Not listed MOIST CONVECTION IS LIKELY A CRITICAL PROCESS FOR DETERMINING ENERGY REDISTRIBUTION AND THE DRIVE FOR THE LARGE SCALE CIRCULATION ON GAS GIANT PLANETS. THE UNDERSTANDING OF THESE PROCESSES AND CONSEQUENTLY THEIR REPRESENTATION IN DYNAMICAL MODELS IS AS YET POORLYDEVELOPED. PART OF THIS LACK OF DEVELOPMENT HAS BEEN ASSOCIATED WITH THE LACK OF MODELING FRAMEWORKS AND COMPUTING POWER TO ADEQUATELY ADDRESS THE PROBLEM BUT THE LACK OF GOOD OBSERVATIONAL 'CALIBRATION' CASES HAS ALSO PRESENTED AN OBSTACLE. IN THIS PROPOSAL WE PROPOSE TO USE ADVANCES IN COMPUTING POWER AND MODEL DEVELOPMENT TO EMPLOY NESTED SYNOPTIC-TO-MESOSCALE MODELING OF CLOUDSYSTEMS AND MOIST CONVECTION USING MASSIVELY PARALLEL COMPUTING. CRUCIALLY WE PROPOSE TO FOCUS THE EFFORT ON WELL DOCUMENTED "GREAT WHITE SPOT" (GWS) CONVECTIVE CLOUD SYSTEMS ON SATURN. NOT ONLY IS THE MORPHOLOGICAL EVOLUTION OF THESE STORMS WELL OBSERVED USING IMAGING BUT THERMAL AND TRACE PROCESS DATA EXIST FROM THERMAL OBSERVATIONS. IN PARTICULAR PARA/ORTHO HYDROGEN OBSERVATIONS PROVIDESIGNIFICANT CONSTRAINTS ON THE DISTRIBUTION AND VIGOR OF MOIST CONVECTION.THE GOAL OF THIS PROPOSAL IS TO UNDERSTAND THE PHYSICAL PROCESSES ASSOCIATED WITH CONVECTIVE STORMS AND THE DYNAMICAL INTERACTIONS BETWEEN STORMS AND THE LARGE-SCALE DYNAMICS. MORE SPECIFICALLY WE WILL DEVELOP A COMPREHENSIVE MOIST CONVECTION SCHEME THAT CHARACTERIZES THE WATER AND AMMONIA CLOUD DYNAMICS ON SATURN AND JUPITER AND INVESTIGATE THE FORMATION AND EVOLUTION OF CONVECTIVESTORMS AT VARIOUS SCALES. THE DEVELOPMENT OF SUCH A NUMERICAL SCHEME WITHIN GLOBAL MODELS IS A CRITICAL PREREQUISITE FOR MAKING FURTHER PROGRESS ON UNDERSTANDING THE GENERAL CIRCULATION OF THE GAS GIANT ATMOSPHERES.WE PROPOSE TO USE IMAGING AND INFRARED OBSERVATIONS FROM CASSINI IN COMBINATION WITH OUR PLANETWRF MODEL TO EXAMINE MOIST CONVECTION AND SPECIFICALLY THE WELL DOCUMENTED GWS TEST CASE ON CLOUD RESOLVING SCALES AND ALSO THEIR INTERACTION WITH LARGER-SCALE FLOWS. THE NESTED CLOUD-RESOLVING TO GLOBAL SCALE CAPABILITY OF PLANETWRF MAKES IT A UNIQUELY CAPABLE MODEL IN THIS APPLICATION. THERESULTS FROM THE USE OF PLANETWRF TO SYNTHESIZE AND GENERALIZED OBSERVATIONS OF MOIST CONVECTION WILL BE USED TO FORMULATE SIMPLIFIED PLUME MODELS OF MOIST CONVECTION THAT CAN BE INCLUDED IN PURELY GLOBAL MODELS OF INSUFFICIENT RESOLUTION TO DIRECTLY CAPTURE THESEPROCESSES.THE GENERAL CIRCULATION OF GAS GIANT ATMOSPHERES IS A MAJOR SCIENCE FOCUS FOR NASA BOTH IN TERMS OF THE GAS GIANTS IN OUR OWN SOLAR SYSTEM BUT ALSO BECAUSE OF THE IMPORTANCE OF GAS GIANT DYNAMICS FOR UNDERSTANDING EXTRA-SOLAR PLANETS. ($95k) 11/7/17 4 MOIST CONVECTION IS LIKELY A CRITICAL PROCESS FOR