VENUS COULD HAVE ACCRETED AN EARTH-LIKE MASS OF WATER THAT CONDENSED EARLY IN HISTORY. PUTATIVE AQUEOUS PROCESSES SHOULD HAVE AFFECTED COMPOSITIONS OF THE LITHOSPHERE AND THE ATMOSPHERE. EARLY CHEMICAL AND MINERALOGICAL TRANSFORMATIONS INFLUENCED THE GEOLOGICAL EVOLUTION AFTER EVAPORATION OF AN OCEAN AND LOSS OF WATER FROM THE PLANET. SINGS OF PAST AQUEOUS PROCESSES COULD BE PRESENT IN MINERALOGY AND CHEMICAL AND PHYSICAL PROPERTIES OF SURFACE MATERIALS. IN ORDER TO UNDERSTAND LINKS BETWEEN PUTATIVE AQUEOUS PROCESSES AND PRESENT VENUS WE WILL INVESTIGATE CHEMISTRY AND MINERALOGY OF AQUEOUS INTERACTIONS ON THE EARLY PLANET AND EVALUATE THEIR EFFECTS ON THE SUBSEQUENT EVOLUTION. ON EARLY VENUS CHEMICAL INTERACTIONS BETWEEN OCEANIC WATER ATMOSPHERIC GASES AND ROCKS COULD HAVE AFFECTED THE COMPOSITION ON VOLATILE-BEARING PLANETARY ENVELOPES. DISSOLUTION ATMOSPHERIC GASES AND ROCKS FORMED THE COMPOSITION AND PH OF OCEANIC WATER. ALTERATION OF ROCKS LED TO FORMATION OF SECONDARY MINERALS SUCH AS CLAYS CARBONATES AND OXIDES. SALTS COULD HAVE PRECIPITATED DURING WARMING AND EVAPORATION OF OCEANIC WATER. THE SPECIATION OF THE ATMOSPHERE-OCEAN-ROCK SYSTEM MASSES OF COMPOUNDS AND SECONDARY MINERALOGY CAN BE EVALUATED BY METHODS OF PHYSICAL CHEMISTRY WHICH ASSUME AT LEAST PARTIAL CHEMICAL EQUILIBRATION BETWEEN PHASES. WE WILL EVALUATE THE COMPOSITION OF ALTERED ROCKS AND PRECIPITATED SALTS ON EARLY VENUS. THE COMPLETE EVAPORATION OF AN OCEAN SHOULD HAVE CAUSED ACCUMULATION OF SALTS ATOP AN ALTERED LITHOSPHERE. THE GREENHOUSE WARMING TRANSFORMED AQUEOUS MINERALS THROUGH DEHYDRATION DECARBONATION EVAPORATION MELTING AND INTERACTION WITH OTHER SPECIES. SOME MINERALS FORMED AT THE AQUEOUS STAGE COULD HAVE BEEN BURIED AND MELTED. AN OCCURRENCE OF REWORKED ANCIENT MINERALS IN THE LITHOSPHERE COULD HAVE BEEN MANIFESTED IN THE CHEMICAL COMPOSITION AND THE REDOX STATE OF SURFACE ROCKS. ERUPTIONS OF MOLTEN SALTS COULD BE RESPONSIBLE FOR THE FORMATION OF MEANDERING CHANNELS SEEN ON MAGELLAN RADAR IMAGES. WE WILL EVALUATE FATE OF AQUEOUS MINERALS AFTER CESSATION OF AN AQUEOUS STAGE OF VENUS EVOLUTION. THE COMPOSITION OF THE HYDROSPHERE-LITHOSPHERE-ATMOSPHERE SYSTEM WILL BE EVALUATED THROUGH MASS BALANCE CALCULATIONS CONSTRAINED BY DATA ON VENUS AND EARTH. THE SPECIATION AND AMOUNTS OF COMPOUNDS WILL BE EVALUATED THROUGH CALCULATIONS OF CHEMICAL EQUILIBRIA IN THE WATER-SOLID-GAS TYPE SYSTEM. THE SPECIATION WILL REFLECT MASS BALANCES EQUILIBRIUM CONSTANTS OF CHEMICAL REACTIONS AND TEMPERATURE-PRESSURE CONDITIONS ADOPTED FROM CLIMATE MODELS. WE WILL CONSTRAIN COMPOSITIONS OF ALTERED ROCKS AND PRECIPITATED SALTS TOGETHER WITH THE ATMOSPHERIC COMPOSITION AND CONCENTRATIONS OF SOLUTES IN OCEANIC WATER. THE STABILITY OF HEATED SALTS AND OTHER MINERALS WILL BE EVALUATED THROUGH CALCULATIONS OF GAS-SOLID SOLID-MELT TYPE CHEMICAL EQUILIBRIA AND BY THE ANALYSIS OF PHASE DIAGRAMS. THE PROPOSED WORK WILL PROVIDE INSIGHTS INTO EARLY HISTORY OF VENUS EFFECTS OF PUTATIVE AQUEOUS PROCESSES ON SUBSEQUENT EVOLUTION AND THE CURRENT STAGE OF THE PLANET. THE WORK WILL HELP ENVISION SINGS OF ANCIENT AQUEOUS PROCESSES ON VENUS. RESULTS OF THIS WORK WILL HELP INTERPRET DATA FROM FURTHER MISSIONS INCLUDING A SAMPLE RETURN MISSION. THE WORK COMPLEMENTS CLIMATE MODELING EFFORTS TO CONSTRAIN THE PREVALENCE OF ANCIENT AQUEOUS PROCESSES ON VENUS. A COMPARISON OF OUR RESULTS WITH DATA ON EARLY EARTH WILL LINK EARLY EVOLUTIONS OF THE SISTER PLANETS. THE RESULTS COULD BE APPLIED TO TERRESTRIAL EXOPLANETS WITH EARLY HYDROSPHERES. THE PROPOSAL IS RELEVANT TO THE NASA SSW PROGRAM BECAUSE IT IS INTENDED TO UNDERSTAND GEOLOGICAL HISTORY OF FLUID INVENTORIES AND THEIR EFFECTS ON OBSERVABLE PROPERTIES OF SURFACE MATERIALS ON VENUS.