WITH COLLABORATORS XXX XXX XXX WE WILL PERFORM EVAPORATION CALCULATIONS ON CHONDRULE BULK COMPOSITIONS TO SEE IF DUST AND WATER ENRICHMENTS AND PRESSURE AND TEMPERATURE VS TIME PROFILES IN PLUMES GENERATED BY IMPACTS ON ICY PLANETESIMALS ARE COMPATIBLE WITH CHONDRULE CHEMICAL AND ISOTOPIC PROPERTIES. WE WILL STUDY WARK-LOVERING RIM LAYERS ON INCLUSIONS AND THEIR CONSTITUENTS IN PRIMITIVE CHONDRITES BY SCANNING ELECTRON MICROSCOPY (SEM) ELECTRON PROBE MICROANALYSIS (EPMA) AND WITH COLLABORATORS XXX AND XXX FOCUSED ION BEAM-TRANSMISSION ELECTRON MICROSCOPY (FIB-TEM) AND NANO-SECONDARY ION MASS SPECTROMETRY (SIMS) RESPECTIVELY TO DETERMINE THEIR ORIGIN AND INFER THE PHYSICO-CHEMICAL CONDITIONS OF THE SUCCESSIVE SOLAR NEBULAR ENVIRONMENTS IN WHICH THEY FORMED. WITH COLLABORATOR XXX WE WILL USE SYNCHROTRON MICRO-X-RAY ABSORPTION NEAR EDGE STRUCTURE SPECTROSCOPY (XANES) TO STUDY TI VALENCE IN SILICATES OF ACFER AND UNEQUILIBRATED ENSTATITE CHONDRITES TO INFER THE OXYGEN FUGACITIES UNDER WHICH THEY FORMED AND TO MEASURE THE VALENCE AND COORDINATION OF TI IN SILICATES OF H CHONDRITES AND ENSTATITE CHONDRITES AS A FUNCTION OF METAMORPHIC GRADE. WITH COLLABORATORS XXX XXX XXX WE WILL PERFORM DYNAMIC CRYSTALLIZATION EXPERIMENTS AT CONTROLLED OXYGEN FUGACITY TO DETERMINE RATES OF OXIDATION AND REDUCTION OF IRON AND TITANIUM IN CHONDRULE COMPOSITION MELTS AS A FUNCTION OF COOLING RATE PARTIAL PRESSURE OF WATER AND DROPLET SIZE IN ORDER TO CONSTRAIN THE FORMATION CONDITIONS OF CHONDRULES. WITH COLLABORATORS XXX XXX XXX XXX WE WILL FIND MIXTURES OF LAYERS IN MODEL SUPERNOVA STARS WHOSE ISOTOPIC COMPOSITIONS MOST CLOSELY MATCH THOSE OF PRESOLAR GRAPHITE AND SIC X-GRAINS AND WHOSE ELEMENTAL COMPOSITIONS SIMULTANEOUSLY YIELD EQUILIBRIUM CONDENSATION SEQUENCES IDENTICAL TO THOSE INFERRED FROM TEXTURES OF INCLUSIONS IN THOSE PHASES.