DETERMINING ENERGY REDISTRIBUTION AND THE DRIVE FOR THE LARGE SCALE CIRCULATION ON GAS GIANT PLANETS. THE UNDERSTANDING OF THESE PROCESSES AND CONSEQUENTLY THEIR REPRESENTATION IN DYNAMICAL MODELS IS AS YET POORLY DEVELOPED. PART OF THIS LACK OF DEVELOPMENT HAS BEEN ASSOCIATED WITH THE LACK OF MODELING FRAMEWORKS AND COMPUTING POWER TO ADEQUATELY ADDRESS THE PROBLEM, BUT THE LACK OF GOOD OBSERVATIONAL 'CALIBRATION' CASES HAS ALSO PRESENTED AN OBSTACLE. IN THIS PROPOSAL, WE PROPOSE TO USE ADVANCES IN COMPUTING POWER AND MODEL DEVELOPMENT TO EMPLOY NESTED SYNOPTIC-TO-MESOSCALE MODELING OF CLOUD SYSTEMS AND MOIST CONVECTION USING MASSIVELY PARALLEL COMPUTING. CRUCIALLY, WE PROPOSE TO FOCUS THE EFFORT ON WELL DOCUMENTED "GREAT WHITE SPOT" (GWS) CONVECTIVE CLOUD SYSTEMS ON SATURN. NOT ONLY IS THE MORPHOLOGICAL EVOLUTION OF THESE STORMS WELL OBSERVED USING IMAGING, BUT THERMAL AND TRACE PROCESS DATA EXIST FROM THERMAL OBSERVATIONS. IN PARTICULAR, PARA/ORTHO HYDROGEN OBSERVATIONS PROVIDE SIGNIFICANT CONSTRAINTS ON THE DISTRIBUTION AND VIGOR OF MOIST CONVECTION. THE GOAL OF THIS PROPOSAL IS TO UNDERSTAND THE PHYSICAL PROCESSES ASSOCIATED WITH CONVECTIVE STORMS AND THE DYNAMICAL INTERACTIONS BETWEEN STORMS AND THE LARGE-SCALE DYNAMICS. MORE SPECIFICALLY, WE WILL DEVELOP A COMPREHENSIVE MOIST CONVECTION SCHEME THAT CHARACTERIZES THE WATER AND AMMONIA CLOUD DYNAMICS ON SATURN AND JUPITER AND INVESTIGATE THE FORMATION AND EVOLUTION OF CONVECTIVE STORMS AT VARIOUS SCALES. THE DEVELOPMENT OF SUCH A NUMERICAL SCHEME WITHIN GLOBAL MODELS IS A CRITICAL PREREQUISITE FOR MAKING FURTHER PROGRESS ON UNDERSTANDING THE GENERAL CIRCULATION OF THE GAS GIANT ATMOSPHERES. WE PROPOSE TO USE IMAGING AND INFRARED OBSERVATIONS FROM CASSINI IN COMBINATION WITH OUR PLANETWRF MODEL TO EXAMINE MOIST CONVECTION, AND SPECIFICALLY THE WELL DOCUMENTED GWS TEST CASE, ON CLOUD RESOLVING SCALES AND ALSO THEIR INTERACTION WITH LARGER-SCALE FLOWS. THE NESTED CLOUD-RESOLVING TO GLOBAL SCALE CAPABILITY OF PLANETWRF MAKES IT A UNIQUELY CAPABLE MODEL IN THIS APPLICATION. THE RESULTS FROM THE USE OF PLANETWRF TO SYNTHESIZE AND GENERALIZED OBSERVATIONS OF MOIST CONVECTION WILL BE USED TO FORMULATE SIMPLIFIED PLUME MODELS OF MOIST CONVECTION THAT CAN BE INCLUDED IN PURELY GLOBAL MODELS OF INSUFFICIENT RESOLUTION TO DIRECTLY CAPTURE THESE PROCESSES. THE GENERAL CIRCULATION OF GAS GIANT ATMOSPHERES IS A MAJOR SCIENCE FOCUS FOR NASA, BOTH IN TERMS OF THE GAS GIANTS IN OUR OWN SOLAR SYSTEM, BUT ALSO BECAUSE OF THE IMPORTANCE OF GAS GIANT DYNAMICS FOR UNDERSTANDING EXTRA-SOLAR PLANETS. Funding Only Action ($95k) 11/7/17 3 MOIST CONVECTION IS LIKELY A CRITICAL PROCESS FOR DETERMINING ENERGY REDISTRIBUTION