  The observed features of the radio sources indicate complex propagation
effects embedded in the waves of solar radio bursts. In this work, we perform
ray-tracing simulations on radio wave transport in the corona and
interplanetary region with anisotropic electron density fluctuations. For the
first time, the variation of the apparent source size, burst duration, and
source position of both fundamental emission and harmonic emission at frequency
35 MHz are simulated as the function of the anisotropic parameter $\alpha$ and
the angular scattering rate coefficient $\eta =\epsilon^2/h_0$, where
$\epsilon^2={\langle \delta n^2\rangle}/{n^2}$ is the density fluctuation level
and $h_0$ is its correlation length near the wave exciting site. It is found
that isotropic fluctuations produce a much larger decay time than a highly
anisotropic fluctuation for fundamental emission. By comparing the observed
duration and source size with the simulation results in the parameter space, we
can estimate the scattering coefficient and the anisotropy parameter $\eta =
8.9\times 10^{-5}\, \mathrm{km^{-1}}$ and $\alpha = 0.719$ with point pulse
source assumption. Position offsets due to wave scattering and refraction can
produce the co-spatial of fundamental and harmonic waves in observations of
some type III radio bursts. The visual speed due to the wave propagation effect
can reach 1.5\,$c$ for $\eta = 2.4\times 10^{-4}\, \mathrm{km^{-1}}$ and
$\alpha=0.2$ for fundamental emission in the sky plane, accompanying with large
expansion rate of the source size. The visual speed direction is mostly
identical to the offset direction, thus, for the observation aiming at
obtaining the source position, the source centroid at the starting point is
closer to the wave excitation point.
