital distribution of asteroids, and in particular the low ratio between highly and low inclined population could be better explained in the ``Jumping-Jupiter'' scenario, in which both Jupiter and Saturn have close encounters with a Neptune-mass planet. The implication of this scenario for the main asteroid belt involve, apart for a paucity of highly inclined objects, the formation of about 10 asteroid families with a parent body with a diameter larger than 200 km and about 100 asteroid families from parent body with diameters of the order of 100 km. While it has been argued that asteroid families from parent bodies with diameters of the order of 100 km would no longer be recognizable, because of dynamical evolution caused by comminution of asteroids with D < 10 km and evolution through the Yarkovsky and YORP effect of the smaller fragments, a key parameter for constraining the models of planetary migration through the Jumping-Jupiter scenario is the number of families from large parent bodies old enough to have experienced the last phases of planetary migration and collisions with cometary bodies (the Late Heavy Bombardment phase, or LHB). Better understanding of the YORP cycle (the so-called stochastic YORP effect) and of the modeling of the evolution of asteroid families can now allow to obtain a better estimate of the ages of the 12 asteroid families currently believed to be older than 2 Byr. In this work we are proposing to i) use new and improved Monte Carlo methods (the so-called Yarko-Yorpmodeling) to obtain refined estimates of the ages of these 12 key families, and ii) to estimate the effect that the last phases of the jumping-jupiter migration may have had on the real and ficticious families already formed 3.8 Byr ago. Spin-offs of this research project also include the study of families in the so-calles ``pristine region'' between the 5J:-2A and 7J:-3A mean-motion resonances with Jupiter to check the possibility that some of them could be associated with the long-lost 100~km parent-body families formed during the late phases of the LHB. (AU)

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Scientific publications (5)
(References retrieved automatically from Web of Science and SciELO through information on FAPESP grants and their corresponding numbers as mentioned in the publications by the authors)
CARRUBA, V.; ALJBAAE, S.; WINTER, O. C.. On the Erigone family and the z(2) secular resonance. Monthly Notices of the Royal Astronomical Society, v. 455, n. 3, p. 2279-2288, . (13/15357-1, 14/24071-7, 11/08171-3, 14/06762-2)
CARRUBA, V.; NESVORNY, D.; ALJBAAE, S.. Characterizing the original ejection velocity field of the Koronis family. ICARUS, v. 271, p. 57-66, . (13/15357-1, 14/24071-7)
CARRUBA, V.; NESVORNY, D.; ALJBAAE, S.; DOMINGOS, R. C.; HUAMAN, M.. On the oldest asteroid families in the main belt. Monthly Notices of the Royal Astronomical Society, v. 458, n. 4, p. 3731-3738, . (14/24071-7, 14/06762-2)
CARRUBA, V.; NESVORNY, D.. Constraints on the original ejection velocity fields of asteroid families. Monthly Notices of the Royal Astronomical Society, v. 457, n. 2, p. 1332-1338, . (14/24071-7)

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