AND THE DRIVE FOR THE LARGE SCALE CIRCULATION ON GAS GIANT PLANETS. THE UNDERSTANDING OF THESE PROCESSES AND CONSEQUENTLY THEIR REPRESENTATION IN DYNAMICAL MODELS IS AS YET POORLY DEVELOPED. PART OF THIS LACK OF DEVELOPMENT HAS BEEN ASSOCIATED WITH THE LACK OF MODELING FRAMEWORKS AND COMPUTING POWER TO ADEQUATELY ADDRESS THE PROBLEM, BUT THE LACK OF GOOD OBSERVATIONAL 'CALIBRATION' CASES HAS ALSO PRESENTED AN OBSTACLE. IN THIS PROPOSAL, WE PROPOSE TO USE ADVANCES IN COMPUTING POWER AND MODEL DEVELOPMENT TO EMPLOY NESTED SYNOPTIC-TO-MESOSCALE MODELING OF CLOUD SYSTEMS AND MOIST CONVECTION USING MASSIVELY PARALLEL COMPUTING. CRUCIALLY, WE PROPOSE TO FOCUS THE EFFORT ON WELL DOCUMENTED "GREAT WHITE SPOT" (GWS) CONVECTIVE CLOUD SYSTEMS ON SATURN. NOT ONLY IS THE MORPHOLOGICAL EVOLUTION OF THESE STORMS WELL OBSERVED USING IMAGING, BUT THERMAL AND TRACE PROCESS DATA EXIST FROM THERMAL OBSERVATIONS. IN PARTICULAR, PARA/ORTHO HYDROGEN OBSERVATIONS PROVIDE SIGNIFICANT CONSTRAINTS ON THE DISTRIBUTION AND VIGOR OF MOIST CONVECTION. THE GOAL OF THIS PROPOSAL IS TO UNDERSTAND THE PHYSICAL PROCESSES ASSOCIATED WITH CONVECTIVE STORMS AND THE DYNAMICAL INTERACTIONS BETWEEN STORMS AND THE LARGE-SCALE DYNAMICS. MORE SPECIFICALLY, WE WILL DEVELOP A COMPREHENSIVE MOIST CONVECTION SCHEME THAT CHARACTERIZES THE WATER AND AMMONIA CLOUD DYNAMICS ON SATURN AND JUPITER AND INVESTIGATE THE FORMATION AND EVOLUTION OF CONVECTIVE STORMS AT VARIOUS SCALES. THE DEVELOPMENT OF SUCH A NUMERICAL SCHEME WITHIN GLOBAL MODELS IS A CRITICAL PREREQUISITE FOR MAKING FURTHER PROGRESS ON UNDERSTANDING THE GENERAL CIRCULATION OF THE GAS GIANT ATMOSPHERES. WE PROPOSE TO USE IMAGING AND INFRARED OBSERVATIONS FROM CASSINI IN COMBINATION WITH OUR PLANETWRF MODEL TO EXAMINE MOIST CONVECTION, AND SPECIFICALLY THE WELL DOCUMENTED GWS TEST CASE, ON CLOUD RESOLVING SCALES AND ALSO THEIR INTERACTION WITH LARGER-SCALE FLOWS. THE NESTED CLOUD-RESOLVING TO GLOBAL SCALE CAPABILITY OF PLANETWRF MAKES IT A UNIQUELY CAPABLE MODEL IN THIS APPLICATION. THE RESULTS FROM THE USE OF PLANETWRF TO SYNTHESIZE AND GENERALIZED OBSERVATIONS OF MOIST CONVECTION WILL BE USED TO FORMULATE SIMPLIFIED PLUME MODELS OF MOIST CONVECTION THAT CAN BE INCLUDED IN PURELY GLOBAL MODELS OF INSUFFICIENT RESOLUTION TO DIRECTLY CAPTURE THESE PROCESSES. THE GENERAL CIRCULATION OF GAS GIANT ATMOSPHERES IS A MAJOR SCIENCE FOCUS FOR NASA, BOTH IN TERMS OF THE GAS GIANTS IN OUR OWN SOLAR SYSTEM, BUT ALSO BECAUSE OF THE IMPORTANCE OF GAS GIANT DYNAMICS FOR UNDERSTANDING EXTRA-SOLAR PLANETS. Funding Only Action $0 6/2/17 Not listed MOIST CONVECTION IS LIKELY A CRITICAL PROCESS FOR DETERMINING ENERGY REDISTRIBUTION AND THE DRIVE FOR