@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"
}