THE EVOLUTION OF THE CORONAL AND SOLAR WIND PLASMA AND HELIOSPHERIC ENERGETIC PARTICLES INVOLVES A BROAD RANGE OF LENGTH AND TIME SCALES EXTENDING ACROSS DIVERSE REGIONS OF SPACE AND ACCORDINGLY INVOLVING AT LEAST SEVERAL LEVELS OF PHYSICAL DESCRIPTION FLUID KINETIC ELECTROMAGNETIC AND MULTISPECIES. THE GENERAL GOALS OF UNDERSTANDING HELIOSPHERIC PHYSICS AND THE SPECIFIC GOALS OF SPACE WEATHER STUDIES MUST DEAL AT SOME LEVEL WITH ALL OF THESE MULTI-SCALE MULTI-REGIONAL AND MULTI-PHYSICS CHALLENGES. A GRAND CHALLENGE OBJECTIVE OF THE LIVING WITH A STAR (LWS) AND SPACE WEATHER IS TO ATTAIN SUN-TO-MUD DYNAMICAL DESCRIPTIONS OF STEADY AND TRANSIENT CONDITIONS. EXISTING EFFORTS HAVE GENERALLY SIMPLIFIED THE MULTI-SCALE AND MULTIPHYSICS ASPECTS IN ORDER TO ATTAIN MULTI-REGIONAL RESULTS.THE PREMISE OF THE PRESENT PROPOSAL IS THAT TO MOVE FORWARD SIGNIFICANT IMPROVEMENTS ARE NEEDED IN THE MULTISCALE AREA WHERE MODELS NEED TO DEAL WITH THE SCALE SEPARATION PROBLEM INHERENT IN NONSTEADY NONLINEAR FLOWS WHILE ALSO TAKING IMPORTANT STEPS TOWARDSMORE REALISTIC PHYSICS BY DEVELOPING MULTIFLUID DESCRIPTIONS.THIS PROPOSAL SEEKS TO IMPROVE MODELING OF THE SOLAR WIND CORONA AND ENERGETIC PARTICLES IN THE INNER HELIOSPHERE AND TO DEVELOP THREE DELIVERABLES WITHIN A FIVE YEAR PERIOD: (1) THE CENTER PIECE OF THE PROJECT IS A MULTIFLUID SOLAR WIND CODE THAT WILL INCLUDE TURBULENCE MODELING. THIS THREE DIMENSIONAL (3D) SOLAR WIND CODE WILL BE BASED ON THE CURRENT USMANOV ET AL. CODE BUT OPERATING BETWEEN 0.1 AU AND 1 AU THAT IS OUTSIDE THE ALFV EN CRITICAL POINT TO THE EARTH. THE TURBULENCE MODEL CURRENTLY OF THE REYNOLDS AVERAGED NAVIER-STOKES (RANS) TYPE WILL BE EXPANDED AND IMPROVED TO INCLUDE A LARGE EDDY SIMULATION (LES) APPROACH AND SUBGRID-SCALE MODELING. THE MODEL WILL INCLUDE PROTON ELECTRON AND HELIUM FLUIDS; 2) AN IMPORTANT ELEMENT BOTH FOR COMPLETENESS OF SPACE WEATHER MODELING AND TO PROVIDE BOUNDARY DATA FOR THE SOLAR WIND CODE IS A NEW 3D CORONAL CODE IN THE SUB-ALFV ENIC REGION ALSO INCLUDING MULTIFLUIDS AND A TURBULENCE MODEL SPECIALIZED FOR CORONAL PLASMA CONDITIONS. THIS MODEL IS MORE EXPERIMENTAL IN NATURE AND WILL REQUIRE DEVELOPMENT IN STAGES; 3) THE FINAL COMPONENT A TRANSPORT CODE FOR ENERGETIC PARTICLES NOTABLY SOLAR ENERGETIC PARTICLES WILL INCLUDE A FOCUSED TRANSPORT MODEL ADAPTED TO THE DYNAMIC SIMULATION DATA FROM MODELS (1) AND (2). THE INTERFACES BETWEEN THESE MODELS WILL BE DESIGNED FOR INTEROPERABILITY INCLUDING INTERFACING WITH MODELS DEVELOPED ELSEWHERE. WE WILL ALSO WORK TOWARD INTEGRATION OF THE TRANSPORT CODE AND INTERPLANETARY CODES WITH GLOBAL MAGNETOHYDRODYNAMIC (MHD) MODELS OF THE MAGNETOSPHERE TO ESTIMATE THE EFFECT OF SPACE WEATHER EVENTS ON MAGNETOSPHERIC DYNAMICS.BY BRINGING TOGETHER AN EXPERIENCED TEAM WITH EXPERTISE IN SOLAR WIND CORONAL AND MAGNETOSPHERIC PHYSICS HYDRODYNAMIC AND MHD TURBULENCE MODELING AND LARGE SCALE TURBULENCE CORONAL AND SOLAR WIND SIMULATIONS IN COMBINATION WITH EXPERIENCE IN ANALYSIS OF SPACECRAFT OBSERVATIONS FOR VERIFICATION AND TESTING WE EXPECT TO MAKE STEADY AND SIGNIFICANT PROGRESS IN THIS CHALLENGING AREA LEADING TO USEFUL DELIVERABLES WITHIN BOTH THREE AND FIVE YEAR PERIODS. THIS PROJECT DIRECTLY ADDRESSES GOALS OF LWS AND SPACE WEATHER AND WILL PRODUCE VALUABLE TOOLS TO BE MADE PUBLICLY AVAILABLE OF DIRECT VALUE TO THE SOLAR PROBE AND SOLAR ORBITER MISSIONS. SCOPE AND COLLABORATOR LIST IS ADJUSTED TO REFLECT PARTIAL SUPPORT REQUESTED.