CURRENT STUDIES OF STAR AND GALAXY FORMATION HAVE CONCLUDED THAT ENERGETIC FEEDBACK FROM YOUNG STARS AND SUPERNOVAE (SNE) IS CRUCIAL BOTH FOR CONTROLLING OBSERVED INTERSTELLAR MEDIUM (ISM) PROPERTIES AND STAR FORMATION RATES IN THE MILKY WAY AND OTHER GALAXIES AND FOR DRIVING GALACTIC WINDS THAT GOVERN THE BARYON ABUNDANCE IN DARK MATTER HALOS. HOWEVER IN MANY NUMERICAL STUDIES OF THE ISM ENERGY INPUTS HAVE NOT BEEN IMPLEMENTED SELF-CONSISTENTLY WITH THE EVOLVING RATE OF GRAVITATIONAL COLLAPSE TO MAKE STARS OR HAVE CONSIDERED ONLY ISOLATED STAR-FORMING CLOUDS WITHOUT A REALISTIC GALACTIC ENVIRONMENT (INCLUDING SHEARED ROTATION AND EXTERNALLYORIGINATING SNE) OR HAVE NOT DIRECTLY INCORPORATED RADIATION MAGNETIC AND CHEMICAL EFFECTS THAT ARE IMPORTANT OR EVEN DOMINANT. IN MODELS OF GALAXY FORMATION AND EVOLUTION IN THE COSMIC CONTEXT GALACTIC WINDS ARE INDISPENSABLE BUT HIGHLY UNCERTAIN AS THE PHYSICS OF SUPERBUBBLE EVOLUTION AND RADIATION-GAS INTERACTIONS CANNOT BE RESOLVED. OUR CENTRAL OBJECTIVES ARE (1) TO ADDRESS THE ABOVE LIMITATIONS OF CURRENT MODELS DEVELOPING SELF-CONSISTENT SIMULATIONS OF THE MULTIPHASE ISM IN DISK GALAXIES THAT RESOLVE BOTH STAR FORMATION AND STELLAR FEEDBACK COVERING THE RANGE OF SCALES NEEDED TO CONNECT STAR CLUSTER FORMATION TO GALACTIC SUPERWIND EJECTION AND THE RANGE OF ENVIRONMENTS FROM DWARFS TO ULIRGS; AND (2) TO ANALYZE THE DETAILED PROPERTIES OF THE GAS MAGNETIC FIELD RADIATION FIELD AND STAR FORMATION/SNE IN OUR SIMULATIONS INCLUDING DEPENDENCIES ON LOCAL GALACTIC DISK ENVIRONMENT AND TO CONNECT INTRINSIC PROPERTIES WITH OBSERVABLE DIAGNOSTICS. THE PROPOSED PROJECT WILL EMPLOY THE ATHENA CODE FOR NUMERICAL MAGNETO-HYDRODYNAMIC (MHD) AND RADIATION-HYDRODYNAMIC (RHD) SIMULATIONS USING COMPREHENSIVE PHYSICS MODULES THAT HAVE BEEN DEVELOPED TESTED AND DEMONSTRATED IN SAMPLE SIMULATIONS. WE WILL CONSIDER LOCAL ``SHEARING BOX'' DISK MODELS WITH GAS SURFACE DENSITY SIGMA = 2 - 10 000 MSUN/PC^2 AND A RANGE OF STELLAR POTENTIALS AND GALACTIC ROTATION RATES. OUR SIMULATIONS FOLLOW ALL THERMAL PHASES OF THE GAS THE DRIVING OF TURBULENCE AND THE EXPULSION OF MATERIAL IN HIGH-VELOCITY GALACTIC WINDS AS WELL AS THE CIRCULATION OF LOWER-VELOCITY MATERIAL IN GALACTIC ``FOUNTAINS.'' WE RESOLVE GRAVITATIONAL COLLAPSE AND APPLY STELLAR POPULATION MODELING TO DETERMINE RADIATION EMITTED BY STAR CLUSTER PARTICLES AND BOTH IN SITU AND RUNAWAY O-STAR SN EVENTS. WITH TIME-DEPENDENT CHEMISTRY WE WILL BE ABLE TO FOLLOW C+/C/CO TRANSITIONS AND ASSESS THE RELATIONSHIP BETWEEN THE OBSERVED MOLECULAR COMPONENT AND SELF-GRAVITATING OR DIFFUSE CLOUDS IN VARYING GALACTIC ENVIRONMENTS ALSO DETERMINING HOW CLOUD PROPERTIES (E.G. DISTRIBUTIONS OF MASS SIZE VIRIAL PARAMETER INTERNAL/EXTERNAL PRESSURE MAGNETIZATION) AND LIFETIMES DEPEND ON ENVIRONMENT. WE WILL ALSO INVESTIGATE THE DEPENDENCE ON LOCAL GALACTIC ENVIRONMENT OF: * MASS AND VOLUME FRACTIONS AND TURBULENT AND MAGNETIC STATE OF EACH THERMAL AND CHEMICAL ISM PHASE * STAR FORMATION RATE AND GALACTIC WIND MASS LOSS RATE IN EACH ISM PHASE * METRICS OF ISM ENERGY GAIN/LOSS LARGE-SCALE FORCE BALANCE WIND ACCELERATION * ROLES OF SN AND RADIATION FEEDBACK IN SETTING CLOUD SFES OVERALL SFRS AND WIND MASS-LOSS RATES OUR MODELS WILL BE VALUABLE FOR INTERPRETING A WIDE RANGE OF OBSERVATIONS WITH CHANDRA HUBBLE SPITZER HERSCHEL HERSCHEL PLANCK AND GROUND-BASED TELESCOPES. OBTAINING SELF-CONSISTENT SOLUTIONS FOR THE DYNAMICAL THERMAL MAGNETIC CHEMICAL AND RADIATIVE STATE OF THE STAR-FORMING ISM IS A LONG-SOUGHT GOAL OF GALACTIC THEORY. UNDERSTANDING WHY ISM AND STAR FORMATION PROPERTIES VARY AMONG AND WITHIN GALAXIES IS ESSENTIAL FOR INTERPRETING NEW MULTIWAVELENGTH EXTRAGALACTIC SURVEYS. CONNECTING GALACTIC WINDS TO STAR FORMATION VIA RESOLVED PHYSICAL MECHANISMS WILL PROVIDE A MISSING LINK IN CONTEMPORARY GALAXY FORMATION MODELS. WITH OUR PLANNED RESEARCH PROGRAM WE ARE IN A POSITION TO ACHIEVE ALL OF THESE ADVANCES.