Not listed OBJECTIVES WE AIM TO UNDERSTAND THE INTERIOR OF SATURN THROUGH A COMBINATION OF NEW GRAVITY FIELD DATA FROM CASSINI NEW AB INITIO SIMULATIONS OF PLANETARY MATERIALS AT HIGH PRESSURE AND NEW CALCULATIONS OF THE TEMPERATURE STRUCTURE AND GRAVITY FIELD OF THE PLANET. SATURNS INTERIOR HOLDS TREMENDOUS UNKNOWNS AND COMPLEXITIES. SATURNS INTERIOR IS COOL ENOUGH THAT THE PHASE SEPARATION OF HE FROMLIQUID METALLIC HYDROGEN HAS LIKELY BEEN OCCURRING FOR THE PAST 2 GYR. THIS HE RAIN HAS LONG BEEN SUGGESTED TO BE THE ADDITIONAL ENERGY SOURCE THAT EXPLAINS SATURNS OBSERVED HIGH INTRINSIC HEAT FLUX. HOWEVER AT THIS POINT THIS IS STILL JUST A PLAUSIBLE STORY WITHOUT A SUPPORTING QUANTITATIVE THEORY. WE AIM TO DEVELOP A CONSISTENT AND PREDICTIVE THEORETICAL FRAMEWORK TO PUT THE HE RAIN HYPOTHESIS ON A SOLID QUANTITATIVE FOOTING FOR THE FIRST TIME. THE EFFECTS OF COMPOSITION GRADIENTS DUE TO HE OR HEAVY ELEMENTS ARE NOT YET WELL UNDERSTOOD. AT THE SAME TIME THE CASSINI GRAND FINALE ORBITS WILL BRING UNPRECEDENTED JUNO LIKE CONSTRAINTS ON SATURNS GRAVITYFIELD SO WE WILL BE ABLE TO TEST IF INTERIOR STRUCTURES GUIDED BY THERMAL EVOLUTION MODELING AGREE WITH OUR UNDERSTANDING OF THE PLANETS CURRENT STATE.METHODOLOGY WE PROPOSE A TWO PRONGED APPROACH TO BETTER UNDERSTAND THE PHYSICAL STATE AND PROCESSES AFFECTING THE INTERIOR OF SATURN. AT UC BERKELEY CO I AND HIS STUDENT WILL USE POWERFUL FIRST PRINCIPLES SIMULATIONS TO MAP OUT THE H HE PHASE DIAGRAM AND EQUATION OF STATE IN THE VICINITY OF SATURNS ADIABAT. THE PRESSURE TEMPERATURE CONDITIONS FOR THE ONSET OF HE RAIN WILL BE DETERMINED. FURTHERMORE SIMULATIONS WILL PERFORMED TO DETERMINE THE EFFECTS OF WATER ROCKS AND IRON BEING MIXED WITH THE DENSEH HE FLUID. AT UC SANTA CRUZ PI AND A STUDENT WILL INCORPORATE THESE FIRST PRINCIPLE MATERIALS PROPERTIES INTO A NEW THERMAL EVOLUTION CODE TO INVESTIGATE THE THERMAL EVOLUTION OF SATURN AND FOR THE FIRST TIME ACCURATELY TREAT TEMPERATURE GRADIENTS IN REGIONS OF HE AND HEAVY ELEMENT COMPOSITION GRADIENTS. WE PLAN TO DETERMINE WHEN HE RAIN STARTED IN SATURN. WHAT IS THE MAXIMUM AMOUNTOF HEAVY ELEMENTS THAT IS CONSISTENT WITH THE OBSERVATIONS AND MATERIALS PROPERTIES? HOW ARE THESE HEAVY ELEMENTS DISTRIBUTED IN THE PLANETS INTERIOR? ALONG WITH CO I HUBBARD FORTNEY AND HIS STUDENT WILL COMPUTE STATE OF THE ART STRUCTURE MODELS THAT WILL YIELD DETAILED PREDICTIONS FOR SATURNS GRAVITY FIELD WHICH WILL BE COMPARED TO CASSINI GRAVITY DATA AND ALL AVAILABLE RING SEISMOLOGY DATA.AFTER CASSINI DATA IS IN HAND WE WILL ASSESS DEVIATIONS FROM HYDROSTATIC EQUILIBRIUM DUE TO THE POSSIBLE PRESENCE OF DEEP ZONAL WINDS. RELEVANCE THE PROPOSED THEORETICAL AND MODELING INVESTIGATION SEEKS