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@Article{ChanutAljbPradCarr:2017:SoRaPr,
               author = "Chanut, T. G. G. and Aljbaae, S. and Prado, Antonio Fernando 
                         Bertachini de Almeida and Carruba, V.",
          affiliation = "{Universidade Estadual Paulista (UNESP)} and {Universidade 
                         Estadual Paulista (UNESP)} and {Instituto Nacional de Pesquisas 
                         Espaciais (INPE)} and {Universidade Estadual Paulista (UNESP)}",
                title = "Dynamics in the vicinity of (101955) Bennu: Solar radiation 
                         pressure effects in equatorial orbits",
              journal = "Monthly Notices of the Royal Astronomical Society",
                 year = "2017",
               volume = "470",
               number = "3",
                pages = "2687--2701",
                month = "Sept.",
             keywords = "gravitation, methods: numerical, celestial mechanics, minor 
                         planets, asteroids: individual: (101955) Bennu.",
             abstract = "Here, we study the dynamical effects of the solar radiation 
                         pressure (SRP) on a spacecraft that will survey the near-Earth 
                         rotating asteroid (101955) Bennu when the projected shadow is 
                         accounted for. The spacecrafts motion near (101955) Bennu is 
                         modelled in the rotating frame fixed at the centre of the 
                         asteroid, neglecting the Sun gravity effects. We calculate the SRP 
                         at the perihelion, semimajor axis and aphelion distances of the 
                         asteroid from the Sun. The goals of this work are to analyse the 
                         stability for both homogeneous and inhomogeneous mass distribution 
                         and study the effects of the SRP in equatorial orbits close to the 
                         asteroid (101955) Bennu. As results, we find that the mascon model 
                         divided into 10 equal layers seems to be the most suitable for 
                         this problem. We can highlight that the centre point E8, which was 
                         linearly stable in the case of the homogeneous mass distribution, 
                         becomes unstable in this new model changing its topological 
                         structure. For a Sun initial longitude \ψ0 = 
                         \−180\◦, starting with the spacecraft longitude 
                         \λ = 0, the orbits suffer fewer impacts and some (between 
                         0.4 and 0.5 km), remaining unwavering even if the maximum solar 
                         radiation is considered. When we change the initial longitude of 
                         the Sun to \ψ0 = \−135\◦, the orbits with 
                         initial longitude \λ = 90\◦ appear to be more stable. 
                         Finally, when the passage of the spacecraft in the shadow is 
                         accounted for, the effects of SRP are softened, and we find more 
                         stable orbits.",
                  doi = "10.1093/mnras/stx1204",
                  url = "http://dx.doi.org/10.1093/mnras/stx1204",
                 issn = "0035-8711 and 1365-2966",
             language = "en",
           targetfile = "chanut_dynamics.pdf",
        urlaccessdate = "25 nov. 2020"
}


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