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@Article{Gomes-JúniorGBAVCSTGBBBBDDDEEHJMMMMPSW:2015:ReTwMu,
               author = "Gomes-J{\'u}nior, A. R. and Giacchini, B. L. and Braga-Ribas, F. 
                         and Assafin, M. and Vieira-Martins, R. and Camargo, J. I. B. and 
                         Sicardy, B. and Timerson, B. and George, T. and Broughton, J. and 
                         Blank, T. and Benedetti-Rossi, G. and Brooks, J. and Dantowitz, R. 
                         F. and Dunham, D. W. and Dunham, J. B. and Ellington, C. K. and 
                         Emilio, M. and Herpich, F. R. and Jacques, C. and Maley, P. D. and 
                         Mehret, L. and Mello, A. J. T. and Milone, Andr{\'e} de Castro 
                         and Pimentel, E. and Schoenell, W. and Weber, N. S.",
          affiliation = "{Universidade Federal do Rio de Janeiro (UFRJ)} and {Centro 
                         Brasileiro de Pesquisas F{\'{\i}}sica (CBPF)} and 
                         {Observat{\'o}rio Nacional (ON)} and {Universidade Federal do Rio 
                         de Janeiro (UFRJ)} and {Universidade Federal do Rio de Janeiro 
                         (UFRJ)} and {Observat{\'o}rio Nacional (ON)} and {Observatoire de 
                         Paris} and {International Occultation Timing Association} and 
                         {International Occultation Timing Association} and {RASNZ 
                         Occultation Section} and {International Occultation Timing 
                         Association} and {Observat{\'o}rio Nacional (ON)} and 
                         {International Occultation Timing Association} and {Clay Center 
                         Observatory at Dexter Southfield} and {International Occultation 
                         Timing Association} and {International Occultation Timing 
                         Association} and {International Occultation Timing Association} 
                         and {Universidade Estadual de Ponta Grossa} and {Universidade 
                         Federal de Santa Catarina (UFSC)} and {Se{\c{c}}{\~a}o de 
                         Oculta{\c{c}}{\^o}es/REA-Brasil} and {International Occultation 
                         Timing Association} and {Universidade Estadual de Ponta Grossa} 
                         and {Universidade Tecnol{\'o}gica Federal do Paran{\'a} (UTFPR)} 
                         and {Instituto Nacional de Pesquisas Espaciais (INPE)} and 
                         {Se{\c{c}}{\~a}o de Oculta{\c{c}}{\^o}es/REA-Brasil} and 
                         {Universidade Federal de Santa Catarina (UFSC)} and {Centro de 
                         Estudos Astron{\^o}micos de Minas Gerais}",
                title = "Results of two multichord stellar occultations by dwarf planet (1) 
                         Ceres",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2015",
               volume = "451",
               number = "3",
                pages = "2295--2302",
             keywords = "Minor planets, asteroids: individual: (1, Ceres), Occultations, 
                         Planets and satellites: fundamental parameters.",
             abstract = "We report the results of two multichord stellar occultations by 
                         the dwarf planet (1) Ceres that were observed from Brazil on 2010 
                         August 17, and from the USA on 2013 October 25. Four positive 
                         detections were obtained for the 2010 occultation, and nine for 
                         the 2013 occultation. Elliptical models were adjusted to the 
                         observed chords to obtain Ceres' size and shape. Two limb-fitting 
                         solutions were studied for each event. The first one is a nominal 
                         solution with an indeterminate polar aspect angle. The second one 
                         was constrained by the pole coordinates as given by Drummond et 
                         al. Assuming a Maclaurin spheroid, we determine an equatorial 
                         diameter of 972 ± 6 km and an apparent oblateness of 0.08 ± 0.03 
                         as our best solution. These results are compared to all available 
                         size and shape determinations for Ceres made so far, and shall be 
                         confirmed by the NASA's Dawn space mission.",
                  doi = "10.1093/mnras/stv1081",
                  url = "http://dx.doi.org/10.1093/mnras/stv1081",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
        urlaccessdate = "04 dez. 2020"
}


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