TO ADVANCE OUR KNOWLEDGE AND UNDERSTANDING OF THE COMPOSITION AND PHYSICAL PROCESSES AT WORK IN THE INTERIOR SATURN. THE NASA CALL FOR THE CASSINI PARTICIPATING SCIENTISTS PROGRAM STATES THAT PARTICIPATING SCIENTISTS MAY PROPOSE ANY INVESTIGATION THAT WOULD USE FUTURE MISSION DATA TO ADDRESS THE GOALS OF THE CASSINI GRAND FINALE INCLUDING USING THE HIGH INCLINATION ORBITS TO STUDY SATURNS INTERNAL STRUCTURE ATMOSPHERE INNERMAGNETOSPHERE AND RINGS. OUR PROPOSED WORK FITS WITHIN THE SCOPE OF THIS PROGRAM. ($40) 2/25/22 6 OBJECTIVES WE AIM TO UNDERSTAND THE INTERIOR OF SATURN THROUGH A COMBINATION OF NEW GRAVITY FIELD DATA FROM CASSINI, NEW AB INITIO SIMULATIONS OF PLANETARY MATERIALS AT HIGH PRESSURE, AND NEW CALCULATIONS OF THE TEMPERATURE STRUCTURE AND GRAVITY FIELD OF THE PLANET. SATURNS INTERIOR HOLDS TREMENDOUS UNKNOWNS AND COMPLEXITIES. SATURNS INTERIOR IS COOL ENOUGH THAT THE PHASE SEPARATION OF HE FROM LIQUID METALLIC HYDROGEN HAS LIKELY BEEN OCCURRING FOR THE PAST 2 GYR. THIS HE RAIN HAS LONG BEEN SUGGESTED TO BE THE ADDITIONAL ENERGY SOURCE THAT EXPLAINS SATURNS OBSERVED HIGH INTRINSIC HEAT FLUX. HOWEVER, AT THIS POINT THIS IS STILL JUST A PLAUSIBLE STORY WITHOUT A SUPPORTING, QUANTITATIVE THEORY. WE AIM TO DEVELOP A CONSISTENT AND PREDICTIVE THEORETICAL FRAMEWORK TO PUT THE HE RAIN HYPOTHESIS ON A SOLID QUANTITATIVE FOOTING FOR THE FIRST TIME. THE EFFECTS OF COMPOSITION GRADIENTS DUE TO HE OR HEAVY ELEMENTS ARE NOT YET WELL UNDERSTOOD. AT THE SAME TIME, THE CASSINI GRAND FINALE ORBITS WILL BRING UNPRECEDENTED JUNO LIKE CONSTRAINTS ON SATURNS GRAVITY FIELD, SO WE WILL BE ABLE TO TEST IF INTERIOR STRUCTURES GUIDED BY THERMAL EVOLUTION MODELING AGREE WITH OUR UNDERSTANDING OF THE PLANETS CURRENT STATE. METHODOLOGY WE PROPOSE A TWO PRONGED APPROACH TO BETTER UNDERSTAND THE PHYSICAL STATE AND PROCESSES AFFECTING THE INTERIOR OF SATURN. AT UC BERKELEY, CO I AND HIS STUDENT WILL USE POWERFUL FIRST PRINCIPLES SIMULATIONS TO MAP OUT THE H HE PHASE DIAGRAM AND EQUATION OF STATE IN THE VICINITY OF SATURNS ADIABAT. THE PRESSURE TEMPERATURE CONDITIONS FOR THE ONSET OF HE RAIN WILL BE DETERMINED. FURTHERMORE, SIMULATIONS WILL PERFORMED TO DETERMINE THE EFFECTS OF WATER, ROCKS, AND IRON BEING MIXED WITH THE DENSE H HE FLUID. AT UC SANTA CRUZ, PI AND A STUDENT WILL INCORPORATE THESE FIRST PRINCIPLE MATERIALS PROPERTIES INTO A NEW THERMAL EVOLUTION CODE, TO INVESTIGATE THE THERMAL EVOLUTION OF SATURN, AND FOR THE FIRST TIME ACCURATELY TREAT TEMPERATURE GRADIENTS IN REGIONS OF HE AND HEAVY ELEMENT COMPOSITION GRADIENTS. WE PLAN TO DETERMINE WHEN HE RAIN STARTED IN SATURN. WHAT IS THE MAXIMUM AMOUNT OF HEAVY ELEMENTS THAT IS CONSISTENT WITH THE OBSERVATIONS