JUPITER'S MOON IO IS PRESENTLY UNDERGOING A PRODIGIOUS AMOUNT OF VOLCANIC ACTIVITY FAR EXCEEDING THE LEVEL OF VOLCANISM ON EARTH OR ANY OTHER SOLID-BODY OBJECT IN OUR SOLAR SYSTEM. UNDERSTANDING THE INTERIOR DYNAMICS THAT PRODUCES THIS VOLCANISM IS A FUNDAMENTAL PROBLEM IN PLANETARY GEOPHYSICS. IO'S VOLCANISM IS DRIVEN BY TIDAL HEATING OF ITS INTERIOR AND THE MAGNITUDE OF TIDAL HEATING AT A GIVEN LOCATION DEPENDS IN PART ON THE VISCOSITY AND SHEAR MODULUS OF THAT MATERIAL AND THUS ON BOTH THE MANTLE TEMPERATURE AND THE PRESENCE OF MAGMA. HOWEVER THE THERMAL STRUCTURE CAN EVOLVE WITH TIME BOTH DUE TO CONVECTIVE FLOW IN THE MANTLE AND BY THE PRODUCTION OF MAGMA. RISING MAGMA TRANSPORTS HEAT FROM THE MANTLE TO THE CRUST. AS THE MANTLE TEMPERATURE EVOLVES THE VISCOSITY WILL CHANGE LEADING IN TURN TO CHANGES IN THE TIDAL HEATING RATE. CHANGES IN THE TIDAL HEATING MAY IN TURN CAUSE CHANGES IN THE MANTLE FLOW. THUS RIGOROUS MODELS OF MANTLE CONVECTION ON IO MUST CONSIDER THE COUPLINGS AMONG TIDAL HEAT GENERATION MANTLE CONVECTION THE RHEOLOGY LAW AND THE PRODUCTION AND TRANSPORT OF MAGMA. EXISTING MODELS OF MANTLE CONVECTION ON IO HAVE MADE THE SIMPLIFYING ASSUMPTION THAT TIDAL HEATING CAN BE IMPOSED WITH A FIXED SPATIAL PATTERN AND AMPLITUDE. MOST EXISTING IO CONVECTION MODELS ALSO DO NOT CALCULATE MAGMA PRODUCTION AND INSTEAD TREAT ITS EFFECTS ON HEAT TRANSPORT BY A SURFACE BOUNDARY CONDITION.