  We report the results of an analysis of the redshift power spectrum
$P^S(k,\mu)$ in three typical Cold Dark Matter (CDM) cosmological models, where
$\mu$ is the cosine of the angle between the wave vector and the line-of-sight.
Two distinct biased tracers derived from the primordial density peaks of
Bardeen et al. and the cluster-underweight model of Jing, Mo, & B\"orner are
considered in addition to the pure dark matter models. Based on a large set of
high resolution simulations, we have measured the redshift power spectrum for
the three tracers from the linear to the nonlinear regime. We investigate the
validity of the relation - guessed from linear theory - in the nonlinear regime
$$ P^S(k,\mu)=P^R(k)[1+\beta\mu^2]^2D(k,\mu,\sigma_{12}(k)), $$ where $P^R(k)$
is the real space power spectrum, and $\beta$ equals $\Omega_0^{0.6}/b_l$. The
damping function $D$ which should generally depend on $k$, $\mu$, and
$\sigma_{12}(k)$, is found to be a function of only one variable
$k\mu\sigma_{12}(k)$. This scaling behavior extends into the nonlinear regime,
while $D$ can be accurately expressed as a Lorentz function - well known from
linear theory - for values $D > 0.1$. The difference between $\sigma_{12}(k)$
and the pairwise velocity dispersion defined by the 3-D peculiar velocity of
the simulations (taking $r=1/k$) is about 15%. Therefore $\sigma_{12}(k)$ is a
good indicator of the pairwise velocity dispersion. The exact functional form
of $D$ depends on the cosmological model and on the bias scheme. We have given
an accurate fitting formula for the functional form of $D$ for the models
studied.
