ACCRETION DISKS LIKELY PROVIDE THE CONDUIT FOR FUELING ACTIVE GALACTIC NUCLEI (AGN) LINKING THE BLACK HOLE S IMMEDIATE SURROUNDINGS TO THE HOST GALAXY S NUCLEAR STAR CLUSTER AND POSSIBLY BEYOND. YET DETAILED AGN DISK MODELS FAIL TO EXPLAIN SEVERAL OF THE MOST BASIC OBSERVATIONAL FEATURES OF AGN: HOW DO THE OUTER REGIONS OF THE DISK AVOID STALLING AS A RESULT OF WHOLESALE GRAVITATIONAL FRAGMENTATION? WHAT REGULATES THE AMOUNT OF STAR FORMATION THAT IS INFERRED TO ACCOMPANY ACCRETION IN SOME AGN? WHY IS THE BROAD EMISSION LINE REGION A UBIQUITOUS FEATURE OF LUMINOUS AGN? WHAT PROCESSES CREATE AND MAINTAIN THE SO-CALLED DUSTY TORUS ? ANALYTIC WORK SUGGESTS THAT VERTICAL PRESSURE SUPPORT OF THE DISK PRIMARILY BY A TOROIDAL MAGNETIC FIELD RATHER THAN BY GAS OR RADIATION PRESSURE CAN READILY RESOLVE THESE PROBLEMS. AND RECENT NUMERICAL SIMULATIONS HAVE INDICATED THAT SUCH A STRONG TOROIDAL FIELD IS THE INEVITABLE CONSEQUENCE OF THE MAGNETOROTATIONAL INSTABILITY (MRI) WHEN A DISK ACCUMULATES A MODEST AMOUNT OF NET MAGNETIC FLUX THUS PROVIDING A SOUND THEORETICAL BASIS FOR STRONGLY MAGNETIZED DISKS. WE PROPOSE AN ANALYTIC AND COMPUTATIONAL STUDY OF SUCH DISKS IN THE AGN CONTEXT FOCUSING ON: (1) THE BASIC PHYSICAL PROPERTIES OF STRONGLY MAGNETIZED AGN DISKS. WE WILL FOCUS ON THE COMPETITION BETWEEN FIELD GENERATION AND BUOYANCY IMPROVING ON PREVIOUS WORK BY CONSIDERING REALISTIC EQUATIONS OF STATE DISSIPATIVE PROCESSES AND RADIATIVE LOSSES. WE WILL USE GLOBAL SIMULATIONS TO TEST THE LIMITING MAGNETIC FIELDS THAT CAN BE PRODUCED BY MRI-DRIVEN ACCRETION DISK DYNAMOS AND EXPLORE THE DRIVING MECHANISMS OF DISK WINDS AND THE RESULTING LEVELS OF MASS ANGULAR MOMENTUM AND ENERGY LOSS. (2) GRAVITATIONAL FRAGMENTATION AND STAR FORMATION IN STRONGLY MAGNETIZED DISKS. WE WILL DETERMINE HOW A STRONG FIELD REDUCES AND REGULATES GRAVITATIONAL FRAGMENTATION BY BOTH LOWERING THE DISK DENSITY AND CREATING A STRATIFIED STRUCTURE IN WHICH STAR FORMATION NEAR THE EQUATOR CAN CO-EXIST WITH ACCRETION AT LARGE HEIGHTS. USING SIMULATIONS WE WILL STUDY FRAGMENTATION CONDITIONS THE CLUMPINESS OF STABLE AGN DISKS AND THE MASS FUNCTION OF COLLAPSED CLUMPS. (3) PHYSICS OF THE BROAD EMISSION LINE REGION AND DUSTY TORUS . WE WILL STUDY THE POSSIBLE ROLE OF THE STRONG TOROIDAL FIELD IN PROMOTING THERMAL INSTABILITIES TO CREATE DENSE LINE-EMITTING FILAMENTS TRANSPORTING THEM IN HEIGHT AND CONFINING THE LINE-EMITTING GAS. EXTRAPOLATING TO SLIGHTLY LARGER DISTANCES WE WILL EXAMINE WHETHER THE FIELD CAN ELEVATE DUSTY GAS TO HEIGHTS AT WHICH IT CAN REPROCESS A SUBSTANTIAL FRACTION OF THE AGN RADIATION. THIS STUDY WILL ESTABLISH A NEW THEORETICAL FRAMEWORK FOR INTERPRETING MULTI-WAVELENGTH OBSERVATIONS OF AGN INVOLVING NASA S INFRARED ULTRAVIOLET AND X-RAY OBSERVATORIES AS WELL AS GROUND-BASED DETECTORS. IT ADDRESSES FUNDAMENTAL QUESTIONS ABOUT HOW SUPERMASSIVE BLACK HOLES INTERACT WITH THEIR GALACTIC ENVIRONMENTS AS WELL AS BROADER ISSUES OF FEEDBACK AND BLACK HOLE-GALAXY COEVOLUTION.