  Radio observations grant access to a wide range of physical processes through
different emission mechanisms. These processes range from thermal and quiescent
to eruptive phenomena, such as shock waves and particle beams. We present a new
synthetic radio imaging tool that calculates and visualizes the Bremsstrahlung
radio emission. This tool works concurrently with state-of-the-art
Magnetohydrodynamic (MHD) simulations of the solar corona using the code
BATS-R-US. Our model produces results that are in good agreement with both high
and low frequency observations of the solar disk. In this study, a ray-tracing
algorithm is used and the radio intensity is computed along the actual curved
ray trajectories. We illustrate the importance of refraction in locating the
radio emitting source by comparison of the radio imaging illustrations when the
line-of-sight instead of the refracted paths are considered. We are planning to
incorporate non-thermal radio emission mechanisms in a future version of the
radio imaging tool.