AND MATERIALS PROPERTIES? HOW ARE THESE HEAVY ELEMENTS DISTRIBUTED IN THE PLANETS INTERIOR? ALONG WITH CO I HUBBARD, FORTNEY AND HIS STUDENT WILL COMPUTE STATE OF THE ART STRUCTURE MODELS THAT WILL YIELD DETAILED PREDICTIONS FOR SATURNS GRAVITY FIELD, WHICH WILL BE COMPARED TO CASSINI GRAVITY DATA AND ALL AVAILABLE RING SEISMOLOGY DATA. AFTER CASSINI DATA IS IN HAND, WE WILL ASSESS DEVIATIONS FROM HYDROSTATIC EQUILIBRIUM DUE TO THE POSSIBLE PRESENCE OF DEEP ZONAL WINDS. RELEVANCE THE PROPOSED THEORETICAL AND MODELING INVESTIGATION SEEKS TO ADVANCE OUR KNOWLEDGE AND UNDERSTANDING OF THE COMPOSITION AND PHYSICAL PROCESSES AT WORK IN THE INTERIOR SATURN. THE NASA CALL FOR THE CASSINI PARTICIPATING SCIENTISTS PROGRAM STATES THAT PARTICIPATING SCIENTISTS MAY PROPOSE ANY INVESTIGATION THAT WOULD USE FUTURE MISSION DATA TO ADDRESS THE GOALS OF THE CASSINI GRAND FINALE, INCLUDING USING THE HIGH INCLINATION ORBITS TO STUDY SATURNS INTERNAL STRUCTURE, ATMOSPHERE, INNER MAGNETOSPHERE, AND RINGS. OUR PROPOSED WORK FITS WITHIN THE SCOPE OF THIS PROGRAM. Funding Only Action ($40) 2/25/22 5 OBJECTIVES WE AIM TO UNDERSTAND THE INTERIOR OF SATURN THROUGH A COMBINATION OF NEW GRAVITY FIELD DATA FROM CASSINI, NEW AB INITIO SIMULATIONS OF PLANETARY MATERIALS AT HIGH PRESSURE, AND NEW CALCULATIONS OF THE TEMPERATURE STRUCTURE AND GRAVITY FIELD OF THE PLANET. SATURNS INTERIOR HOLDS TREMENDOUS UNKNOWNS AND COMPLEXITIES. SATURNS INTERIOR IS COOL ENOUGH THAT THE PHASE SEPARATION OF HE FROM LIQUID METALLIC HYDROGEN HAS LIKELY BEEN OCCURRING FOR THE PAST 2 GYR. THIS HE RAIN HAS LONG BEEN SUGGESTED TO BE THE ADDITIONAL ENERGY SOURCE THAT EXPLAINS SATURNS OBSERVED HIGH INTRINSIC HEAT FLUX. HOWEVER, AT THIS POINT THIS IS STILL JUST A PLAUSIBLE STORY WITHOUT A SUPPORTING, QUANTITATIVE THEORY. WE AIM TO DEVELOP A CONSISTENT AND PREDICTIVE THEORETICAL FRAMEWORK TO PUT THE HE RAIN HYPOTHESIS ON A SOLID QUANTITATIVE FOOTING FOR THE FIRST TIME. THE EFFECTS OF COMPOSITION GRADIENTS DUE TO HE OR HEAVY ELEMENTS ARE NOT YET WELL UNDERSTOOD. AT THE SAME TIME, THE CASSINI GRAND FINALE ORBITS WILL BRING UNPRECEDENTED JUNO LIKE CONSTRAINTS ON SATURNS GRAVITY FIELD, SO WE WILL BE ABLE TO TEST IF INTERIOR STRUCTURES GUIDED BY THERMAL EVOLUTION MODELING AGREE WITH OUR UNDERSTANDING OF THE PLANETS CURRENT STATE. METHODOLOGY WE PROPOSE A TWO PRONGED APPROACH TO BETTER UNDERSTAND THE PHYSICAL STATE AND PROCESSES AFFECTING THE INTERIOR OF SATURN. AT UC BERKELEY, CO I AND HIS STUDENT WILL USE POWERFUL FIRST PRINCIPLES SIMULATIONS TO MAP OUT THE H HE PHASE DIAGRAM AND EQUATION OF STATE IN THE VICINITY OF SATURNS ADIABAT. THE PRESSURE TEMPERATURE CONDITIONS FOR THE ONSET OF HE RAIN WILL BE