DOMINATING THE SATURNIAN SATELLITE SYSTEM AND FEATURING A MODERATELY LARGE INCLINATION AND ECCENTRICITY TITAN IS A MYSTERY. ITS ORIGINS HAVE YET TO BE SATISFACTORILY EXPLAINED USING CONVENTIONAL MODELS; NEITHER IN SITU FORMATION NOR CAPTURE FROM HELIOCENTRIC ORBIT CAN EASILY EXPLAIN ANY OF ITS PECULIARITIES. WE ARGUE THAT DYNAMICAL INSTABILITY AND SUBSEQUENT MERGERS WITHIN A RESONANT CHAIN OF SATELLITES SIMILAR TO THE GALILEAN MOONS COULD BE RESPONSIBLE FOR MANY BIZARRE FEATURES OF TITAN AND ITS EQUALLY STRANGE COMPANION HYPERION. TO TEST THIS THEORY WE WILL EMPLOY THE N-BODY INTEGRATORS HNBODY AND HNDRAG. INITIALLY WE WILL PERFORM SIMULATIONS TO TEST FOR CONDITIONS NECESSARY FOR INSTABILITY BY VARYING A WIDE RANGE OF PARAMETERS INCLUDING NUMBER OF SATELLITES MASS DISTRIBUTION AND TYPE AND STRENGTH OF RESONANCES. AFTER FINDING SUITABLE CANDIDATES FOR FURTHER STUDY WE WILL RESTRICT OUR FOCUS TO DETERMINE POSSIBLE MERGER SEQUENCES THAT CULMINATE IN A SINGLE BODY MIRRORING TITAN S FEATURES. WE WILL ALSO STUDY THE LIKELIHOOD OF FRAGMENTS FROM THE RESULTANT DEBRIS CLOUD ESCAPING TITAN S GRAVITY WELL AND SUBSEQUENTLY STABILIZING AND ACCRETING NEARBY WHICH WE BELIEVE WAS THE PROCESS LEADING TO THE FORMATION OF HYPERION. THIS WORK DIRECTLY ADDRESSES BOTH THE PLANETARY SCIENCE RESEARCH PROGRAM GOALS AND THE BROADER NASA SCIENCE MISSION DIRECTORATE. IT SEEKS TO ANSWER QUESTIONS ABOUT THE ORIGIN OF A NOTEWORTHY SOLAR SYSTEM BODY AND ALSO INDIRECTLY EVALUATES THE POTENTIAL FOR PAST OR PRESENT LIFE ON TITAN BY HELPING US BETTER UNDERSTAND THE EVOLUTION OF ITS ATMOSPHERE AND SURFACE FEATURES. FURTHERMORE KNOWLEDGE GAINED ABOUT THE REQUISITE CONDITIONS FOR DYNAMICAL INSTABILITY WITHIN SATELLITE SYSTEMS IS BROADLY APPLICABLE TO FORMATION THEORIES ON A VARIETY OF SCALES FROM THE FIVE SATELLITES OF PLUTO TO LARGE TIGHTLY PACKED EXOPLANET SYSTEMS TO OUR OWN MOON.