@Article{BrasilNesvGome:2014:DyImOb,
               author = "Brasil, Pedro Ivo de Oliveira and Nesvorny, D. and Gomes, R. S.",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Southwest 
                         Research Institute} and {Observatorio Nacional (ON)}",
                title = "Dynamical implantation of objects in the kuiper belt",
              journal = "Astronomical Journal",
                 year = "2014",
               volume = "148",
               number = "3",
                month = "Sep.",
             keywords = "Kuiper belt: general, planetary systems.",
             abstract = "Several models have been suggested in the past to describe the 
                         dynamical formation of hot Kuiper Belt objects (hereafter Hot 
                         Classicals or HCs for short). Here, we discuss a dynamical 
                         mechanism that allows orbits to evolve from the primordial 
                         planetesimal disk at less than or similar to 35 AU to reach the 
                         orbital region now occupied by HCs. We performed three different 
                         sets of numerical simulations to illustrate this mechanism. Two of 
                         these simulations were based on modern theories for the early 
                         evolution of the solar system (the Nice and jumping-Jupiter 
                         models). The third simulation was performed with the purpose of 
                         increasing the resolution at 41-46 AU. The common aspect of these 
                         simulations is that Neptune scatters planetesimals from less than 
                         or similar to 35 AU to >40 AU and then undergoes a long phase of 
                         slow residual migration. Our results show that to reach an HC 
                         orbit, a scattered planetesimal needs to be captured in a mean 
                         motion resonance (MMR) with Neptune where the perihelion distance 
                         rises due to the Kozai resonance (which occurs in MMRs even for 
                         moderate inclinations). Finally, while Neptune is still migrating, 
                         the planetesimal is released from the MMR on a stable HC orbit. We 
                         show that the orbital distribution of HCs expected from this 
                         process provides a reasonable match to observations. The capture 
                         efficiency and the mass deposited into the HC region appears to be 
                         sensitive to the maximum eccentricity reached by Neptune during 
                         the planetary instability phase. Additional work will be needed to 
                         resolve this dependency in detail.",
                  doi = "10.1088/0004-6256/148/3/56",
                  url = "http://dx.doi.org/10.1088/0004-6256/148/3/56",
                 issn = "0004-6256",
                label = "isi 2014-11 BrasilNesvGome:2014:DYIMOB",
             language = "en",
        urlaccessdate = "28 abr. 2024"
}