  We intend to study a modified version of the planar Circular Restricted
Three-Body Problem (CRTBP) by incorporating several perturbing parameters. We
consider the bigger primary as an oblate spheroid and emitting radiation while
the small primary has an elongated body. We also consider the perturbation from
a disk-like structure encompassing this three-body system. First, we develop a
mathematical model of this modified CRTBP. We have found there exist five
equilibrium points in this modified CRTBP model, where three of them are
collinear and the other two are non-collinear. Second, we apply our modified
CRTBP model to the Sun-Haumea system by considering several values of each
perturbing parameter. Through our numerical investigation, we have discovered
that the incorporation of perturbing parameters has resulted in a shift in the
equilibrium point positions of the Sun-Haumea system compared to their
positions in the classical CRTBP. The stability of equilibrium points is
investigated. We have shown that the collinear equilibrium points are unstable
and the stability of non-collinear equilibrium points depends on the mass
parameter $\mu$ of the system. Unlike the classical case, non-collinear
equilibrium points have both a maximum and minimum limit of $\mu$ for achieving
stability. We remark that the stability range of $\mu$ in non-collinear
equilibrium points depends on the perturbing parameters. In context of the
Sun-Haumea system, we have found that the non-collinear equilibrium points are
stable.

Earth and Planetary Astrophysics;Dynamical Systems