DETERMINED. FURTHERMORE, SIMULATIONS WILL PERFORMED TO DETERMINE THE EFFECTS OF WATER, ROCKS, AND IRON BEING MIXED WITH THE DENSE H HE FLUID. AT UC SANTA CRUZ, PI AND A STUDENT WILL INCORPORATE THESE FIRST PRINCIPLE MATERIALS PROPERTIES INTO A NEW THERMAL EVOLUTION CODE, TO INVESTIGATE THE THERMAL EVOLUTION OF SATURN, AND FOR THE FIRST TIME ACCURATELY TREAT TEMPERATURE GRADIENTS IN REGIONS OF HE AND HEAVY ELEMENT COMPOSITION GRADIENTS. WE PLAN TO DETERMINE WHEN HE RAIN STARTED IN SATURN. WHAT IS THE MAXIMUM AMOUNT OF HEAVY ELEMENTS THAT IS CONSISTENT WITH THE OBSERVATIONS AND MATERIALS PROPERTIES? HOW ARE THESE HEAVY ELEMENTS DISTRIBUTED IN THE PLANETS INTERIOR? ALONG WITH CO I HUBBARD, FORTNEY AND HIS STUDENT WILL COMPUTE STATE OF THE ART STRUCTURE MODELS THAT WILL YIELD DETAILED PREDICTIONS FOR SATURNS GRAVITY FIELD, WHICH WILL BE COMPARED TO CASSINI GRAVITY DATA AND ALL AVAILABLE RING SEISMOLOGY DATA. AFTER CASSINI DATA IS IN HAND, WE WILL ASSESS DEVIATIONS FROM HYDROSTATIC EQUILIBRIUM DUE TO THE POSSIBLE PRESENCE OF DEEP ZONAL WINDS. RELEVANCE THE PROPOSED THEORETICAL AND MODELING INVESTIGATION SEEKS TO ADVANCE OUR KNOWLEDGE AND UNDERSTANDING OF THE COMPOSITION AND PHYSICAL PROCESSES AT WORK IN THE INTERIOR SATURN. THE NASA CALL FOR THE CASSINI PARTICIPATING SCIENTISTS PROGRAM STATES THAT PARTICIPATING SCIENTISTS MAY PROPOSE ANY INVESTIGATION THAT WOULD USE FUTURE MISSION DATA TO ADDRESS THE GOALS OF THE CASSINI GRAND FINALE, INCLUDING USING THE HIGH INCLINATION ORBITS TO STUDY SATURNS INTERNAL STRUCTURE, ATMOSPHERE, INNER MAGNETOSPHERE, AND RINGS. OUR PROPOSED WORK FITS WITHIN THE SCOPE OF THIS PROGRAM. Other Administrative Action $0 4/15/20 Not listed OBJECTIVES WE AIM TO UNDERSTAND THE INTERIOR OF SATURN THROUGH A COMBINATION OF NEW GRAVITY FIELD DATA FROM CASSINI NEW AB INITIO SIMULATIONS OF PLANETARY MATERIALS AT HIGH PRESSURE AND NEW CALCULATIONS OF THE TEMPERATURE STRUCTURE AND GRAVITY FIELD OF THE PLANET. SATURNS INTERIOR HOLDS TREMENDOUS UNKNOWNS AND COMPLEXITIES. SATURNS INTERIOR IS COOL ENOUGH THAT THE PHASE SEPARATION OF HE FROMLIQUID METALLIC HYDROGEN HAS LIKELY BEEN OCCURRING FOR THE PAST 2 GYR. THIS HE RAIN HAS LONG BEEN SUGGESTED TO BE THE ADDITIONAL ENERGY SOURCE THAT EXPLAINS SATURNS OBSERVED HIGH INTRINSIC HEAT FLUX. HOWEVER AT THIS POINT THIS IS STILL JUST A PLAUSIBLE STORY WITHOUT A SUPPORTING QUANTITATIVE THEORY. WE AIM TO DEVELOP A CONSISTENT AND PREDICTIVE THEORETICAL FRAMEWORK TO PUT THE HE RAIN HYPOTHESIS ON A SOLID QUANTITATIVE FOOTING FOR THE FIRST TIME. THE EFFECTS OF COMPOSITION GRADIENTS DUE TO HE OR HEAVY ELEMENTS ARE NOT YET WELL UNDERSTOOD. AT THE SAME TIME THE CASSINI GRAND FINALE ORBITS WILL BRING UNPRECEDENTED JUNO LIKE CONSTRAINTS