THIS PROPOSAL IS DEVOTED TO A SERIES OF THEORETICAL AND COMPUTATIONAL STUDIES ON THE FORMATION OF CLOSE-IN GIANT PLANETS SUCH AS HOT JUPITERS (HJS WITH PERIODS<10 DAYS) AND WARM JUPITERS (WJS WITH PERIODS 10-200 DAYS). MORE THAN TWO DECADES AFTER THE DISCOVERY OF THE FIRST HJS THE ORIGIN OF HJS REMAINS AN OUTSTANDING UNSOLVED PROBLEM IN EXOPLANETARY SCIENCE. MANY OF THESE SYSTEMS EXHIBIT INTRIGUING SPIN-ORBIT MISALIGNMENTS I.E. THE PLANET'S ORBITAL ANGULAR MOMENTUM AXIS IS MISALIGNED WITH THE SPIN AXIS OF THE HOST STAR. A LARGE CLASS OF MODELS FOR HJ/WJ FORMATION RELY ON HIGH-ECCENTRICITY MIGRATION IN WHICH A GAS GIANT (FORMED AT A FEW AU) IS PUMPED INTO A VERY ECCENTRIC ORBIT AS A RESULT OF GRAVITATIONAL INTERACTIONS WITH OTHER PLANETS OR WITH A DISTANT STELLAR COMPANION FOLLOWED BY TIDAL DISSIPATION WHICH CIRCULARIZES THE PLANET S ORBIT. WHILE THESE MODELS ARE SUCCESSFUL IN EXPLAINING SOME OBSERVATIONS SEVERAL FUNDAMENTAL PROBLEMS REMAIN AND CONCRETE PREDICTIONS ARE LACKING IN MANY CASES. A MAJOR CONCERN IS THE TIDAL DISSIPATION IN THE PLANET. WE HAVE RECENTLY ``DISCOVERED'' THAT UNDER SOME REALISTIC CONDITIONS TIDAL EXCITATIONS OF INTERNAL OSCILLATION MODES IN THE PLANET IN AN ECCENTRIC ORBIT CAN DRIVE CHAOTIC MODE GROWTH LEADING TO RAPID MODE DISSIPATION AND ORBITAL DECAY. THESE DYNAMICAL (CHAOTIC) TIDES MAY RESOLVE SEVERAL OUTSTANDING ISSUES RELATED TO HIGH-ECCENTRICITY MIGRATION. IN PARTICULAR THEY COULD LEAD TO RAPID FORMATION OF ECCENTRIC WJS AND INCREASE THE FORMATION FRACTION OF HJS. COMBINING WITH A PROPER TREATMENT OF SPIN-ORBIT COUPLING THEY MAY ALSO LEAD TO SIGNIFICANT CHANGES IN THE PREDICTIONS OF THE FINAL SPIN-ORBIT MISALIGNMENTS IN ALL HIGH-ECCENTRICITY MIGRATION SCENARIOS. THE MAIN EFFORT OF OUR PROPOSED RESEARCH WILL BE DEVOTED TO INCORPORATING DYNAMICAL TIDES INTO TWO OF MOST IMPORTANT CLASSES OF HIGH-ECCENTRICITY MIGRATION SCENARIOS: (1) LIDOV-KOZAI MIGRATION DRIVEN BY STELLAR OR PLANETARY COMPANIONS; (2) ``SECULAR CHAOS'' RESULTING FROM INTERACTIONS BETWEEN THREE OR MORE PLANETS. WE WILL USE THE SECULAR EQUATIONS OF MOTION AT THE OCTUPOLE-LEVEL [FOR (1)] AND A NEWLY DEVELOPED GAUSSIAN RING CODE [FOR (2)] TO EVOLVE THE PLANET'S ORBITS AND AT THE SAME TIME FOLLOW THE EVOLUTION OF THE MODE AMPLITUDES (DYNAMICAL TIDES). THE GOAL IS TO UNDERSTAND HOW DYNAMICAL TIDES AFFECT THE HJ/WJ FORMATION EFFICIENCY AND TIMESCALES AND COMPUTE THE ORBITAL PROPERTIES OF HJS AND WJS PRODUCED IN THESE SCENARIOS. WE WILL ALSO INVESTIGATE THE DYNAMICS OF STELLAR SPIN WITH THE GOAL OF PREDICTING THE SPIN-ORBIT MISALIGNMENT DISTRIBUTIONS FOR DIFFERENT HOST STARS AND PLANETS. WE WILL ALSO CARRY OUT MORE EXPLORATORY STUDIES ON THE PHYSICS OF DYNAMICAL TIDES AND THE THERMAL EVOLUTION OF GIANT PLANETS (INCLUDING DYNAMICAL TIDAL HEATING) UNDERGOING HIGH-ECCENTRICITY MIGRATION. THIS PROPOSAL IS RELEVANT TO NASA'S EXOPLANET RESEARCH PROGRAM GOAL OF ``IMPROVE UNDERSTANDING OF THE ORIGINS OF EXOPLANETARY SYSTEMS''. THE PROPOSED RESEARCH WILL ALSO HELP ENHANCE THE SCIENCE RETURN OF ONGOING AND FUTURE NASA SPACE MISSIONS SUCH AS KEPLER/K2 AND TESS.