THREE GOALS ARE THE DRIVERS FOR THE PROPOSED WORK. ONE GOAL IS TO PROVIDE 3D INTERIOR STRUCTURE MODELS OF JUPITER. ANOTHER GOALS IS TO INFER IMPLICATIONS FROM THE OBSERVED ATMOSPHERIC ABUNDANCES OF ELEMENTS LIKE OXYGEN AND HELIUM ON THE INTERNAL STRUCTURE EVOLUTION AND FORMATION OF JUPITER. AS STRUCTURE AND EVOLUTION MODELS RELY HEAVILY ON THE ASSUMED HIGH-DENSITY BEHAVIOR OF HYDROGEN AND HELIUM THE COMPUTED JUPITER MODELS WILL ALSO BE IMPORTANT FOR CONSTRAINING THE PROPERTIES OF H-HE UNDER TEMPERATURE-PRESSURE CONDITIONS WHERE THE MAGNETIC FIELD OF GAS GIANT PLANETS LIKE JUPITER ORIGINATES FROM. TO BETTER UNDERSTAND THIS INTERPLAY IS THE THIRD GOAL OF THIS WORK. TO GIVE AN EXAMPLE JUPITER'S ATMOSPHERIC HELIUM ABUNDANCE IS CLOSE TO THE COSMIC ABUNDANCE BUT IT APPEARS DEPLETED IF COMPARED TO THE SOLAR VALUE AT THE TIME OF SOLAR SYSTEM FORMATION. THIS DEPLETION IS THOUGHT TO RESULT FROM HELIUM RAIN AT GREAT DEPTH ATOP BELOW OR WITHIN THE MAGNETIC DYNAMO REGION. HELIUM RAIN CAN LEAD TO AN INHOMOGENEOUS EVOLUTION. HOWEVER DIFFERENT STATE-OF-THE ART H-HE PHASE DIAGRAMS AND EQUATIONS OF STATE YIELD DIFFERENT PREDICTIONS. THIS WORK WILL EMPLOY VARIOUS H-HE DATA SETS AND VALIDATE THE RESULTING JUPITER MODELS AGAINST OBSERVATIONAL CONSTRAINTS AND PREDICTIONS FROM MAGNETIC FIELD MODELS.