Solar radio bursts are strongly affected by radio-wave scattering on density inhomogeneities, changing their observed time characteristics, size, and positions. Using the large-scale simulations of radio-wave transport published in Kontar et al. (2023), this interactive tool visualises the effects of anisotropic scattering on radio images with a size and shape dictated by the turbulence model $\overline{q\epsilon^2}(r)$. This quantity is the spectrum-weighted mean wavenumber of the density fluctuations (proportional to the scattering rate of radio waves), which when normalised by the solar radius and plasma density, is approximated by $\overline{q\epsilon^2}R_\odot n^2=6.5\times10^{14}\left(r/R_\odot – 1\right)^{-5.17}$ from 0.1 to 1 au. The model is inferred from solar, non-solar, and in-situ density fluctuation measurements where the largest contribution comes from the density fluctuations near the inner-scale. The model has a broad maximum near (4 - 7) R$_\odot$ and can be multiplied by a scaling factor between 0.25 - 4, with the level of anisotropy varied between 0.19 - 0.42 (where 1.0 is isotropic). This range of anisotropy and spread in $\overline{q\epsilon^2}$ scaling from 0.5 - 2 is found to account for the majority of solar radio observations.