  The physical properties responsible for the formation and evolution of the
corona and heliosphere are still not completely understood. 3D MHD global
modeling is a powerful tool to investigate all the possible candidate
processes. To fully understand the role of each of them, we need a validation
process where the output from the simulations is quantitatively compared to the
observational data. In this work, we present the results from our validation
process applied to the wave turbulence driven 3D MHD corona-wind model
WindPredict-AW. At this stage of the model development, we focus the work to
the coronal regime in quiescent condition. We analyze three simulations
results, which differ by the boundary values. We use the 3D distributions of
density and temperature, output from the simulations at the time of around the
First Parker Solar Probe perihelion (during minimum of the solar activity), to
synthesize both extreme ultraviolet (EUV) and white light polarized (WL pB)
images to reproduce the observed solar corona. For these tests, we selected AIA
193 A, 211 A and 171 A EUV emissions, MLSO K-Cor and LASCO C2 pB images
obtained the 6 and 7 November 2018. We then make quantitative comparisons of
the disk and off limb corona. We show that our model is able to produce
synthetic images comparable to those of the observed corona.
