AM Canum Venaticorum (AM CVn) systems are binary systems composed of a white dwarf accreting from a helium donor star. The system is formed after the binary systems becomes so compact that the helium star starts depositing matter around the white dwarf, creating an accretion disk. AM CVn systems are of great interest since they have the smallest spatial dynamic range of all other  binary systems, making them perfect for global simulations of the accretion disk around the white dwarf star. Similarly, they are a prominent source of gravitational waves because of their compactness. We attempt to reproduce the frequency spectrum of AM CVn systems by calculating line spectra and including scattering effects in the accretion disk. To obtain the frequency spectrum we use Python scripts to solve the time independent radiative transfer equation using the method of short characteristics. We hope to better understand turbulent dynamics and thermodynamics of accretion disks in binary systems in general, not just AM CVn systems. So far, we have successfully reproduced absorption line spectra for hydrogen accretion disks using local shearing box simulations. We then make the transition to local and global simulations of AM CVn systems (helium systems) and including scattering effects. By calculating the frequency spectrum and comparing it to the observational data, we aim to understand how well our simulations of turbulence in accretion disks can explain observations. We will then analyze this information to further our understanding of other accretion disk systems.