@Article{DeiennoMorbGomeNesv:2017:ImTiPl,
author = "Deienno, Rog{\'e}rio and Morbidelli, Alessandro and Gomes, Rodney
S. and Nesvorny, David",
affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and
{Universit{\'e} C{\^o}te d’Azur} and {Observat{\'o}rio Nacional
(ON)} and {Southwest Research Institute}",
title = "Constraining the giant planets' initial configuration from their
evolution: implications for the timing of the planetary
instability",
journal = "Astronomical Journal",
year = "2017",
volume = "153",
number = "4",
month = "Apr.",
keywords = "planets and satellites: dynamical evolution and stability.",
abstract = "Recent works on planetary migration show that the orbital
structure of the Kuiper Belt can be very well reproduced if,
before the onset of planetary instability, Neptune underwent a
long-range planetesimal-driven migration up to \∼28 au.
However, considering that all giant planets should have been
captured in mean motion resonances among themselves during the
gas-disk phase, it is not clear whether such a very specific
evolution for Neptune is possible, or whether the instability
could have happened at late times. Here, we first investigate
which initial resonant configuration of the giant planets can be
compatible with Neptune being extracted from the resonant chain
and migrating to \∼28 au before planetary instability. We
address the late instability issue by investigating the conditions
where the planets can stay in resonance for about 400 Myr. Our
results indicate that this can happen only in the case where the
planetesimal disk is beyond a specific minimum distance \δ
stab from Neptune. Then, if there is a sufficient amount of dust
produced in the planetesimal disk, which drifts inwards, Neptune
can enter a slow dust-driven migration phase for hundreds of Myr
until it reaches a critical distance from the disk. From that
point, faster planetesimal-driven migration takes over and Neptune
continues migrating outward until the instability happens. We
conclude that although an early instability more easily reproduces
the evolution of Neptune required to explain the structure of the
Kuiper Belt, such evolution is also compatible with a late
instability.",
doi = "10.3847/1538-3881/aa5eaa",
url = "http://dx.doi.org/10.3847/1538-3881/aa5eaa",
issn = "0004-6256",
language = "en",
targetfile = "deienno.pdf",
urlaccessdate = "27 abr. 2024"
}