WITH THE RECENT ROVER RESULTS FROM THE MARS' SURFACE AND ATMOSPHERE AND WITH THE DISCOVERY OF THE EXTREME WATER-RICH NWA 7034 THE PRESENCE OF WATER ON MARS HAS RECEIVED NEW ATTENTION AND INTEREST.METEORITES FROM MARS ALL CONTAIN WATER IN LIMITED PROPORTIONS. WATER EXTRACTED FROM METEORITES CAN PROVIDE INFORMATION ABOUT THE TYPE ORIGIN AND NATURE OF THE WATER ON THE PARENT BODY. INFORMATION ABOUT THE ISOTOPE GEOCHEMISTRY OF SUCH WATER IS VALUABLE IN TERMSOF TRACING ITS ORIGIN AND ASSESSING THE NATURE AND DEGREE OF POSSIBLE WATER-ROCK AND ATMOSPHERE-WATER-ROCK INTERACTIONS.LIMITED WORK HAS BEEN DONE IN THE PAST ON THE OXYGEN AND HYDROGEN ISOTOPE COMPOSITION OF WATER RELEASED FROM MARTIAN METEORITES. ISOTOPIC ANALYSES OF EXTRACTED WATERS SHOW THAT THEIR COMPOSITIONS ARE DIFFERENT FROM THAT OF THE SILICATE PORTION OF THE METEORITES INDICATING DIFFERENT SOURCES OF THE OXYGEN IN WATER AND ROCK (MARTIAN ATMOSPHERE CRUSTAL FLUIDS AN ANCIENT MARTIAN OCEAN A COMETARY IMPACT). NWA 7034 ALSO SHOWS TWO OXYGEN ISOTOPE RESERVOIRS IN ITS SILICATE PHASE. THESE FEW STUDIES HAVE BEEN CARRIED OUT ON DIFFERENT METEORITES.WE PROPOSE TO CONDUCT A SYSTEMATIC STUDY OF WATER EXTRACTED FROM MARTIAN METEORITES. WE WILL ANALYSE THE OXYGEN AND HYDROGEN ISOTOPIC COMPOSITION OF SUCH WATERS FROM A VARIETY OF MARTIAN METEORITES THAT ALSO DISPLAY DIFFERENCES IN WATER-CONTENT MINERALOGY/ MINERAL-CHEMISTRY AND DEGREE OF MARTIAN ALTERATION (IN PARTICULAR THE AMOUNT OF THE OLIVINE ALTERATION-PRODUCT IDDINGSITE). BOTH OXYGEN AND HYDROGEN ANALYSES WILL BE OBTAINED FROM THE SAME ALIQUOTS OF THE SAME METEORITE.WATER WILL BE EXTRACTED FROM THE SAMPLES BY HEATING IN VACUUM AND ITS OXYGEN ISOTOPE RATIO WILL BE DETERMINED BY DIRECT FLUORINATION IN SEALED NI-BOMBS. FOR THE HYDROGEN ISOTOPE ANALYSES THE WATER WILL BE ANALYZED BY THERMAL COMBUSTION. DEPENDING ON THE TOTAL WATER CONTENT 10S OF MG SAMPLES ARE REQUIRED FOR BULK ANALYSES WHEREAS STEPWISE HEATING AND COLLECTION/ANALYSIS OF WATER FROM VARIOUS TEMPERATURE RANGES REQUIRES 100S OF MG. OUR STABLE ISOTOPE LABORATORY IS EQUIPPED TO CONDUCT ALL OF THE REQUIRED ANALYSES. WE WILL ADDRESS THE FOLLOWING ISSUES: (I) IS WATER CONTAINED IN MARTIAN METEORITES IN ISOTOPIC EQUILIBRIUM WITH THE HOST ROCK? IF NOT WHY IS THIS? WICH PROCESSES CREATED THIS DISEQUILIBRIUM AND WHICH GEOCHEMICAL MINERALOGICAL AND GEOLOGIC CONDITIONS ARE REQUIRED TO MAINTAIN IT? (II) DO MARTIAN METEORITES HAVE SIMILAR OR DIFFERENT WATER RELEASE PATTERNS? ARE THEY ALL SIMILAR TO MSL RESULTS? IS WATER FROM DIFFERENT TEMPERATURE INTERVALS ISOTOPICALLY DIFFERENT? (III) DO WATERS FROM DIFFERENT MARTIAN METEORITES GROUPS HAVE DIFFERENTISOTOPE COMPOSITIONS? ESPECIALLY IS WATER CONTAINED IN DEPLETED AND ENRICHED SHERGOTTITES ISOTOPICALLY DIFFERENT? AND IF SO WHAT DOES THIS TELL US ABOUT THEIR GEOLOGIC ORIGIN? (IV) DOES ATMOSPHERIC WATER ON MARS CARRY A MASS-INDEPENDENT OXYGEN ISOTOPE SIGNAL? IF SO HOW WAS THIS SIGNAL IMPRINTED ONTO THE SURFACE MATERIAL (ROCKS WATER) OF MARS? AND DO WE SEE MORE "ATMOSPHERIC" SIGNALS INMETEORITES THAT HAVE HIGHER DEGREES OF AQUEOUS ALTERATION AND/OR OXIDATION? (V) DO THE DIFFERENT AGES AND DIFFERENT OXYGEN ISOTOPIC COMPOSITIONS OF DIFFERENT COMPONENTS (PYROXENES VS. OXIDES AND EASILY EXCHANGEABLE FELDSPARS) IN THE BASALTIC BRECCIA NWA 7034 TELL US SOMETHING ABOUT THE DIFFERENT OXYGEN ISOTOPE RESERVOIRS ON MARS AS ITEVOLVED FROM YOUNG AND WET TO OLD AND DRY? WHAT IMPLICATIONSCAN WE DRAW FROM THIS ABOUT THE EVOLUTION OF THE MARTIAN ATMOSPHERE?WITH THIS RESEARCH WE WILL BE ABLE TO ADD PREVIOUSLY UNSEEN DETAILS OF OXYGEN ISOTOPIC RESERVOIRS AND EVOLUTION OF MARS AND OF SECONDARY AQUEOUS PROCESSES OPERATING ON ITS SURFACE. WE WILL REACH A BETTER UNDERSTANDING OF THE ROLE THAT WATER PLAYED DURING MARS' EVOLUTION AND OF THE INTERACTIONS BETWEEN ITS SURFACE AND ATMOSPHERE.