ON SATURNS GRAVITYFIELD SO WE WILL BE ABLE TO TEST IF INTERIOR STRUCTURES GUIDED BY THERMAL EVOLUTION MODELING AGREE WITH OUR UNDERSTANDING OF THE PLANETS CURRENT STATE.METHODOLOGY WE PROPOSE A TWO PRONGED APPROACH TO BETTER UNDERSTAND THE PHYSICAL STATE AND PROCESSES AFFECTING THE INTERIOR OF SATURN. AT UC BERKELEY CO I AND HIS STUDENT WILL USE POWERFUL FIRST PRINCIPLES SIMULATIONS TO MAP OUT THE H HE PHASE DIAGRAM AND EQUATION OF STATE IN THE VICINITY OF SATURNS ADIABAT. THE PRESSURE TEMPERATURE CONDITIONS FOR THE ONSET OF HE RAIN WILL BE DETERMINED. FURTHERMORE SIMULATIONS WILL PERFORMED TO DETERMINE THE EFFECTS OF WATER ROCKS AND IRON BEING MIXED WITH THE DENSEH HE FLUID. AT UC SANTA CRUZ PI AND A STUDENT WILL INCORPORATE THESE FIRST PRINCIPLE MATERIALS PROPERTIES INTO A NEW THERMAL EVOLUTION CODE TO INVESTIGATE THE THERMAL EVOLUTION OF SATURN AND FOR THE FIRST TIME ACCURATELY TREAT TEMPERATURE GRADIENTS IN REGIONS OF HE AND HEAVY ELEMENT COMPOSITION GRADIENTS. WE PLAN TO DETERMINE WHEN HE RAIN STARTED IN SATURN. WHAT IS THE MAXIMUM AMOUNTOF HEAVY ELEMENTS THAT IS CONSISTENT WITH THE OBSERVATIONS AND MATERIALS PROPERTIES? HOW ARE THESE HEAVY ELEMENTS DISTRIBUTED IN THE PLANETS INTERIOR? ALONG WITH CO I HUBBARD FORTNEY AND HIS STUDENT WILL COMPUTE STATE OF THE ART STRUCTURE MODELS THAT WILL YIELD DETAILED PREDICTIONS FOR SATURNS GRAVITY FIELD WHICH WILL BE COMPARED TO CASSINI GRAVITY DATA AND ALL AVAILABLE RING SEISMOLOGY DATA.AFTER CASSINI DATA IS IN HAND WE WILL ASSESS DEVIATIONS FROM HYDROSTATIC EQUILIBRIUM DUE TO THE POSSIBLE PRESENCE OF DEEP ZONAL WINDS. RELEVANCE THE PROPOSED THEORETICAL AND MODELING INVESTIGATION SEEKS TO ADVANCE OUR KNOWLEDGE AND UNDERSTANDING OF THE COMPOSITION AND PHYSICAL PROCESSES AT WORK IN THE INTERIOR SATURN. THE NASA CALL FOR THE CASSINI PARTICIPATING SCIENTISTS PROGRAM STATES THAT PARTICIPATING SCIENTISTS MAY PROPOSE ANY INVESTIGATION THAT WOULD USE FUTURE MISSION DATA TO ADDRESS THE GOALS OF THE CASSINI GRAND FINALE INCLUDING USING THE HIGH INCLINATION ORBITS TO STUDY SATURNS INTERNAL STRUCTURE ATMOSPHERE INNERMAGNETOSPHERE AND RINGS. OUR PROPOSED WORK FITS WITHIN THE SCOPE OF THIS PROGRAM. $0 4/15/20 Not listed OBJECTIVES WE AIM TO UNDERSTAND THE INTERIOR OF SATURN THROUGH A COMBINATION OF NEW GRAVITY FIELD DATA FROM CASSINI NEW AB INITIO SIMULATIONS OF PLANETARY MATERIALS AT HIGH PRESSURE AND NEW CALCULATIONS OF THE TEMPERATURE STRUCTURE AND GRAVITY FIELD OF THE PLANET. SATURNS INTERIOR HOLDS TREMENDOUS UNKNOWNS AND COMPLEXITIES. SATURNS INTERIOR IS COOL ENOUGH THAT THE PHASE SEPARATION OF HE FROMLIQUID METALLIC HYDROGEN HAS LIKELY BEEN OCCURRING FOR THE PAST 2 GYR. THIS HE RAIN HAS LONG BEEN SUGGESTED TO BE