@Article{DeiennoGomWalMorNes:2016:GrTaMo,
author = "Deienno, Rog{\'e}rio and Gomes, R. S. and Walsh, K. J. and
Morbidelli, A. and Nesvorn{\'y}, D.",
affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and
{Observat{\'o}rio Nacional (ON)} and {Southwest Space Research
Institute} and {Universit{\'e} C{\^o}te d'Azur} and {Southwest
Space Research Institute}",
title = "Is the Grand Tack model compatible with the orbital distribution
of main belt asteroids?",
journal = "Icarus",
year = "2016",
volume = "272",
pages = "114--124",
month = "July",
keywords = "Asteroids, dynamics, Origin, Solar System, Planetary dynamics,
Planets, migration.",
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.",
doi = "10.1016/j.icarus.2016.02.043",
url = "http://dx.doi.org/10.1016/j.icarus.2016.02.043",
issn = "0019-1035",
language = "en",
targetfile = "Deienno_is the grand.pdf",
urlaccessdate = "27 abr. 2024"
}