WE PROPOSE TO STUDY THE ROLE OF WAVE DYNAMICS ON THE ORIGIN AND EVOLUTION OF HOT JUPITERS. THIS WORK WILL ADDRESS HOW ANGULAR MOMENTUM TRANSPORT BY TIDALLY AND CONVECTIVELY DRIVEN WAVES AFFECTS THE ORBITAL EVOLUTION AND OBSERVATIONAL INFERENCES OF HOT JUPITERS. WE WILL USE TWO (2D) AND THREE (3D) DIMENSIONAL NONLINEAR HYDRODYNAMIC SIMULATIONS TO UNDERSTAND: 1) ANGULAR MOMENTUM TRANSPORT BY CONVECTIVELY DRIVEN WAVES WITHIN STARS AND HOW THESE WAVES AFFECT STELLAR ROTATIONAL EVOLUTION 2) THE INTERACTION OF TIDALLY-INDUCED WAVES WITH CONVECTIVELY-GENERATED WAVES AND HOW THEIR MUTUAL DISSIPATION AFFECTS THE ORBITAL EVOLUTION OF HOT JUPITERS AND 3) HOW THIS COMBINED ANGULAR MOMENTUM TRANSPORT AFFECTS THE OBSERVATIONAL INFERENCES OF THE EVOLUTION OF PLANETARY ORBITAL PROPERTIES. SPECIFICALLY THESE STUDIES WILL SHED LIGHT ON THE OBSERVED DICHOTOMY BETWEEN THE OBLIQUITY OF PLANETS AROUND HOT STARS VERSUS THOSE AROUND COOL STARS AND WILL PROVIDE AN ESTIMATE FOR THE TIDAL DISSIPATION FUNCTION Q FOR EXOPLANETS' HOST STARS. IN ORDER TO TEST OUR MODELS WE WILL MAKE OBSERVATIONAL PREDICTIONS WHICH MAY BE CHECKED WITH EXISTING DATA FROM NASA'S KEPLER MISSION AND FORTHCOMING SEARCHES FROM THE TESS MISSION AS WELL AS GROUND-BASED FOLLOW-UP RADIAL VELOCITY OBSERVATIONS.