@Article{NesvornıVokrDeieWals:2014:ExOrIn,
               author = "Nesvorn{\'y}, David and Vokrouhlicky, David and Deienno, Rogerio 
                         and Walsh, Kevin J.",
          affiliation = "SW Res Inst, Dept Space Studies, Boulder, CO 80302 USA. and SW Res 
                         Inst, Dept Space Studies, Boulder, CO 80302 USA.; Charles Univ 
                         Prague, Inst Astron, CR-18000 Prague 8, Czech Republic. and 
                         {Instituto Nacional de Pesquisas Espaciais (INPE)} and SW Res 
                         Inst, Dept Space Studies, Boulder, CO 80302 USA.",
                title = "Excitation of the orbital inclination of iapetus during planetary 
                         encounters",
              journal = "Astronomical Journal",
                 year = "2014",
               volume = "148",
               number = "3",
                month = "Sep.",
             keywords = "planets and satellites: dynamical evolution and stability, planets 
                         and satellites: individual (Titan, Iapetus).",
             abstract = "Saturn's moon, Iapetus, has an orbit in a transition region where 
                         the Laplace surface is bending from the equator to the orbital 
                         plane of Saturn. The orbital inclination of Iapetus to the local 
                         Laplace plane is similar or equal to 8 degrees, which is 
                         unexpected because the inclination should be similar or equal to 0 
                         if Iapetus formed from a circumplanetary disk on the Laplace 
                         surface. It thus appears that some process has pumped up Iapetus's 
                         inclination while leaving its eccentricity near zero (e similar or 
                         equal to 0.03 at present). Here, we examined the possibility that 
                         Iapetus's inclination was excited during the early solar system 
                         instability when encounters between Saturn and ice giants 
                         occurred. We found that the dynamical effects of planetary 
                         encounters on Iapetus's orbit sensitively depend on the distance 
                         of the few closest encounters. In 4 out of 10 instability cases 
                         studied here, the orbital perturbations were too large to be 
                         plausible. In one case, Iapetus's orbit was practically 
                         unaffected. In the remaining five cases, the perturbations of 
                         Iapetus's inclination were adequate to explain its present value. 
                         In three of these cases, however, Iapetus's eccentricity was 
                         excited to >0.1-0.25, and it is not clear whether it could have 
                         been damped to its present value (similar or equal to 0.03) by a 
                         subsequent process (e.g., tides and dynamical friction from 
                         captured irregular satellites do not seem to be strong enough). 
                         Our results therefore imply that only 2 out of 10 instability 
                         cases (similar to 20\%) can excite Iapetus's inclination to its 
                         current value (similar to 30\% of trials lead to >5 degrees) 
                         while leaving its orbital eccentricity low.",
                  doi = "10.1088/0004-6256/148/3/52",
                  url = "http://dx.doi.org/10.1088/0004-6256/148/3/52",
                 issn = "0004-6256",
                label = "isi 2014-11 NesvornyVokrDeieWals:2014:EXORIN",
             language = "en",
        urlaccessdate = "28 abr. 2024"
}