High velocity clouds (HVCs) are collections of gas around the Milky Way galaxy and othergalaxies with masses ranging from tens of thousands of solar masses to millions of solarmasses. These cool clouds can potentially supply new cool material to the disks of galaxies.Many unanswered questions exist about HVCs; e.g. How do HVCs form?, How long canHVCs survive while interacting with the hot ambient material?, and How do HVCs affect,and how are they affected by, our Galaxy?Using detailed multi-dimensional numerical simulations, this study focuses on how HVCsinteract with their ambient environments and how these interactions affect the clouds metalconcentration, condensation and evaporation rates, and morphology. Using the results ofthese simulations this study suggests methods to determine the origins of HVCs based onobserved metal concentrations, and how initial parameter space affects the condensation ofambient material onto HVCs.