Many previous studies have proposed the slow stressing of magnetic field and subsequent release of energy as a mechanism for maintaining the high temperature of coronal plasma. Whilst direct observational evidence of braided fields within the Sun's atmosphere remains elusive, if these models are representative, then we might expect significant field complexity to exist within coronal structures. Meanwhile, over the past 20 years, many observational studies have highlighted the abundance of wave power throughout the solar atmosphere. In this context, we present the results of three dimensional MHD simulations of propagating waves in complex magnetic fields. We discuss the observed wave dynamics, formation of small spatial scales and establish what may be inferred about the nature of the background plasma.