THE ADDITIONAL ENERGY SOURCE THAT EXPLAINS SATURNS OBSERVED HIGH INTRINSIC HEAT FLUX. HOWEVER AT THIS POINT THIS IS STILL JUST A PLAUSIBLE STORY WITHOUT A SUPPORTING QUANTITATIVE THEORY. WE AIM TO DEVELOP A CONSISTENT AND PREDICTIVE THEORETICAL FRAMEWORK TO PUT THE HE RAIN HYPOTHESIS ON A SOLID QUANTITATIVE FOOTING FOR THE FIRST TIME. THE EFFECTS OF COMPOSITION GRADIENTS DUE TO HE OR HEAVY ELEMENTS ARE NOT YET WELL UNDERSTOOD. AT THE SAME TIME THE CASSINI GRAND FINALE ORBITS WILL BRING UNPRECEDENTED JUNO LIKE CONSTRAINTS ON SATURNS GRAVITYFIELD SO WE WILL BE ABLE TO TEST IF INTERIOR STRUCTURES GUIDED BY THERMAL EVOLUTION MODELING AGREE WITH OUR UNDERSTANDING OF THE PLANETS CURRENT STATE.METHODOLOGY WE PROPOSE A TWO PRONGED APPROACH TO BETTER UNDERSTAND THE PHYSICAL STATE AND PROCESSES AFFECTING THE INTERIOR OF SATURN. AT UC BERKELEY CO I AND HIS STUDENT WILL USE POWERFUL FIRST PRINCIPLES SIMULATIONS TO MAP OUT THE H HE PHASE DIAGRAM AND EQUATION OF STATE IN THE VICINITY OF SATURNS ADIABAT. THE PRESSURE TEMPERATURE CONDITIONS FOR THE ONSET OF HE RAIN WILL BE DETERMINED. FURTHERMORE SIMULATIONS WILL PERFORMED TO DETERMINE THE EFFECTS OF WATER ROCKS AND IRON BEING MIXED WITH THE DENSEH HE FLUID. AT UC SANTA CRUZ PI AND A STUDENT WILL INCORPORATE THESE FIRST PRINCIPLE MATERIALS PROPERTIES INTO A NEW THERMAL EVOLUTION CODE TO INVESTIGATE THE THERMAL EVOLUTION OF SATURN AND FOR THE FIRST TIME ACCURATELY TREAT TEMPERATURE GRADIENTS IN REGIONS OF HE AND HEAVY ELEMENT COMPOSITION GRADIENTS. WE PLAN TO DETERMINE WHEN HE RAIN STARTED IN SATURN. WHAT IS THE MAXIMUM AMOUNTOF HEAVY ELEMENTS THAT IS CONSISTENT WITH THE OBSERVATIONS AND MATERIALS PROPERTIES? HOW ARE THESE HEAVY ELEMENTS DISTRIBUTED IN THE PLANETS INTERIOR? ALONG WITH CO I HUBBARD FORTNEY AND HIS STUDENT WILL COMPUTE STATE OF THE ART STRUCTURE MODELS THAT WILL YIELD DETAILED PREDICTIONS FOR SATURNS GRAVITY FIELD WHICH WILL BE COMPARED TO CASSINI GRAVITY DATA AND ALL AVAILABLE RING SEISMOLOGY DATA.AFTER CASSINI DATA IS IN HAND WE WILL ASSESS DEVIATIONS FROM HYDROSTATIC EQUILIBRIUM DUE TO THE POSSIBLE PRESENCE OF DEEP ZONAL WINDS. RELEVANCE THE PROPOSED THEORETICAL AND MODELING INVESTIGATION SEEKS TO ADVANCE OUR KNOWLEDGE AND UNDERSTANDING OF THE COMPOSITION AND PHYSICAL PROCESSES AT WORK IN THE INTERIOR SATURN. THE NASA CALL FOR THE CASSINI PARTICIPATING SCIENTISTS PROGRAM STATES THAT PARTICIPATING SCIENTISTS MAY PROPOSE ANY INVESTIGATION THAT WOULD USE FUTURE MISSION DATA TO ADDRESS THE GOALS OF THE CASSINI GRAND FINALE INCLUDING USING THE HIGH INCLINATION ORBITS TO STUDY SATURNS INTERNAL STRUCTURE ATMOSPHERE INNERMAGNETOSPHERE AND RINGS. OUR PROPOSED WORK FITS WITHIN THE SCOPE OF THIS PROGRAM. $0 5/8/19