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@Article{AljbaaeChPrCaHuSoMe:2019:OrStNe,
               author = "Aljbaae, Safwan and Chanut, Thierry Gregory Gil and Prado, Antonio 
                         Fernando Bertachini de Almeida and Carruba, V. and Hussmann, H. 
                         and Souchay, J. and Merguizo Sanchez, Diogo",
          affiliation = "{Instituto Nacional de Pesquisas Espaciais (INPE)} and {Instituto 
                         Nacional de Pesquisas Espaciais (INPE)} and {Instituto Nacional de 
                         Pesquisas Espaciais (INPE)} and {Universidade Estadual Paulista 
                         (UNESP)} and {DLR Institute of Planetary Research} and {Sorbonne 
                         Universites} and {Instituto Nacional de Pesquisas Espaciais 
                         (INPE)}",
                title = "Orbital stability near the (87) Sylvia system",
              journal = "Monthly Notices of The Royal Astronomical Society",
                 year = "2019",
               volume = "486",
               number = "2",
                pages = "2557--2569",
             keywords = "Astrodin{\^a}mica, Astrodynamics, Aster{\'o}ides, gravitation, 
                         celestial mechanics, minor planets, asteroids: individual: (87) 
                         Sylvia.",
             abstract = "The main goal of our work is to study the orbital dynamics of a 
                         spacecraft near the (87) Sylvia system. Here, we consider a 
                         non-homogeneous mass distribution with a dense core inside the 
                         primary asteroid. The Mascon gravity framework using the shaped 
                         polyhedral source, from light-curve data, is chosen to calculate 
                         the gravitational field. The zero-velocity curves show four 
                         unstable equilibrium points. In the absence of any solar or other 
                         celestial body perturbations, a numerical analysis of the orbital 
                         dynamics in the potential field of Sylvia is done to delineate the 
                         region of stable and unstable motions. In our model, the motions 
                         of the two moons of Sylvia and of the spacecraft are integrated 
                         with the classical equations of motion in the body-fixed frame of 
                         reference. An orbit is considered stable if the variation of its 
                         periapsis radius does not exceed a threshold value (i.e. 6 km), 
                         and the variation of its eccentricity does not exceed 0.05, 
                         although the orientation of these orbits may change. We found that 
                         the first stable orbit is detected at a distance of 550 km from 
                         the centre of Sylvia. No collision occurs with the central body 
                         beyond 350 km. The collisions with Remus occur between 300 and 900 
                         km, while with Romulus they occur between 900 and 1450 km. 
                         Moreover, the orbits escape from the system when the distance is 
                         smaller than 350 km. Finally, we found that the stability region 
                         around our system decreases when the initial eccentricity 
                         increases.",
                  doi = "10.1093/mnras/stz998",
                  url = "http://dx.doi.org/10.1093/mnras/stz998",
                 issn = "0035-8711 and 1365-2966",
                label = "lattes: 7340081273816424 3 AljbaaeChPrCaHuSoSa:2019:OrStNe",
             language = "en",
        urlaccessdate = "23 nov. 2020"
}


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