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The observed features of the radio sources indicate complex propagationeffects embedded in the waves of solar radio bursts. In this work, we performray-tracing simulations on radio wave transport in the corona andinterplanetary region with anisotropic electron density fluctuations. For thefirst time, the variation of the apparent source size, burst duration, andsource position of both fundamental emission and harmonic emission at frequency35 MHz are simulated as the function of the anisotropic parameter $\alpha$ andthe angular scattering rate coefficient $\eta =\epsilon^2/h_0$, where$\epsilon^2={\langle \delta n^2\rangle}/{n^2}$ is the density fluctuation leveland $h_0$ is its correlation length near the wave exciting site. It is foundthat isotropic fluctuations produce a much larger decay time than a highlyanisotropic fluctuation for fundamental emission. By comparing the observedduration and source size with the simulation results in the parameter space, wecan estimate the scattering coefficient and the anisotropy parameter $\eta =8.9\times 10^{-5}\, \mathrm{km^{-1}}$ and $\alpha = 0.719$ with point pulsesource assumption. Position offsets due to wave scattering and refraction canproduce the co-spatial of fundamental and harmonic waves in observations ofsome type III radio bursts. The visual speed due to the wave propagation effectcan 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 largeexpansion rate of the source size. The visual speed direction is mostlyidentical to the offset direction, thus, for the observation aiming atobtaining the source position, the source centroid at the starting point iscloser to the wave excitation point.

Parametric simulation studies on the wave propagation of solar radio emission: the source size, duration, and position