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@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 = "01 dez. 2020"
}


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