  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 spacecraft's 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 solar radiation
pressure at the perihelion, semi-major 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 solar radiation pressure in equatorial orbits close to the asteroid
(101955) Bennu. As results, we find that the mascon model divided into ten
equal layers seems to be the most suitable for this problem. We can highlight
that the centre point $E$8, 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 $\psi_0 = -180^o$, starting
with the spacecraft longitude $\lambda = 0$, 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 $\psi_0 = -135^o$, the orbits with initial longitude $\lambda = 90^0 $
appear to be more stable. Finally, when the passage of the spacecraft in the
shadow is accounted for, the effects of solar radiation pressure are softened,
and we find more stable orbits.
