BLACK HOLES (BHS) ARE A FUNDAMENTAL PREDICTION OF EINSTEIN'S THEORY OF GENERAL RELATIVITY (GR) AND ARE CHARACTERIZED BY THEIR MASSES AND SPINS. THIS PROPOSAL CONSIDERS HOW THE RATES AND LIGHT CURVES OF TIDAL DISRUPTION EVENTS (TDES) DEPEND ON BH SPIN. TDES OCCUR WHEN A SUPERMASSIVE BH'S TIDAL FIELD OVERWHELMS A STAR'S SELF-GRAVITY RIPPING THE STAR APART AND FUELING LUMINOUS EMISSION FROM TIDAL STREAM COLLISIONS AND ACCRETION DISKS. SEVERAL DOZEN TDE CANDIDATES HAVE BEEN OBSERVED ACROSS THE ELECTROMAGNETIC SPECTRUM (INCLUDING SEVERAL BY THE NASA MISSIONS GALEX CHANDRA AND SWIFT) AND POTENTIALLY THOUSANDS MORE MAY BE SEEN IN FUTURE SURVEYS. GR IS CRUCIAL TO UNDERSTANDING TDES AS THE GRAVITATIONAL RADIUS WHERE RELATIVITY BECOMES IMPORTANT CAN BE COMPARABLE TO THE TIDAL RADIUS AT WHICH DISRUPTION OCCURS. SEVERAL RELATIVISTIC EFFECTS MAKE TDES OBSERVATIONALLY SENSITIVE TO BH SPIN. WHILE TIDAL FORCES ONLY DEPEND ON THE DISTANCE FROM THE BH AND ITS MASS IN NEWTONIAN GRAVITY IN GR THEY ALSO DEPEND ON THE BH'S SPIN AND THE ENERGY ANGULAR MOMENTUM AND INCLINATION OF THE STAR'S INITIAL ORBIT WITH RESPECT TO THE BH'S EQUATORIAL PLANE.