THE INDUCTIVE GENERATION OF A GLOBAL MAGNETIC FIELD BY THE MOTION OF CONDUCTING FLUID IN A PLANETARY CORE IS KNOWN AS THE DYNAMO. ALTHOUGH THE MOON TODAY HAS NO GLOBAL MAGNETIC FIELD RECENT PALEOMAGNETIC MEASUREMENTS OF APOLLO SAMPLES INDICATE THAT THE MOON GENERATED A DYNAMO FROM AT LEAST 4.25 TO 1.92 BILLION YEARS AGO (GA). FURTHERMORE SAMPLE MEASUREMENTS SUGGEST THAT PRIOR TO ABOUT 3.5 GA A PUTATIVE HIGH-FIELD EPOCH EXISTED WHEN THE FIELD INTENSITY MAY HAVE REACHED ~70 MICROTESLAS (UT) (EARTH-STRENGTH). HOWEVER BECAUSE METALLIC MINERALS IN LUNAR SAMPLES ALTER WHEN HEATED IN AIR NEARLY ALL PREVIOUS PALEOINTENSITY DETERMINATIONS FROM SAMPLES OLDER THAN ~3.3 GA HAVE EMPLOYED NON-HEATING TECHNIQUES WHICH HAVE UNCERTAINTIES RANGING UP TO AN ORDER OF MAGNITUDE OR MORE FOR SOME SAMPLES. DYNAMO SCALING LAWS INDICATE THAT IF THE MOON S DYNAMO WERE GENERATED BY CONVECTION IN THE CORE ITS SURFACE FIELD SHOULD NOT HAVE CONTINUOUSLY EXCEEDED ~10 UT OVER THE PERIOD 4.2-3.5 GA. THEREFORE IF THE FIELD INDEED CONTINUOUSLY REACHED SUCH VALUES OF&GT;70 UT AS TENTATIVELY SUGGESTED BY EXISTING DATA THEN TWO POSSIBLE EXPLANATIONS ARE (I) THE LUNAR CORE GENERATED A CONVECTIVE DYNAMO BUT ONE THAT ONLY INTERMITTENTLY REACHED SUCH HIGH FIELDS DURING THIS PERIOD OR (II) THE LUNAR DYNAMO WAS DRIVEN BY A PROCESS OTHER THAN CORE CONVECTION THAT WAS CAPABLE OF CONTINUOUSLY PRODUCING STRONGER FIELDS. ALTERNATIVELY (III) THE HIGH APPARENT PALEOINTENSITIES ARE IN ERROR AND THE FIELD NEVER ACTUALLY EXCEED 10 UT. ANY OF THESE 3 OUTCOMES WOULD HAVE MAJOR IMPLICATIONS FOR OUR UNDERSTANDING OF THE MOON S ORIGIN THERMAL HISTORY INTERIOR STRUCTURE ORBITAL HISTORY AND THE PHYSICS OF DYNAMO GENERATION. THE KEY TO RESOLVING THIS ISSUE IS TO OBTAIN ACCURATE (&LT;10% UNCERTAINTY) PALEOINTENSITIES. SUCH ACCURACIES COULD BE OBTAINED IF LABORATORY HEATING COULD BE CONDUCTED WITHOUT ALTERING THE SAMPLES. WITH THIS GOAL WE RECENTLY DEVELOPED A CONTROLLED-OXYGEN FUGACITY THERMAL DEMAGNETIZATION SYSTEM. FURTHERMORE WE HAVE RECENTLY RECOGNIZED THAT GLASSY LUNAR REGOLITH BRECCIAS HAVE OPTIMAL MAGNETIC RECORDING PROPERTIES DUE TO THE FINE SIZES OF THEIR CONSTITUENT METAL GRAINS. APPLYING THIS CONTROLLED ATMOSPHERE HEATING APPARATUS TO THREE REGOLITH BRECCIAS WE HAVE RECENTLY OBTAINED THE FIRST ACCURATE HEATING-BASED LUNAR PALEOINTENSITIES FOR THE PERIOD AFTER 2 GA. HERE WE PROPOSE TO CONSTRAIN THE INTENSITY OF THE EARLY LUNAR DYNAMO AND OR REFUTE THE EXISTENCE OF A HIGH-FIELD (I.E. TENS OF UT) EPOCH USING CONTROLLED-ATMOSPHERE THERMAL PALEOINTENSITY ANALYSES. WE WILL ANALYZE FOUR GLASSY LUNAR BRECCIAS OLDER THAN 3.4 GA THAT ARE LIKELY TO HAVE HIGH-FIDELITY RECORDS OF THE GLOBAL LUNAR FIELD SPANNING&GT;0.2 BILLION YEARS OF HISTORY. WE WILL CONDUCT THIS WORK AS PART OF TWO TASKS: TASK 1. MEASURE THE PALEOINTENSITY OF THE LUNAR FIELD USING PALEOMAGNETIC ANALYSES TASK 2. CONSTRAIN THE AGES OF THE PALEOINTENSITIES USING AR-BASED GEOCHRONOMETRY. IF WE FIND THAT THE LUNAR FIELD OVER THE PERIOD ~3.4-4.9 GA WAS EITHER CONTINUOUSLY PRESENT BUT WEAKER THAN ~10 UT OR ELSE GREATER THAN 10 UT BUT ONLY INTERMITTENTLY THEN THIS WOULD INDICATE THAT THE EARLY DYNAMO COULD HAVE BEEN GENERATED BY CORE CONVECTION [OUTCOME (I) ABOVE]. ALTERNATIVELY IF WE FIND THAT THE DYNAMO SURFACE FIELD WAS CONTINUOUSLY STRONGER THAN ~10 UT OVER THIS PERIOD THIS WOULD SUGGEST THAT THE DYNAMO WAS GENERATED BY A PROCESS OTHER THAN CORE CONVECTION [OUTCOME (II)]. FINALLY IF WE FIND (III) THAT ALL PALEOINTENSITIES DURING THIS PERIOD ARE ACTUALLY WEAKER THAN ~10 UT THEN THIS WOULD BE COMPATIBLE WITH A CONTINUOUSLY OPERATING CORE CONVECTION DYNAMO.