  In this paper, we present a simulation method within the two-component
spherical collapse model to investigate dark energy perturbations associated
with the formation of dark matter halos. The realistic mass accretion history
of a dark matter halo taking into account its fast and slow growth is
considered by imposing suitable initial conditions and isotropized
virializations for the spherical collapse process. The dark energy component is
treated as a perfect fluid described by two important parameters, the equation
of state parameter $w$ and the sound speed $c_s$. Quintessence models with
$w>-1$ are analyzed. We adopt the Newtonian gauge to describe the spacetime
which is perturbed mainly by the formation of a dark matter halo. It is found
that the dark energy density perturbation $\delta_{DE}$ depends on $w$ and
$c_s$, and its behavior follows closely the gravitational potential $\Phi$ of
the dark matter halo with $\delta_{DE}\approx -(1+w)\Phi/c_s^2$. For $w>-1$,
the dark energy perturbation presents a clustering behavior with
$\delta_{DE}>0$ during the entire formation of the dark matter halo, from
linear to nonlinear and virialized stages. The value of $\delta_{DE}$ increases
with the increase of the halo mass. For a cluster of mass $M\sim 10^{15}
M_{\odot}$, $\delta_{DE}\sim 10^{-5}$ within the virialized region for $c_s^2
\in [0.5, 1]$, and it can reach $\delta_{DE}=O(1)$ with $c_s^2=0.00001$. For a
scalar-field dark energy model, we find that with suitably modeled $w$ and
$c_s$, its perturbation behavior associated with the nonlinear formation of
dark matter halos can well be analyzed using the fluid approach, demonstrating
the validity of the fluid description for dark energy even considering its
perturbation in the stage of nonlinear dark matter structure formation.
