  We have investigated the relation between the two-point spatial correlation
function and the density profile of the dark matter halo in the strongly
non-linear regime. It is well known that when the density fluctuation grows
into dark matter halo whose density profile is $\rho \propto
r^{-\epsilon}$(${3/2}<\epsilon<3$) on almost all mass scales, the two-point
spatial correlation function obeys a power law with the power index $\gamma =
2\epsilon -3$ in the strongly non-linear regime. We find the form of the
two-point spatial correlation function, which does not obey the power law when
the power index $\epsilon$ is smaller than 3/2, such as the density profile
$\rho \propto r^{-1}$ around the center of the halo which is proposed by
Navarro, Frenk & White (1996,1997). By using the BBGKY equation in the strongly
non-linear regime, it is also found that velocity parameter $h \equiv - < v > /
\dot{a}x$ is not a constant even in the strongly non-linear regime ($\tilde{x}
\equiv x/x_{nl} \to 0$) although it is a constant when $\epsilon > 3/2$ and
then the two-point spatial correlation function can be regarded as the power
law. The velocity parameter $h$ becomes 0 at the non-linear limit of $\tilde{x}
\to 0$, that is, the stable clustering hypothesis cannot be satisfied when
$\epsilon < 3/2$.
