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@Article{CarrubaHuaDomSanSou:2014:DyEvVt,
               author = "Carruba, V. and Huaman, M. E. and Domingos, R. C. and Santos, C. 
                         R. dos and Souami, D.",
          affiliation = "UNESP, Univ. Estadual Paulista, Grupo de din{\^a}mica Orbital e 
                         Planetologia, Guaratinguet{\'a}, SP 12516-410, Brazil and UNESP, 
                         Univ. Estadual Paulista, Grupo de din{\^a}mica Orbital e 
                         Planetologia, Guaratinguet{\'a}, SP 12516-410, Brazil and 
                         {Instituto Nacional de Pesquisas Espaciais (INPE)} and UNESP, 
                         Univ. Estadual Paulista, Grupo de din{\^a}mica Orbital e 
                         Planetologia, Guaratinguet{\'a}, SP 12516-410, Brazil and NAXYS, 
                         Namur Center for Complex Systems, Department of Mathematics, 
                         University of Namur, B-5000 Namur, Belgium; UPMC, Universit{\'e} 
                         Pierre et Marie Curie, 4 Place Jussieu, F-75005 Paris, France; 
                         SYRTE, Observatoire de Paris, Syst{\`e}mes de R{\'e}f{\'e}rence 
                         Temps Espace, CNRS/UMR 8630, UPMC, Paris, France",
                title = "Dynamical evolution of V-type asteroids in the central main belt",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2014",
               volume = "439",
               number = "3",
                pages = "3168--3179",
             keywords = "celestial mechanics, minor planets, asteroids.",
             abstract = "V-type asteroids are associated with basaltic composition, and are 
                         supposed to be fragments of crust of differentiated objects. Most 
                         V-type asteroids in the main belt are found in the inner main 
                         belt, and are either current members of the Vesta dynamical family 
                         (Vestoids), or past members that drifted away. However, several 
                         V-type photometric candidates have been recently identified in the 
                         central and outer main belt. The origin of this large population 
                         of V-type objects is not well understood. Since it seems unlikely 
                         that Vestoids crossing the 3J:-1A mean-motion resonance with 
                         Jupiter could account for the whole population of V-type asteroids 
                         in the central and outer main belt, origin from local sources, 
                         such as the parent bodies of the Eunomia, and of the Merxia and 
                         Agnia asteroid families, has been proposed as an alternative 
                         mechanism. In this work, we investigated the dynamical evolution 
                         of the V-type photometric candidates in the central main belt, 
                         under the effect of gravitational and non-gravitational forces. 
                         Our results showthat dynamical evolution from the parent bodies of 
                         the Eunomia and Merxia/Agnia families on time-scales of 2 Byr or 
                         more could be responsible for the current orbital location of most 
                         of the low-inclined V-type asteroids.",
                  doi = "10.1093/mnras/stu192",
                  url = "http://dx.doi.org/10.1093/mnras/stu192",
                 issn = "0035-8711",
                label = "scopus 2014-05 CarrubaHuaDomDosSou:2014:DyEvVt",
             language = "en",
           targetfile = "MNRAS-2014-Carruba-mnras_stu192.pdf",
        urlaccessdate = "30 nov. 2020"
}


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