THE LARGE SCALE CIRCULATION ON GAS GIANT PLANETS. THE UNDERSTANDING OF THESE PROCESSES AND CONSEQUENTLY THEIR REPRESENTATION IN DYNAMICAL MODELS IS AS YET POORLYDEVELOPED. PART OF THIS LACK OF DEVELOPMENT HAS BEEN ASSOCIATED WITH THE LACK OF MODELING FRAMEWORKS AND COMPUTING POWER TO ADEQUATELY ADDRESS THE PROBLEM BUT THE LACK OF GOOD OBSERVATIONAL 'CALIBRATION' CASES HAS ALSO PRESENTED AN OBSTACLE. IN THIS PROPOSAL WE PROPOSE TO USE ADVANCES IN COMPUTING POWER AND MODEL DEVELOPMENT TO EMPLOY NESTED SYNOPTIC-TO-MESOSCALE MODELING OF CLOUDSYSTEMS AND MOIST CONVECTION USING MASSIVELY PARALLEL COMPUTING. CRUCIALLY WE PROPOSE TO FOCUS THE EFFORT ON WELL DOCUMENTED "GREAT WHITE SPOT" (GWS) CONVECTIVE CLOUD SYSTEMS ON SATURN. NOT ONLY IS THE MORPHOLOGICAL EVOLUTION OF THESE STORMS WELL OBSERVED USING IMAGING BUT THERMAL AND TRACE PROCESS DATA EXIST FROM THERMAL OBSERVATIONS. IN PARTICULAR PARA/ORTHO HYDROGEN OBSERVATIONS PROVIDESIGNIFICANT CONSTRAINTS ON THE DISTRIBUTION AND VIGOR OF MOIST CONVECTION.THE GOAL OF THIS PROPOSAL IS TO UNDERSTAND THE PHYSICAL PROCESSES ASSOCIATED WITH CONVECTIVE STORMS AND THE DYNAMICAL INTERACTIONS BETWEEN STORMS AND THE LARGE-SCALE DYNAMICS. MORE SPECIFICALLY WE WILL DEVELOP A COMPREHENSIVE MOIST CONVECTION SCHEME THAT CHARACTERIZES THE WATER AND AMMONIA CLOUD DYNAMICS ON SATURN AND JUPITER AND INVESTIGATE THE FORMATION AND EVOLUTION OF CONVECTIVESTORMS AT VARIOUS SCALES. THE DEVELOPMENT OF SUCH A NUMERICAL SCHEME WITHIN GLOBAL MODELS IS A CRITICAL PREREQUISITE FOR MAKING FURTHER PROGRESS ON UNDERSTANDING THE GENERAL CIRCULATION OF THE GAS GIANT ATMOSPHERES.WE PROPOSE TO USE IMAGING AND INFRARED OBSERVATIONS FROM CASSINI IN COMBINATION WITH OUR PLANETWRF MODEL TO EXAMINE MOIST CONVECTION AND SPECIFICALLY THE WELL DOCUMENTED GWS TEST CASE ON CLOUD RESOLVING SCALES AND ALSO THEIR INTERACTION WITH LARGER-SCALE FLOWS. THE NESTED CLOUD-RESOLVING TO GLOBAL SCALE CAPABILITY OF PLANETWRF MAKES IT A UNIQUELY CAPABLE MODEL IN THIS APPLICATION. THERESULTS FROM THE USE OF PLANETWRF TO SYNTHESIZE AND GENERALIZED OBSERVATIONS OF MOIST CONVECTION WILL BE USED TO FORMULATE SIMPLIFIED PLUME MODELS OF MOIST CONVECTION THAT CAN BE INCLUDED IN PURELY GLOBAL MODELS OF INSUFFICIENT RESOLUTION TO DIRECTLY CAPTURE THESEPROCESSES.THE GENERAL CIRCULATION OF GAS GIANT ATMOSPHERES IS A MAJOR SCIENCE FOCUS FOR NASA BOTH IN TERMS OF THE GAS GIANTS IN OUR OWN SOLAR SYSTEM BUT ALSO BECAUSE OF THE IMPORTANCE OF GAS GIANT DYNAMICS FOR UNDERSTANDING EXTRA-SOLAR PLANETS. $0 6/2/17 Not listed MOIST CONVECTION IS LIKELY A CRITICAL PROCESS FOR DETERMINING ENERGY REDISTRIBUTION AND THE DRIVE FOR THE LARGE SCALE CIRCULATION ON GAS GIANT PLANET $132.1k 9/29/16